mini|desno|300px|Prikaz Velike crvene pjege i oblaka ono nje, snimljen sa svemirske letjelice Voyager 1 25. veljače 1979. Bijela ovalna oluja kola se nalazi is pod Velike crvene pjege ima približno promjer veličine promjera Zemlje.

mini|desno|300px|Okomit presjek temperature atmosfere ovisno o visini.

mini|desno|300px|Brzina vjetra u Jupiterovoj atmosferi ovisno o zemljopisnoj širini (jovigrafske širine).

mini|300px|Polarna svjetlost na Jupiteru, snimka u ultraljubičastom zračenju, lažno obojana u plavo. Tri svijetle točke su stvorene cijevima magnetskog toka koje su povezane sa Galilejanskim satelima: Io (na lijevoj strani), Ganimed (na dnu) i Europa (isto na dnu).

Jupiter je planet iz klase plinovitih divova s najvećim promjerom i najvećom masom u Sunčevu sustavu, peti po udaljenosti od Sunca (prosječna udaljenost mu je 778 milijuna kilometara); jednom obiđe Sunce za 11,862 godina. Masa mu je 318,4 puta veća od Zemljine (na njega otpada 71 % ukupne planetske mase), a gustoća mu je samo oko četvrtine gustoće Zemlje. Veliki mu dio volumena tvori vodik, kojeg Jupiter, zbog svoje velike mase i gravitacije, nije izgubio od postanka Sunčeva sustava (4,57 milijarde godina), kao što se zbilo s drugim planetima.

Prema astronomskim ispitivanjima, podatcima i prema teorijskim modelima, Jupiter se sastoji od razmjerno malene silikatne jezgre bez oštre granice u sastavu (difuzna jezgra), okružene s dva sloja vodika: donji sloj, pod većim tlakom, ima metalna svojstva gdje su vodikovi elektroni u slabo vezanom ili u slobodnom stanju; gornji je sloj molekularni vodik (H2) u stanju superkritičnog fluida. Ni na kojoj dubini nema fazne granice, odnosno ne postoji čvrsta površina na koju se može stati ili tekuća u koju se može zaroniti.

Dno atmosfere definira kao dubina od 1000 km (1/70 polumjera planeta). U atmosferi je utvrđena prisutnost vodika, metana, helija, amonijaka, amonijeva hidrosulfida i smrznute vode. Pretpostavlja se da postoje i drugi spojevi (vodikov sulfid, različiti organski spojevi, kompleksni anorganski polimeri).

Jupiter se vrlo brzo vrti što, uz njegov velik promjer, uzrokuje jake centrifugalne sile, pa je izrazito spljošten prema polovima; ekvatorski mu je promjer 142 800 km, a polarni samo 134 000 km. Atmosfera mu je raslojena na pojaseve i zone. Rotacija mu je nejednolika: na ekvatoru jedan okret traje 9 h, 50 min, 30 s, a na 10° sjeverne ili južne širine 9 h, 55 min, 41 s.

Jupiter ima oko 10 puta veće magnetsko polje od Zemlje. U njegovoj su atmosferi zamjetljive meteorološke i magnetske pojave slične onima na Zemlji, ali mnogo veće raširenosti i trajanja (na primjer oluje slične tropskim ciklonima). Do sada je otkriveno 79 Jupiterovih satelita, a četiri najveća otkrio je Galileo Galilei (do 1610.; galilejanski sateliti). Dva najveća, Ganimed i Kalista, veći su od planeta Merkura. Potom slijede Ija i Europa, približno veličine Mjeseca.

Motrenja pomrčine Jupiterovih satelita služila su u pomorstvu za određivanje položaja broda, zemljopisne dužine, u doba kada nije bilo pouzdanih kronometara ni radiosignala. Na temelju neravnomjernosti u pojavama pomrčina satelita, s obzirom na njihovu udaljenost od Zemlje, izračunao je Ole Rømer prvi put brzinu svjetlosti. Jupiterovi prsteni sastoje se od čestica mikroskopske veličine. Prošireni Halo prsten udaljen je od središta planeta 1,40 do 1,72 Jupiterovog polumjera, najsjajniji Glavni prsten na udaljenosti je od 1,72 do 1,81 polumjera, a rijetki Paučinasti (engl.: Gossamer Ring) prsten udaljen je 1,81 do 3 polumjera. Jupiter,  "Hrvatska enciklopedija", Leksikografski zavod Miroslav Krleža, www.enciklopedija.hr, 2014.

Jupiter je prividno četvrto najsjajnije nebesko tijelo, nakon Sunca, Mjeseca i Venere.

Dobio je ime po vrhovnom bogu starih Rimljana, kojeg su Grci zvali Zeus. (Vidi Jupiter). Po uzoru na stara češka imena planeta, kajkavci su jedno vrijeme upotrebljavali ime Kraljomoć (Kralyomoch po starom kajkavskom pravopisu). Danicza Zagrebechka, ili Dnèvnik za prözto leto 1834, Vu Zágrebu, pritizkana vu Ferencza Suppan Szlovarniczi: str. 8.

 Fizička svojstva

 Atmosfera
thumb|lijevo|400px|Pogled na Jupiterov južni pol s letjelicom Juno, boje i kontrasti su umjetno snažno naglašeni.
Jupiterova atmosfera sastoji se od gustih slojeva oblaka čija visina seže do 1000 kilometara. Slojevi oblaka dijele se u tri glavne skupine koji se međusobno razlikuju po boji, s prugama usporednim ekvatoru. Rub Jupiterovog diska je prividno zatamnjen, jer tu pogled prodire kroz deblji sloj atmosfere. Među oblačnim prugama razlikuju se blijedožute zone i tamniji pojasevi blagih crvenkastosmeđih nijansi. Na vrhu atmosfere se nalaze crvenkasti oblaci čiji sastav je mješavina leda i vode. Kristali amonijevog hidrogensulfida čine bijele i smeđe oblake koji su u središnjem dijelu atmosfere. Dno atmosfere pokrivaju slabašno plavičasti oblaci koji svoju boju zahvaljuju kristalima amonijakovog leda.

Općenit sastav po masenom udjelu je 75 % vodika i 23 % helija, koji se u planetologiji nazivaju "plinovima" jer se nekoć nisu mogli ukapljiti pa su se smatrali "permanentnim plinovima", otud naziv "plinoviti div" - po kemijskom sastavu, a ne agregatnom stanju. Ostatak otpada na vodenu paru, metan, amonijak i slične kemijske spojeve.

Sa Zemlje prate se promjene širine, boje i kontrasta zona i pojasa te razne pjege, od kojih je Velika crvena pjega najviđenija i najstalnija pojava. To je područje eliptičnog oblika u Jupiterovoj atmosferi čija je veličina otprilike 12 000 x 25 000 km. Velika crvena pjega je velika oluja koja traje već stoljećima. Vjetrovi koji u njoj pušu mogu premašiti brzinu od 600 km/h. Područje Velike crvene pjege nije jedino aktivno - cijela atmosfera je vrlo turbulentna i aktivna. Prosječna brzina vjetra u gornjim slojevima atmosfere je 500 km/h.

Brzina vrtnje Jupitera određena je nakon dugogodišnjih promatranja uočljivih znakova. U ekvatorskom području, 7° na jug i sjever, prosječan period vrtnje (rotacije) jednak je 9 sati 50 minuta i 30 sekundi. Znakovi na većim jovigrafskim širinama otkrivaju duži period. Različit period vrtnje različitih širina svojstvo je nebeskih tijela koja nisu kruta. Period rotacije pojedinih detalja u oblacima drukčiji je zbog atmosferskih gibanja. Velika crvena pjega u razmaku od stotinu godina imala je prosječan period 9h 55 min 38 s. Period rotacije fluida neposredno ispod atmosfere određen je uz pomoć radio valova i pojava u magnetskom polju, koje se okreću s istom brzinom, na 9 h 55 min 29,7 s.

Stanje atmosfere i cijelog Jupitera razmatra se na temelju poznavanja strukture tvari u najširem rasponu fizičkih uvjeta. Zbog velike mase planeta, tlak se u dubini penje na više desetaka milijuna bara. Tlakovi i temperature koji vladaju u unutrašnjosti Jupitera dovode do agregacijskog stanja vodika koje se naziva superkritičnim fluidom, a na još većinom dubinama takav vodik postaje električno vodljiv kao metal, pa se naziva metalni vodik.Vladis Vujnović: "Astronomija", Školska knjiga, 1989. Vodik u Jupiteru ne može biti tekuć jer je na dubinama gdje vladaju dovoljni tlakovi za ukapljivanje vodika temperatura puno viša od kritične temperature vodika.

Na manjim dubinama, gdje je tlak 20-30 bar, vodik je u plinovitom stanju. Ta dubina uzima se kao baza atmosfere.

 Kemijski sastav
Kemijski sastav atmosfere divovskih planeta obilježen je obiljem vodika i helija; na vodik otpada 5 puta veći obujam nego na helij. Osim tih dvaju kemijskih elemenata, spektrografski je ustanovljen metan (CH4), amonijak (NH3) i vodena para (H2O), uz tragove etana (C2H6), etina (C2H2, fosfina (PH3) i ugljikovog monoksida (CO). Za svijetle zone ustanovljeno je da se sastoje od kristala amonijaka. One su oblačni sloj ograničen na neke jovigrafske širine. U procijepu između zona zapaža se niži neprekinuti sloj; pojasi su samo vidljivi dijelovi tog sloja. Žućkastonarančaste i smeđe nijanse pojasa tumače se kristalima amonijevog hidrogensulfida (NH4HS), a crvena boja nekih detalja, kao i Velike crvene pjege, tumače se kristalima fosfora. Ispod sloja pojaseva nalazi se treći, najniži sloj oblaka, koji se neposredno ne može vidjeti, a sastoji se od kristala vode.

 Temperatura atmosfere
Temperatura raste od razine gdje tlak iznosi 0,1 bar, na obje strane, i prema dolje, i prema gore, u ionosferu. Najniža temperatura iznosi oko 100 K (−173 °C). Temperature su određene opažanjem infracrvenog i radio valnog zračenja planeta. Prosječna temperatura koju otkriva Jupiterovo zračenje jednako je 140 K (−133 °C), što je za 20 K više od ravnotežne temperature, temperature koju bi imao da mu je jedini dotok energije sa Sunca. Do vanjskih slojeva Jupitera stiže od Sunca 51 W/m2 (Sunčeva konstanta). Stoga se temperatura od 140 K dade rastumačiti jedino vlastitim izvorom energije smještenim na Jupiteru. Jupiter sam zrači nešto manje od Sunčeve konstante. Izvorom energije moglo bi biti stezanje planetskog tijela koje se odvija zbog vlastite gravitacijske sile. Ili se stezanje nastavlja i danas (za opaženu količinu energije bilo bi dovoljno da se polumjer godišnje smanji za 1 mm), ili je proces zaustavljen, a Jupiter samo otpušta nakupljenu toplinu.

Jupiter ima dva izvora topline. Zbog unutarnjeg izvora topline razlike u temperaturi oblaka između ekvatorskih i polarnih krajeva iznose svega nekoliko stupnjeva. Zato Jupiterova klima malo ovisi o Sunčevoj toplini. Meridionalna cirkulacija, dizanje masa u ekvatorskom području i spuštanje u polarnom, zamaskirana je brzom vrtnjom (rotacijom).

Brza rotacija je treća okolnost koja bitno određuje ponašanje atmosfere. Zbog nje je građa oblačnog pokrova uređena u smjeru vrtnje. No rotacija dovodi i do veoma zavojitih gibanja zračnih masa koje se pokreću u smjeru juga ili sjevera. Smjer zakretanja ovisi o tome giba li se masa na sjevernoj ili na južnoj polutki. Na sjevernoj vjetrovi skreću udesno, na južnoj ulijevo. Učinak je izražen mnogo jače nego na Zemlji, a izazvan je Coriolisovom silom (inercijska sila što se javlja u sustavu koji se vrti).

Pri niskim temperaturama energija se prenosi veoma sporo, bilo da se prenosi zračenjem ili vođenjem. Dijelovi atmosfere sporo se hlade i sporo zagrijavaju. U zoni zrak se diže i hladi, a zatim ispunjava područje nižeg tlaka, to jest ponire u područje pojasa. Okomito atmosfersko kruženje odvija se u ravnini meridijana, pa dolazi do skretanja zračnih masa. Kada vjetar skrene u smjer paralele, skretanje prestaje, jer Coriolisova sila ne djeluje na tijela koja se gibaju po paralelama vodoravno (Coriolisova sila je inercijska sila koja se javlja u sustavu kada pokretno tijelo mijenja udaljenost od osi vrtnje). Sjeverna granica zone pokazuje strujanje u smjeru vrtnje (rotacije), a južna suprotno; na južnoj je polutki sve obratno.

 Velika crvena pjega
Pri dodiru slojeva koji se gibaju suprotnim smjerovima dolazi do vrtložnog gibanja, javljaju se valovi i pjege, u kojima se odvija ciklonalno i anticiklonalno gibanje. Jedna takva pjega je i Velika crvena pjega, kojoj je veličina 15 000 x 15 000 km. Ona je preživjela više stoljeća. Period njezina obrtanja iznosi 6 dana. Jedna manja pjega koja ponekad prođe kraj Velike crvene pjege viđa se više od 40 godina. Mnogobrojni ovalni vrtlozi i valovi dugotrajnog su obilježja zato što plove u jednoličnom sredstvu, u kojemu se toplina sporo prenosi s jednog mjesta na drugo. Još nije objašnjena dugovječnost Velike crvene pjege.

 Ionosfera
Iznad oblaka neposredno se nastavlja ionosfera. Ona se pruža daleko u prostor i obuhvaćena je magnetosferom, područjem sa svojstvenim oblikom magnetskog polja. Koncentracija elektrona u ionosferi iznosi najviše od 105 do 106 ion/cm3, u predjelu prvih 3000 km iznad oblačnog sloja. Temperatura ovdje premašuje 1000 K, no količina sadržane topline je, zbog praktičnog vakuuma, vrlo sitna.

mini|720px|center| Građa Jupitera.

 Svojstva unutrašnjosti planeta
mini|desno|300px|Veliki plinoviti planet kao Jupiter sadrži velike količine metalnog tekućeg vodika u unutrašnjosti (prikazano sivom bojom).

mini|desno|300px|Jupiter (crveno) obiđe Sunce (u sredini) dok Zemlja (plavo) obiđe oko Sunca 11,86 puta.

Mjerenja gravitacijskog polja ukazuju na postojanje značajne koncentracije stjenovitog i ledenog materijala u Jupiterovoj unutrašnjosti, vjerojatno jezgre mase 10 do 15 puta veće od Zemlje. Tlak u unutrašnjosti Jupitera dostiže više desetaka milijuna bara.

Na stjenovitu jzgru nastavlja se debeli sloj metalnog vodika. Naime, pri tlaku od oko 2 × 1011 Pa, vodik prelazi u metalno tekuće stanje. To je stanje pri kojem su molekule vodika tako gusto složene da pojedine atome susjedna molekula privlači jednako kao i atom partner u istoj molekuli. Posljedica toga je razbijanje molekula. Pored toga događa se da i elektrone u ljuskama privlače susjedne jezgre, pa dolazi do ionizacije (odvajanja elektrona od jezgri). Vodik postaje vrlo vodljiv (slično metalima), pa se zato ovo stanje zove metalni vodik. Ovaj sloj vjerojatno sadrži i primjese helija i raznih volatila. Postojanje metalnog vodika je dokazano u laboratorijima na Zemlji 1996.

Na sloj metalnog vodika se u blagom prijelazu nastavlja sloj vodika i helija u molekularnom obliku stanju superkritičnog fluida, a ovaj prelazi u plinovito bliže površini. Iz svemira vidljiva atmosfera samo je vanjski dio ovog sloja. Ovaj sloj sadrži i manje količine vode, ugljikovog dioksida, metana i drugih jednostavnih spojeva.

Jupiter je po sastavu 90 % vodik i 10 % helij (po volumnom udjelu), s tragovima vode, metana i amonijaka. Taj sastav približno odgovara i sastavu prvotnog oblaka od kojeg je i nastao Sunčev sustav.

Jupiterova unutrašnjost je vrlo vruća, temperature u središtu su čak 20 000 K, pa Jupiter 1,5 puta više energije zrači u svemir nego što je prima od Sunca. Ravnotežna temperatura (ona koju bi imao da ga grije samo Sunce) za Jupiter iznosi 140 K, ali je stvarna temperatura njegovih vanjskih dijelova oko 160 K. To se objašnjava Kelvin-Helmholtzovim mehanizmom (potencijalna energija gravitacijskog polja sažimanjem prelazi u unutarnju energiju).

Postoji urbani mit da Jupiteru nedostaje samo malo mase da bi postao zvijezda. Iako velik, Jupiter je po dimenzijama vrlo daleko od zvijezda ili smeđih patuljaka. Trebala bi mu oko 80 puta veća masa da u njegovu središtu tek započnu nuklearne reakcije s deuterijem.

 Orbita
Jupiter je jedini planet čiji baricentar sa Suncem leži izvan volumena Sunca, iako za samo 7 % Sunčevog polumjera. – See section 3.4. Prosječna udaljenost između Jupitera i Sunca je 778 milijuna km (oko 5,2 puta veća od prosječne udaljenosti između Zemlje i Sunca, ili 5,2 AU) i Jupiter svoju stazu oko Sunca obiđe za 11,87 godina. To je otprilike dvije petine orbitalnog razdoblja Saturna, tvoreći orbitalnu rezonancu između dva najveća planeta Sunčevog sustava. Eliptična orbita Jupitera nagnuta je 1,31° u odnosu na Zemlju. Kako je ekscentričnost njegove orbite 0,048, udaljenost Jupitera od Sunca varira za 75 milijuna  km između najbližeg pristupa (perihel) i najveće udaljenosti (afel). Zbog eliptičnosti putanje udaljenost između Jupitera i Sunca se mijenja od 4,95 do 5,5 AJ.

 Vrtnja ili rotacija
Jedan Jupiterov dan traje 9 sati i 50 minuta. Zbog te brze rotacije na Jupiteru nastaju snažna vrtloženja i turbulencije u atmosferi. Periodi rotacije se razlikuju od sloja do sloja zbog različitih atmosferskih gibanja.

Jupiterov nagib je relativno mali: samo 3,13°. Kao rezultat toga, ona ne doživljava značajne sezonske promjene, za razliku od, primjerice, Zemlje i Marsa.

Jupiterova rotacija najbrža je od svih planeta Sunčevog sustava, dovršavajući rotaciju na svojoj osi za nešto manje od deset sati; ovo stvara ekvatorijalno ispupčenje koje se lako vidi kroz amaterski teleskop sa Zemlje. Planet je oblikovan kao sferoid, što znači da je promjer njegovog ekvatora duži od promjera izmjerenog između Jupiterovih polova. Na Jupiteru ekvatorijalni promjer je 9,275 km duži od promjera izmjerenog kroz polove.

Budući da je planet fluidno tijelo, njegova gornja atmosfera prolazi kroz diferencijalnu rotaciju. Rotacija Jupiterove polarne atmosfere je oko 5 minuta duža od one u ekvatorijalnoj atmosferi; kao referentni okvir koriste se tri sustava, osobito pri graficiranju gibanja atmosferskih značajki. Sustav I primjenjuje se od zemljopisnih širina 10° S do 10° J; njegovo je ophodno vrijeme najkraće na planetu, te iznosi 9h 50m 30,0s. Sustav II primjenjuje se na svim geografskim širinama sjeverno i južno od njih; njegovo razdoblje je 9h 55m 40,6s. Sustav III prvi su definirali radioastronomi i odgovara rotaciji magnetosfere planeta; njegovo razdoblje je službena rotacija Jupitera.

 Magnetosfera
thumb|200px|Jupiterovi radio-izboji.
Godine 1955. otkrivena je radio-emisija s Jupitera, što je upućivalo na jako magnetsko polje. Jako magnetsko polje Jupitera posljedica je debelog sloja metalnog vodika i brze vrtnje (rotacije). Magnetska je os priklonjena za 11° prema osi rotacije. Smjer magnetskog polja suprotan je magnetskom polju na Zemlji, što znači da je sjeverni magnetski pol zaista na sjevernoj polutki planeta. U atmosferi, ono iznosi oko 10-3 T (4000 puta jače od Zemljinog). Jupiterovo magnetsko polje je oko 100 puta veće od Zemljinog. Proteže se nekoliko milijuna kilometara u smjeru Sunca i čak oko 650 milijuna km u suprotnom pravcu, te doseže i do Saturnove putanje. Magnetsko polje stvara jake struje visoko-energetskih čestica koje su 10 puta jače od onih u Zemljinim Van Allenovim pojasima. Ono obuhvaća i putanje Jupiterovih satelita, pa se time djelomično objašnjava velika vulkanska aktivnost na Iji. Između Jupitera i Ije izmjerena je električna struja jakosti 5 megamapera. Naelektrizirane čestice ubrzane do vrlo velikih brzina udaraju u Ijinu površinu i izbijaju atome s površine. Izbijeni atomi čine Ijin torus, veliki prstenasti oblak električki nabijenih čestica oko Ijine putanje. Do položaja na kojem se nalazi satelit Ija magnetosfera se vrti s jednakom kutnom brzinom kao i Jupiter. Ona je izvor dekametarskih radio valova promjenjive jačine, uzrokovanih električnim pražnjenjima. Uopće je Jupiter jedan od relativno najjačih izvora svemirskih radio valova koji se detektiraju sa Zemlje. Snimljene su munje i polarna svjetlost. Iz magnotosfere znadu se osloboditi električke čestice i u obliku kozmičkih zraka stići do Zemlje, a zabilježene su i kod Merkura.
 Jupiterovi prsteni

mini|desno|300 px|Jupiterovi prsteni i Jupiterovi unutarnji sateliti.

Godine 1979. svemirska letjelica Voyager 1 je otkrila Jupiterove prstene. Prsteni se uglavnom sastoje od mikrometarskih čestica prašine, a prostiru se sve do površine planeta. Prsteni su male gustoće, polumjera 129 000 km, a njihova debljina manja je od 30 km. Najbliži Jupiteru je Halo prsten, širok oko 20 000 km, koji ima oblik torusa. Na Halo se nastavlja 7000 km široki Glavni prsten. Unutar glavnog prstena se nalaze i Jupiterovi sateliti Metida i Adrasteja. Smatra se da su ova dva satelita izvor materijala (udari meteorita izbacuju krhotine u svemir) za Glavni pojas, dok su druga dva mala unutarnja satelita – Amalteju i Tebu – izvori materijala za vrlo rijetke Amalthea Gossamer (unutar Amaltejine putanje) i Thebe Gossamer (između putanja Amalteje i Tebe) prstene koji se nastavljaju na Glavni prsten (Paučinasti prsteni).

 Prirodni sateliti
mini|desno|300px|Jupiter i galilejanski sateliti.

mini|desno|300px|Jupiter i Ganimed (dolje lijevo) foto: Voyager 1, izvor: NASA/JPL)

mini|desno|300px|Jupiterov mjesec Ija.

mini|desno|300px|Jupiterov mjesec Europa.

mini|desno|300px|Jupiterov mjesec Ganimed.

mini|desno|300px|Jupiterov mjesec Kalista.

Prema dosadašnjim saznanjima oko Jupitera kruže 79 prirodna satelita. Razdvajanje po skupinama napravljeno je po svojstvima nebeskih tijela kao i po svojstvima njihovih putanja. Na primjer galilejanski sateliti su veliki i nalik su malim planetima, dok su sateliti iz skupine Ananke ili iz skupine Amalteja mala tijela nepravilnog oblika i asteroidnog podrijetla. Kako su mase galilejanskih satelita velike, usporedive s masom Mjeseca, to oni jedan drugome znatno remete staze. Iako su im ekscentriciteti maleni, oni se ipak neprekidno mijenjaju. Zbog velikog broja prirodnih satelita, postoji podjela po sljedećim skupinama:
 Jupiterovi unutarnji sateliti
 Galilejanski sateliti (Io, Europa, Ganimed, Kalista)
 Temisto
 Himalija
 Ananka
 Karma
 Karpo
 Pasifaja

 Jupiterovi unutarnji sateliti

Jupiterovi unutarnji sateliti su Amalteja, Metida, Adrasteja i Teba, a to su nepravilna, planetoidna tijela, i nalaze se s vanjske strane prstena. Prsten je male gustoće. Vanjski mu polumjer iznosi 129 000 km. Najsjajniji dio prstena širok je 6000 km. Bliže Jupiteru sjaj mu veoma opada, no tvar se, sve usitnjenija, prostire do površine Jupitera. Tipične čestice veličine su 1 μm. Debljina prstena manja je od 30 km, no oko njega zapaža se jedan svijetleći halo mnogo veće širine. Amalteja je stijena nepravilna oblika, crvena je i tamna. U središte Jupitera stalno je uperena njena duža os. Orbite satelita su unutar Rocheove granice, pa će, čak i ako zbog svojih malih dimenzija i izbjegnu raspad, prije ili kasnije pasti na Jupiter.

 Galilejanski sateliti

Galilejanski sateliti (Io ili Ija, Europa, Ganimed, Kalisto) po sfernom obliku, čak i po veličini sliče terestričkim plenetima. Kao i prva skupina satelita, oni se gibaju u ravnini Jupiterova ekvatora, a staze su im slabo izdužene. Ophodno vrijeme iznosi im od jednog do desetak dana. Period vrtnje sinkroniziran je s periodom obilaska, a to znači da uvijek jednom stranom gledaju prema Jupiteru. Najveći među njima i ujedno najveći Jupiterov satelit je Ganimed. Gustoća tih satelita opada po redu udaljenosti. To se svojstvo ne protivi predodžbi da su svi oni stvoreni u okolini Jupitera i s njime istodobno. Pred sobom imamo Sunčev sustav u malom. Krajolici galilejanskih satelita iznenađujući su. Sudeći po prosječnoj gustoći, Io i Europa pretežno su izgrađeni od silikata, a Ganimed i Kalisto od jednakih dijelova silikata i vode.

 Ija ili Io

Io ili Ija ima najsnažnije vulkansko djelovanje od svih tijela Sunčeva sustava. Po veličini i gustoći nalik je Mjesecu. Prekriven je slojevima crvenonarančaste boje, sa svjetljiježućkastim i bijelim površinama, te tamnim mrljama. Čitava je površina proizvod vulkanske djelatnosti. Pritom je ekvatorsko područje aktivnije. Osim vulkana ima i planina, visokih do 10 km. Postoje mnogobrojni rasjedi i pukotine, duge nekoliko stotina kilometara. Tipičan vulkanski oblik je kaldera. Jedna polutka sadrži stotinjak kaldera mjera većih od 20 km. Najveće imaju i 250 km. Čitavih 5 % površine prekrivaju kaldere. One su obično zagaravljene, crnosmeđe i blagih padina, a oko njih se šire valovi i rijeke krute lave, u raznim nijansama žutocrvenog. U vrijeme erupcije, lava s plinovitim oblakom izbija s brzinom od 500 do 1000 m/s i diže se uvis 70 do 300 km.

Boje tla dadu se rastumačiti sumporom i sumporovim dioksidom. Vrlo rijetka atmosfera sastoji se od sumporovog dioksida. Vodena para nije uočena. Kako je voda jedan od glavnih sastojaka vulkanizma na Zemlji, nedostatak vodene pare na Io znak je da je unutrašnjost dehidrirana. Talište sumpora nalazi se na temperaturi od 385 K (112 °C). U toku erupcije sumpor se hladi i pokriva tlo, a pri naglom hlađenju poprima razne nijanse. Velike bijele površine vjerojatno su snijeg ili mraz od sumpora ili sumporovog dioksida. Vulkanizam je uvjetovan rastaljenom unutrašnjosti. Izvor topline mogle bi biti plime (plimna sila). Iako je Io Jupiteru blizu kao i naš Mjesec Zemlji, zbog mnogo puta veće Jupiterove mase, plime su razmjerno veće. Energija se prenosi na tijelo satelita trenjem plimnog vala, no ako je vrtnja sinkronizirana, plimni val je stojni. Tada se energija dobiva jedino ako se jakost plime mijenja, pa se nebesko tijelo steže i rasteže. Premda je staza Io slabo izdužena, poremećenja do kojih dolazi posebno zbog utjecaja Europe dovode do ritmičkog mijenjanja udaljenosti do Jupitera, pa se i plimni val ritmički diže i spušta. Tim bi mehanizmom Io bio u središtu rastaljen još od vremena nastanka. Druga je mogućnost da se Io zagrijava jakim električnim strujama koje teku u Jupiterovoj magnetosferi. Zagrijavanje satelita ma kojim od mehanizama u dugim je geološkim razdobljima trebalo dovesti do razdvajanja kemijskih sastojaka po dubini. Lako hlapljivi sastojci, poput vode, napustili su planet, a obilni sumpor izdigao se iz unutrašnjosti do površinskih slojeva debljine od nekoliko kilometara.

Zbog vulkanske erozije današnji reljef kore nije stariji od 10 do 100 milijuna godina, nema stoga ni jednog vidljivog meteoritskog kratera. Vulkanska aktivnost praćena je izdvajanjem topline. Pojedini dijelovi površine imaju temperaturu od 500 K. U infracrvenom području, Io zrači oko 2 W/m2, što se dade usporediti s najaktivnijim geotermalnim predjelima, s tom bitnom razlikom što je ovdje snaga zračenja raspoređena po čitavu globusu satelita.

 Europa

Europa je posve prekrivena ledom i mnogo je sjajnija od Mjeseca, od kojega je i nešto manja. Ledenu površinu šaraju izlomljene sivkaste pruge, duge više tisuća kilometara, široke stotinu kilometara. Inače površina ne pokazuje nikakve osobite visinske razlike. Sivkaste pruge nisu pukotine u kori već, vjerojatnije, ponovno zaleđeni razmak među ledenim santama. U području sumračnice uočeni su hrptovi visine nekoliko stotina metara. Zavojiti su, široki do deset, a dugi više od stotinu kilometara. Dio površine poprskan je tamnim mrljama, koje se pri većem povećanju razlučuju u udubine i izbočine. Nađeno je nekoliko udarnih kratera, promjera oko 20 km. Površina Europe zapravo je ledena santa premale čvrstoće da sačuva kratere i sama je stalno podvrgnuta promjenama. Zato je i razmjerno mlađa, možda oko sto milijuna godina.

 Ganimed

Ganimed ima površinu geološki veoma raznoliku. Starija je površina tamnija, mlađa svjetlija. Trećinu polutke okrenute od Jupitera zauzima tamni oval. Predjel Galileja (lat. Regio Galileo), dugačak je oko 4000 km. U reljefu se vide mnogobrojni udarni krateri, s bijelim zrakama i bez njih; one prestavljaju led izbačen iz kore (rastopljen i ponovo zaleđen). Nema mnogo velikih kratera. Svojstveni dijelovi reljefa su trakasti sustavi usporednih planina, koji znadu teći jedan preko drugoga kao da su češljani. Trake su duge više stotina kilometara, uže od 100 km, a sadrže desetak usporednih planina. Ima terena nevjerojatno izmiješanih oblika. Zapažaju se i pomaci velikih površinskih ploča, klizanja i razmicanja, nastala pucanjem i širenjem kore.

 Kalista

Kalista je tijelo Sunčeva sustava s najvećom gustoćom kratera. Prekrivaju se tako da između njih nema zaravni. Najtamniji je od svih galilejanskih satelita, i s malo kontrasta. Reljef je veoma gladak, što znači da u kori s vremenom dolazi do zaravnjavanja udarnih deformacija. Njegova kora mora teći kao što na Zemlji teku ledenjaci, spuštajući se u doline. Krater se akumulirao preko kratera i postupno tonuo u dubinu, ili je bio preliven svježim ledom. Ne vide se krateri veći od 150 km. Nema planina, što također govori o slaboj nosivosti kore. Najveća značajna pojava je Valhalla, sustav koncentričnih krugova s polumjerom od 1 500 km, nastao padom velikog tijela. Tijelo je probilo ledenu koru i rastalilo je, a ona se ponovo ukrutila u vidu kružnih valova na vodi.

 Grupa Temisto
Temisto je mali Jupiterov satelit između putanja Kalista i Lede, otkriven je 30. rujna 1975., ali mu se zagubio trag sve do 2000. godine kada je ponovno pronađen. Zbog toga je ovaj satelit do listopada 2002. imao dva privremena imena: S/1975 J 1 i S/2000 J 1. Temisto je prvi satelit izvan orbita 8 najbližih satelita (4 unutrašnja + 4 velika galilejanska). Temisto se giba progradno (ili direktno, to jest u smjeru Jupiterove rotacije). Temisto je jedini član grupe Temisto čiji su članovi progradni nepravilni sateliti. Srednji promjer mu iznosi tek oko 8 km.

 Grupa Himalija

Himalija, Leda, Liziteja, Elara i S/2000 J 11 iz te skupine imaju staze veoma izdužene i nalaze se u ravnini za 30° nagnutoj prema Jupiterovu ekvatoru, a svi su gotovo u jednoj ravnini. Srednje udaljenosti malo im se razlikuju, pa im se mnogo ne razlikuje ni ophodno vrijeme.

 Grupa Ananka

Grupa Ananka je grupa Jupiterovih prirodnih satelita sa sličnim parametrima orbite. Ova grupa spada među Jupiterove retrogradne nepravilne satelite. Oni su znatno izduženih staza, no bitna im je karakteristika retrogradno kretanje. Maleni su i nepravilna oblika. Grupa ima između 7 i 16 članova, ovisno o tome koliko strogo shvaćamo definiciju grupe. Poznati članovi uže grupe, redom od većih prema manjim, su: Ananka (najveći satelit, po njemu se zove grupa), Praksidika, Jokasta, Harpalika, Tiona, Euanta, Euporija. Dodatnih 9 rubnih članova grupe su: S/2003 J 16, Mnema, S/2003 J 3, S/2003 J 18, Ortozija, Telksinoa, Hermipa, Helika, S/2003 J 15.

 Grupa Karma

Grupa Karma je grupa Jupiterovih prirodnih satelita sa sličnim parametrima staze. Samo jedan satelit izlazi iz okvira grupe i ima ekscentricitet izvan (0,4295) raspona i to od 0,23 do 0,27. Ova grupa spada među Jupiterove retrogradne nepravilne satelite. Grupa ima 17 članova. Redom od Jupitera prema vani, to su: S/2003 J 17, S/2003 J 10, Pasiteja, Haldena, Arha, Izonoa, Erinoma, Kala, Aitne, Tajgeta, S/2003 J 9, Karma (najveći satelit, po njemu se zove grupa), S/2003 J 5, S/2003 J 19, Kalika, Eukelada i Kalihora.

 Grupa Karpo
Grupa Karpo ima samo satelit Karpo (također Jupiter XLVI). Progradni nepravilni satelit s oko 3 kilometra u promjeru i ophodnim vremenom od 458,625 dana.

 Grupa Pasifaja

Grupa Pasifaja je grupa Jupiterovih prirodnih satelita sa sličnim parametrima putanje. Ova grupa spada među Jupiterove retrogradne nepravilne satelite. Za razliku od preostale dvije retrogradne grupe Jupiterovih nepravilnih satelita (grupa Ananka i grupa Karma), ova je grupa vrlo raspršena po inklinaciji, što se tumači velikom starošću grupe koje se od vremena svojeg nastanka postepeno raspršila. Grupa ima 13 članova. Redom od Jupitera prema vani, to su: Euridoma, S/2003 J 23, Hegemona, Pasifaja (najveći satelit, po njemu se zove grupa), Sponda, Kilena, Megaclite, S/2003 J 4, Kaliroa, Sinopa, Autonoa, Aeda i Kora.

 Interakcija sa Sunčevim sustavom
mini|250px|"Trojanci" i "Grci" u Jupiterovoj orbiti.
Zajedno sa Suncem, Jupierov veliki gravitacijski utjecaj pomogao je oblikovanju Sunčevog sustava. Orbite većine planeta sustava leže bliže Jupiterovoj orbitalnoj ravnini od Sunčeve ekvatorijalne ravnine (Merkur je jedini planet koji je bliži Sunčevom ekvatoru u orbitalnom nagibu), Kirkwoodove zone u asteroidnom pojasu uglavnom uzrokuje Jupiter, te je možda bio odgovoran za kasno teško bombardiranje unutarnjeg Sunčevog sustava u prošlosti.

Zajedno sa svojim mjesecima, Jupiterovo gravitacijsko polje kontrolira brojne asteroide koji su se naselili u regije Lagrangieove točke u Jupiterovoj orbiti oko Sunca. Oni su poznati kao trojanski asteroidi, a podijeljeni su na grčke i trojanske "logore" u spomen na Ilijadu. Prvi od njih, 588 Ahil, otkrio je Max Wolf 1906. godine; od tada je otkriveno više od dvije tisuće. Najveći je 624 Hektor.

Zbog veličine Jupiterove mase, težište između njega i Sunca leži neposredno iznad Sunčeve površine.

 Udari
mini|250px|Infracrvena snimka udara kometa Shoemaker-Levy 9 (lijevo) u Jupiter (sredina). Svijetla točka na desnoj strani je Io.
Jupiter je nazvan usisavačem Sunčevog sustava, zbog njegovog ogromnog gravitacijskog potencijala i položaja u blizini unutarnjeg Sunčevog sustava. Primjećuje se najčešće udare kometa planeta Sunčevog sustava. Smatralo se da planet služi kao djelomična zaštita unutarnjeg sustava od kometnog bombardiranja. Međutim, nedavne računalne simulacije sugeriraju da Jupiter ne uzrokuje neto smanjenje broja kometa koji prolaze unutarnjim Sunčevim sustavom, jer njegova gravitacija pertubira njihove orbite unutar otprilike onoliko često koliko ih skuplja ili izbacuje. Ova tema ostaje sporna među znanstvenicima, jer neki misle da on vuče komete prema Zemlji iz Kuiperovog pojasa, dok drugi misle da Jupiter štiti Zemlju od navodnog Oortovog oblaka. Jupiter doživljava oko 200 puta više udara asteroida i kometa od Zemlje.

Noviji otkriveni udari na Jupiter uključuju sljedeće:

 Vatrenu kuglu fotografirao je Voyager 1 tijekom susreta s Jupiterom u ožujku 1979.
 Tijekom razdoblja od 16. srpnja 1994. do 22. srpnja 1994. godine, preko 20 fragmenata kometa Shoemaker–Levy 9 sudarilo se s Jupiterovom južnom polutkom, pružajući prvo izravno promatranje sudara između dva objekta Sunčevog sustava. Zbog tog sudara mnogo je saznato o sastavu Jupiterove atmosfere.
 19. srpnja 2009. u sustavu II otkriveno je mjesto udara na dužini od približno 216 stupnjeva. Ovaj utjecaj ostavio je iza sebe crnu mrlju u Jupiterovoj atmosferi, sličnu veličinu kao Oval BA. Infracrveno promatranje pokazalo je svijetlu točku gdje se udar dogodio, što znači da je udar zagrijao donju atmosferu u području u blizini Jupiterovog južnog pola.
 Anthony Wesley, astronom amater u Australiji, 3. lipnja 2010. godine otkrio je vatrenu kuglu, manju od prethodnih, a kasnije je otkriveno da ju je snimio i drugi astronom amater na Filipinima
 Još je jedna vatrena kugla viđena 20. kolovoza 2010. godine.
 10. rujna 2012. otkrivena je nova vatrena kugla.
 17. ožujka 2016. snimljen je novi udar asteroida ili kometa u Jupiter.
7. kolovoza 2019. snimljen je novi masivan meteor kako udara u Jupiter.

 Promatranje
mini|225px|Jupiter kroz amaterski teleskop.
Jupiter je obično četvrti najsvjetliji objekt na nebu (nakon Sunca, Mjeseca i Venere); ponekad je Mars svjetliji od Jupitera. Ovisno o položaju Jupitera u odnosu na Zemlju, magnituda može varirati u veličini od jarke poput −2,94 pri opoziciji do –1,66 tijekom gornje konjunkcije sa Suncem. Srednja prividna magnituda iznosi –2,20 sa standardnim odstupanjem 0,33. Kutni promjer Jupitera također varira od 50,1 do 29,8 lučnih sekundi. Povoljne suprotnosti nastaju kada Jupiter prolazi kroz perihel, događaj koji se događa jednom po orbiti.

Zemlja prestiže Jupiter svakih 398,9 dana kad orbitira oko Sunca, u trajanju koje se naziva sinodičkim periodom. Kad to učini, Jupiter izgleda retrogradno u odnosu na pozadinske zvijezde. Odnosno, čini se da se Jupiter za jedno vrijeme kreće natrag prema noćnom nebu, čineći petlju.

Budući da je orbita Jupitera izvan one Zemljine, fazni kut Jupitera gledan sa Zemlje nikada ne prelazi 11,5°: Jupiter se uvijek pojavljuje gotovo potpuno osvijetljen kada se gleda putem zemaljskih teleskopa. Pogled na srpasto osvijetljen planet dobio se tek tijekom misija svemirskih letjelica na Jupiter.

Mali teleskop obično će pokazivati Jupiterova četiri galilejanska satelita kao svjetle točkice te zone i pojaseve oblaka u Jupiterovoj atmosferi. Veći teleskop pokazat će Jupiterovu Veliku crvenu pjegu kada je vidljiva sa Zemlje.

 Povijest istraživanja
mini|desno|300 px|Galileo Galilej pomoću teleskopa otkriva 4 prirodna satelita koji su prozvani: Io, Europa, Ganimed i Kalista. Ovu grupu priodnih satelita nazivamo galilejanskim satelitima.

mini|desno|300 px|Svemirska letjelica Galileo pred Jupiterom.

Zbog svoje vidljivosti golom oku na noćnom nebu Jupiter je bio poznat u antičkim vremenima. Godine 1610. Galileo Galilej pomoću teleskopa otkriva 4 prirodna satelita koji su prozvani: Io, Europa, Ganimed i Kalista. Ovu grupu prirodnih satelita nazivamo galilejanskim satelitima. Galileo je na Saturnu našao izrasline u obliku ušiju. Smatrao je da je to trojno tijelo. Da je to zapravo prsten, ustanovio je 1665. Christiaan Huygens koji je te godine otkrio i najveći Saturnov prirodni satelit, Titan. Ole Rømer je 1675. iskoristio pomrčine Jupiterovih satelita da ocijeni brzinu svjetlosti. Giovanni Domenico Cassini je u razdoblju od 1671. do 1684. otkrio 4 dalja Saturnova satelita i pukotinu unutar prstena (Cassinijeva pukotina). Viđao je i pjege na Jupiteru, te njegovu spljoštenost. Isaac Newton je spljoštenost rastumačio vrtnjom. Zatim je William Herschel 1781. otkrio Uran kao nebesko tijelo 6. prividne veličine. Uran je i prije bio viđen jer je u dometu vidljivosti oka. Herschel je 1787. otkrio Uranove satelite Titaniju i Oberona, a 1789. Saturnove satelite Mimas i Enkelad, te je odredio Saturnov period vrtnje.

Do otkrića Neptuna dolazi 1846. (Urbain Le Verrier i Johann Gottfried Galle), a u razmaku od dvije sedmice nađen je njegov pratilac Triton. Jedan točan položaj Neptuna iz 1612. pronađen je i u zapisima Galileia. James Clerk Maxwell je 1858. ustvrdio da je Saturnov prsten sastavljen od djelića (segmenata) meteorskog materijala, a J. Keller je to 1895. spektroskopski i dokazao. Pažnju astronoma zaokupljale su površine planeta od sedamdesetih godina 19. stoljeća. Izučavala se struktura Jupiterovih pruga, a 1878. obratila se pažnja na Veliku crvenu pjegu, iako je ona zapažena već od 1664. (Robert Hooke i Giovanni Domenico Cassini). Bljedunjave pruge nađene su još na Saturnu. Tridesetih godina 20. stoljeća spektroskopski je ustanovljeno prisustvo metana na svim velikim planetima, a amonijak je nađen samo na Jupiteru. Oko 1960. spektrom je dokazano i prisustvo vodika.

 Pioneer 10 & 11 i Voyager 1 & 2
Sa Zemlje je do sada poslano 7 svemirskih letjelica, koje su bile uspješne u svom cilju. Prva letjelica koja je uspjela stići do Jupitera bila je međuplanetarna sonda Pioneer 10, koja se 4. prosinca 1973. približila Jupiteru na 130 000 km. Točno godinu dana kasnije približio mu se na 43 000 km Pioneer 11. Poslala je prve slike niske rezolucije. Pioneer 10 je također vratila i telemetrijske podatke o magnetosferi i atmosferi Jupitera. Letjelice Voyager (Voyager 1 i Voyager 2) opremljene boljim kamerama i mjernim instrumentima nego letjelice tipa Pioneer. Voyager 1 je prišao Jupiteru 5. ožujka 1979. na daljinu od 278 000 km, snimajući još satelite Io, Ganimed i Kalista. Voyager 2 je obletio Jupiter 9. srpnja 1979. snimajući usto sve galilejanske satelite. Poslale su na Zemlju 1979. slike i telemetrijske podatke, što je pridonijelo proširenju znanja o planetu Jupiter, otkrivši sljedeće:
 orbitalne prstene koje opasuju planet slične onima oko Saturna, ali manje izražene
 nove satelite koje nisu bile opaženi prije, na primjer grupu satelita u porodici Amaltea koji su u niskoj orbiti iznad Jupitera i koji imaju promjer manji od 200 km

Ekspedicije svemirskih letjelica čine prekretnicu u izučavanju divovskih planeta i njihovih satelita. 4. ožujka 1979. otkriven je Jupiterov prsten. Saturn je primio posjet Pioneera 11. rujna 1979., Voyagera 1 u studenom 1980., a Voyagera 2 u kolovozu 1981. Voyagera 2 je u siječnju 1986., osam godina nakon lansiranja, stigao u najveću blizinu Urana, a 1989. i do Neptuna. Plin helij je na Jupiteru spektroskopski dokazan iz Pioneera 10. Na temelju opažanja u optičkom i radio valnom području, i sa Zemlje i s letjelica, te izravnim mjerenjima iz letjelica može se veoma sigurno govoriti o građi tijela koje pripadaju Jupiterovoj skupini planeta.

 Letjelica Galileo
Prva letjelica u orbitu Jupitera je sonda Galileo, koja je lansirana 18. listopada 1989., a ušla u orbitu 7. prosinca 1995.  Ona je kružila oko planeta više od sedam godina, obavila više preleta Galilejanskih satelita i Amalteje. Svemirska letjelica je također bila svjedok raspada kometa Shoeaker-Levy 9 dok se približavala Jupiteru 1994. godine, što je jedinstvenim opažanjem rezultiralo preciznim slikama udara. Njegov prvobitno dizajnirani kapacitet bio je ograničen neuspjelim postavljanjem njegove velike pojačane radio antene, iako su još uvijek dobijene opsežne informacije o Jupiterovom sustavu.

Atmosferska sonda od titana od 340 kilograma puštena je iz svemirskog broda u srpnju 1995. godine, ulazeći u atmosferu Jupitera 7. prosinca.  Padobranom je prošla kroz 150 km (93 milje) atmosfere brzinom od oko 2.575 km/h (1600 mph)  i prikupljao podatke 57,6 minuta prije gubitka signala pri tlaku od oko 23 Zemaljske atmosfere pri temperaturi od 153 °C. Zatim se rastopila i vjerojatno isparila. Orbiter Galileo doživio bržu verziju iste sudbine kad je 21. rujna 2003. namjerno survan u planet brzinom većom od 50 km/s kako bi se izbjegla mogućnost da se upadne u i možda kontaminira Europu, mjesec za koji je pretpostavljeno da ima života na njemu.

Podaci iz ove misije otkrili su da vodik čini do 90 % Jupiterove atmosfere. Zabilježena temperatura bila je veća od 300 °C (> 570 °F), a brzina vjetra izmjerena je više od 644 km/h (> 400 mph) prije nego što je sonda isparila u atmosferi.

 Letjelica Juno
NASA-ina misija Juno lansirana je 5. kolovoza 2011., a nakon pet godina putovanja stigla je na Jupiter 4. srpnja 2016., a dosada je napravila preko 20 polarnih orbita. 27. kolovoza 2016. svemirska letjelica dovršila je svoj prvi prelet Jupitera i poslala natrag prve slike Jupiterovog sjevernog polarnog područja, kao i južnog.

Planirano je da letjelica bude deorbitirana 30. srpnja 2021. kako bi se izbjegla moguća kontaminacija Europe, satelita za kojeg se smatra da je kandidat za izvanzemaljski život.

 Buduće letjelice
Sljedeća planirana misija na Jupiter će biti ESA-ina je Jupiter Icy Mjesec Explorer (JUICE), zbog lansiranja 2022. godine, a koja će doći do Jupitera 2029. godine, istraživati Jupiterove galilejanske mjesece, a onda ući u orbitu Ganimeda gdje će orbitirati do 2034., a 2023. NASA će lansirati misiju Europa Clipper, čiji je cilj napraviti 45 preleta Europe i otkriti ima li tamo života.
  Međuplanetarne sonde  Država
  Ime sonde
  Datum lansiranja
  Datum dolaska
  Kraj misije (za Jupiter)
  Opaska   Pioneer 10  3. ožujka 1972.  prosinac 1973.   Prelet pokraj Jupitera. Prve slike, podaci o magnetosferi.   Pioneer 11  6. travnja 1973.  prosinac 1974.   Prelet pokraj Jupitera. Slike, podaci o magentosferi.   Voyager 1  5. rujna 1977.  ožujak 1979.    Otkrio planetarne prstenove i nove satelite.   Voyager 2  20. kolovoza 1977.  lipanj 1979.    Slike galilejanskih satelita i atmosfere.   Galileo  18. listopada 1989.  7. prosinca 1995.  21. rujna 2003. Spustio sondu u Jupiterovu atmosferu. Velik broj slika Jupitera i satelita,       Cassini  15. listopada 1997.  30. prosinca 2000.    Prelet pokraj Jupitera na putu za Saturn.   New Horizons  19. siječnja 2006.  28. veljače 2007.    Prelet pokraj Jupitera na putu za Pluton.   Juno  5. kolovoza 2011.  5. srpnja 2016. 30. srpnja 2021.   Orbiter u polarnoj orbiti. Prve slike Jupiterovih polarnih regija u velikim detaljima.

 Planet Jupiter u romanima i filmovima

 U filmu 2001: Odiseja u svemiru iz 1968. Stanley Kubricka, Jupiter je središte radnje, dok u nastavku u filmu Odiseja 2010. (2010: Odyssey Two) (1984.) Jupiter se pretvara u zvijezdu s pomoću fiktivne tehnologije koja uspijeva povećati gustoću jezgre Jupitera. Razlog je pospješivanje novonastalog života na Europi.

 Vidi
 Vrući Jupiter
 Model velikog letanja (Grand Tack model)

 Izvori

 Vanjske poveznice

 Astronomska sekcija Fizikalnog društva Split – Jupiter

Jupiter's rings are made up of microscopic particles.

Question: what kind of particles are jupiter's rings made of

Jupiter's rings are made up of microscopic particles.

what kind of particles are jupiter's rings made of

Question: what is the brightest main ring on jupiter called

what is the brightest main ring on jupiter called

Question: what is made up of microscopic particles

Jupiterovi prsteni sastoje se od čestica mikroskopske veličine .

what is made up of microscopic particles

Question: what is a distance from the center of the planet jupiter

what is a distance from the center of the planet jupiter

Jupiter 's rings are made up of microscopic particles .

The extended Halo ring is a distance from the center of the planet from 1.40 to 1.72 Jupiter 's pencil , the brightest Main ring at a distance is from 1.72 to 1.81 pencil , and the rare Paučinasti ( English :

Jupiterovi prsteni sastoje se od čestica mikroskopske veličine.

Jupiter's rings are made up of microscopic particles. The extended Halo ring is a distance from the center of the planet from 1.40 to 1.72 Jupiter's pencil, the brightest Main ring at a distance is from 1.72 to 1.81 pencil, and the rare Paučinasti (English:

Jupiter's rings are made up of microscopic particles.

Jupiter's inclination is relatively small: only 3.13°.

As a result, it does not experience significant seasonal changes, unlike, for example, Earth and Mars.

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|
Every planet in the solar system has seasons. Most have four
like the Earth -- called Winter, Spring, Summer and Fall -- but
that's where the similarities end. Extraterrestrial seasons are
hardly noticeable on some planets (Venus), mindbogglingly extreme
on others (Uranus) and in some cases simply impossible to define
(Mercury).
Seasons
on Other Planets
The table below gives the dates of the seasons for 8 of the 9
planets in the solar system. Only Pluto is missing. It's so far
away that we don't know much about seasons on that distant world.
In the table the equinoxes and solstices are named after the
corresponding season in the northern hemisphere. This is the
convention that astronomers often use to discuss planetary seasons.
When the north pole of a planet is tilted toward the sun, astronomers
call it the Summer Solstice; when the south pole is tilted toward
the sun it is called the Winter Solstice. Nevertheless, the seasons
are always opposite in the two hemispheres. On Earth, for example,
when it is summer in New York, it is winter in Sydney. On a spring
day in Paris, autumn leaves are falling in Argentina, and so
on...
When the Vernal Equinox takes place on March 20, Earth will join
Venus and Jupiter as the only planets in the solar system where
it is now northern Spring.
|
||
||
||
vernal equinox
||
summer solstice
||
autumnal equinox
||
winter solstice
|
|
PLANET
||
e
|
orbital eccentricity
|
spin axis tilt (deg)
||
Spring begins
||
Summer begins
||
Autumn begins
||
Winter begins
|
|
Mercury
||
0.21
||
< 28
||
n/a
||
n/a
||
n/a
||
n/a
|
|
Venus
||
0.01
||
3
||
Feb 24, '00
|
1930 UT
|
Apr 1, '00
|
1600 UT
|
May 28, '00
|
0400 UT
|
Jul 22, '00
|
1800 UT
|
Earth
||
0.02
||
23.5
||
Mar 20, '00
|
0735 UT
|
Jun 21, '00
|
0148 UT
|
Sep 23, '00
|
1727 UT
|
Dec 21, '00
|
1337 UT
|
Mars
||
0.09
||
24
||
May 31 '00
||
Dec 16 '00
||
Jun 12 '01
||
Nov 2 '01
|
|
Jupiter
||
0.05
||
3
||
August 1997
||
May 2000
||
March 2003
||
March 2006
|
|
Saturn
||
0.06
||
26.75
||
1980
||
1987
||
1995
||
2002
|
|
Uranus
||
0.05
||
82
||
1922
||
1943
||
1964
||
1985
|
|
Neptune
||
0.01
||
28.5
||
1880
||
1921
||
1962
||
2003
|
(Table note: seasonal names refer to the northern
hemisphere of each planet.)
Planetary seasons are caused by two factors: axial tilt
and variable distance from the sun (orbital eccentricity). Earth's
orbit is nearly circular and so has little effect on climate.
It's our planet's axial tilt that causes almost all seasonal
changes. When the north pole is tilted toward the Sun, it's northern
summer. Six months later the north pole tilts away from the Sun
and we experience northern winter.
The other two planets where it is northern spring, Jupiter and
Venus, have very small axial tilts -- just 3 degrees compared
to Earth's 23.5 degree tilt. Seasonal changes on those planets
are correspondingly small. Spring on Venus isn't much different
from autumn. The planet's dense, acidic atmosphere produces a
runaway greenhouse effect that keeps the surface at 750 K year-round
-- that's hot enough to melt lead. Spring fever on Venus is really
hot!
Our second-nearest
planetary neighbor Mars has the highest orbital eccentricity
of any world except Pluto. Its distance from the Sun varies between
1.64 and 1.36 AU over the Martian year. This large variation,
combined with an axial tilt greater than Earth's gives rise to
seasonal changes far greater than we experience even in Antarctica.
Right: Over the past six months,
the southern hemisphere of Mars has passed through spring and
into summer. Spring started in early August 1999 and summer arrived
toward the end of December 1999. Mars Global Surveyor is in a
polar orbit, thus the spacecraft's camera has had an excellent
view of seasonal changes. Shown here are three views of the same
portion the layered terrain near the Martian south pole. They
show how the landscape thaws and defrosts as summer approaches.
[more
information]
From the point of view of an Earth-dweller, one of the strangest
effects of seasons on Mars is the change in atmospheric pressure.
During winter the global atmospheric pressure on Mars is 25%
lower than during summer. This happens because of the eccentricity
of Mars's orbit and a complex exchange of carbon dioxide between
Mars's dry-ice polar caps and its CO2 atmosphere. Around the
summer solstice when the Martian north pole is tilted away from
the sun, the northern polar cap expands as carbon dioxide in
the polar atmosphere freezes. At the other end of the planet
the southern polar cap melts, giving CO2 back to the
atmosphere. This process reverses half a year later at the winter
solstice.
At first it might seem that these events occurring at opposite
ends of Mars would simply balance out over the course of the
Martian year, having no net effect on climate. But they don't.
That's because Mars is 10% closer to the Sun in winter than it
is in summer. At the time of the winter solstice the northern
polar cap absorbs more CO2 than the southern polar
cap absorbs half a year later. The difference is so great that
Mars's atmosphere is noticeably thinner during winter.
Seasons on Mars vs. Seasons on Earth
|
|
Season
(Northern Hemisphere)
|
|
Length of Season on Earth
(Earth Days)
|
|
Length of Season on Mars
(Martian Days)
|
Spring
||
93
||
194
|
|
Summer
||
93
||
178
|
|
Autumn
||
90
||
142
|
|
Winter
||
89
||
154
|
Above: The orbit of Mars is very
eccentric, unlike Earth's which is more nearly circular. Its
orbital motion is slowest when it is at aphelion (the farthest
point from the Sun) and fastest at perihelion (the closest point
to the Sun). This effect, combined with the planet's axial tilt,
makes Martian seasons vary in duration more than those on Earth.
The length of the seasons in this table are give in Earth days
and Martian days. The two are almost exactly the same duration.
An Earth day is 24 hours long, a Martian day is 24.6 hours long.
[more
information]
Martian seasons are peculiar by Earth standards, but they probably
pale in comparison to seasons on Uranus. Like Earth, the orbit
of Uranus is nearly circular so it keeps the same distance from
the Sun throughout its long year. But, Uranus's spin axis is
tilted by a whopping 82 degrees! This gives rise to extreme 20-year-long
seasons and unusual weather. For nearly a quarter of the Uranian
year (equal to 84 Earth years), the sun shines directly over
each pole, leaving the other half of the planet plunged into
a long, dark, frigid winter.
Left: A dramatic time-lapse movie
by NASA's Hubble Space Telescope shows seasonal changes on Uranus.
Once considered one of the blander-looking planets, Uranus is
now revealed as a dynamic world with the brightest clouds in
the outer Solar System. more
info.
The Northern Hemisphere of Uranus is just now coming out of the
grip of its decades-long winter. As the sunlight reaches some
latitudes for the first time in years, it warms the atmosphere
and triggers gigantic springtime storms comparable in size to
North America with temperatures of 300 degrees below zero. In
the animation pictured left the bright clouds are probably made
of crystals of methane, which condense as warm bubbles of gas
well up from deep in the atmosphere of Uranus.
Uranus does not have a solid surface, but is instead a ball of
mostly hydrogen and helium. Absorption of red light by methane
in the atmosphere gives the planet its cyan color. Uranus was
discovered March 13, 1781, by William Herschel. Early visual
observers reported Jupiter-like cloud belts on the planet, but
when NASA's Voyager 2 flew by in 1986, Uranus appeared as featureless
as a cue ball. In the past 13 years, the planet has moved far
enough along its orbit for the sun to shine at mid-latitudes
in the Northern Hemisphere. By the year 2007, the sun will be
shining directly over Uranus' equator.
|
Parents and Educators: Please visit
Thursday's Classroom
for lesson plans and activities related to this story.
|
Mercury's seasons -- if they can be called that -- are also remarkable.
Until the 1960's it was thought that Mercury's "day"
was the same length as its "year" keeping the same
face to the Sun much as the Moon does to the Earth. This was
shown to be incorrect by Doppler radar observations. We now known
that Mercury rotates three times during two of its years. Mercury
is the only body in the solar system tidally locked into an orbital-to-rotational
resonance with a ratio other than 1:1.
This fact and the high eccentricity of Mercury's orbit would
produce very strange effects for an observer on Mercury's surface.
[ref]
At some longitudes the observer would see the Sun rise and then
gradually increase in apparent size as it slowly moved toward
the zenith. At that point the Sun would stop, briefly reverse
course, and stop again before resuming its path toward the horizon
and decreasing in apparent size. All the while the stars would
be moving three times faster across the sky. Observers at other
points on Mercury's surface would see different but equally bizarre
motions.
Temperature variations on Mercury are the most extreme in the
solar system ranging from 90 K at night to 700 K during the day.

Question: which two planets do jupiter not experience seasonal changes

Jupiter's inclination is relatively small: only 3.13°.

As a result, it does not experience significant seasonal changes, unlike, for example, Earth and Mars.

which two planets do jupiter not experience seasonal changes

Question: how far is jupiter inclination from earth

how far is jupiter inclination from earth

Question: which other planet besides jupiter does not experience significant seasonal changes

which other planet besides jupiter does not experience significant seasonal changes

Question: which planet has an inclination of only 3.13 degrees

which planet has an inclination of only 3.13 degrees

Question: is jupiter's inclination small or large

Question: jupiter does not experience what kind of changes

jupiter does not experience what kind of changes

Question: what is the inclination of jupiter to earth

what is the inclination of jupiter to earth

Jupiter 's inclination is relatively small : only 3.13 ° .

As a result , it does not experience significant seasonal changes , unlike , for example , Earth and Mars .

Jupiterov nagib je relativno mali: samo 3,13°. Kao rezultat toga, ona ne doživljava značajne sezonske promjene, za razliku od, primjerice, Zemlje i Marsa.

Jupiterov nagib je relativno mali: samo 3,13°.

Kao rezultat toga, ona ne doživljava značajne sezonske promjene, za razliku od, primjerice, Zemlje i Marsa.

Jupiter's inclination is relatively small: only 3.13°. As a result, it does not experience significant seasonal changes, unlike, for example, Earth and Mars.

Jupiter's inclination is relatively small: only 3.13°.

As a result, it does not experience significant seasonal changes, unlike, for example, Earth and Mars.

Jupiter's rotation is the fastest of all the planets in the Solar System, completing the rotation on its axis in a little less than ten hours; this creates an equatorial infusion that is easily seen through an amateur telescope from Earth.

Question: how long does it take jupiter to complete its rotation

how long does it take jupiter to complete its rotation

Question: what is the fastest in our solar system

Question: which planet completes its rotation on its axis in a little less than ten hours

which planet completes its rotation on its axis in a little less than ten hours

Question: how can you see jupiter from earth

Question: which planet completes the rotation on its axis in a little less than ten hours

which planet completes the rotation on its axis in a little less than ten hours

Jupiter 's rotation is the fastest of all the planets in the Solar System , completing the rotation on its axis in a little less than ten hours ; this creates an equatorial infusion that is easily seen through an amateur telescope from Earth .

Interaction with the Sun's system "Trojans" and "Greeks" in Jupiter's orbit.

Together with the Sun, Jupiter's great gravitational influence helped form the Sun's system.

Question: which planet is the only one that is closer to the sun's equatorial plane than

Interaction with the Sun's system "Trojans" and "Greeks" in Jupiter's orbit.

Together with the Sun, Jupiter's great gravitational influence helped form the Sun's system.

which planet is the only one that is closer to the sun's equatorial plane than

Question: which planet is responsible for kirkwood's zone in the asteroid belt

which planet is responsible for kirkwood's zone in the asteroid belt

Question: what helped form the sun's system

Jupiter 's great gravitational influence

Question: what is the name of the group of greeks in jupiter's orbit

what is the name of the group of greeks in jupiter's orbit

Question: what influence helped form the sun's system

what influence helped form the sun's system

Question: what are the names of the planets in jupiter's orbit

what are the names of the planets in jupiter's orbit

Question: what kind of influence did jupiter have on the sun's system

what kind of influence did jupiter have on the sun's system

Interaction with the Sun 's system " Trojans " and " Greeks " in Jupiter 's orbit .

Together with the Sun , Jupiter 's great gravitational influence helped form the Sun 's system .

The orbits of most planets of the system are closer to Jupiter 's orbital plane than the Sun 's equatorial plane ( Mercury is the only planet that is closer to the Sun 's equator in the orbital angle ) , Kirkwood 's zone in the asteroid belt is mainly caused by Jupiter , and may have been responsible for the late hard bombing of the internal Sun 's system in the past .

Interakcija sa Sunčevim sustavom "Trojanci" i "Grci" u Jupiterovoj orbiti. Zajedno sa Suncem, Jupierov veliki gravitacijski utjecaj pomogao je oblikovanju Sunčevog sustava. Orbite većine planeta sustava leže bliže Jupiterovoj orbitalnoj ravnini od Sunčeve ekvatorijalne ravnine (Merkur je jedini planet koji je bliži Sunčevom ekvatoru u orbitalnom nagibu), Kirkwoodove zone u asteroidnom pojasu uglavnom uzrokuje Jupiter, te je možda bio odgovoran za kasno teško bombardiranje unutarnjeg Sunčevog sustava u prošlosti.

Interakcija sa Sunčevim sustavom "Trojanci" i "Grci" u Jupiterovoj orbiti.

Zajedno sa Suncem, Jupierov veliki gravitacijski utjecaj pomogao je oblikovanju Sunčevog sustava.

Interaction with the Sun's system "Trojans" and "Greeks" in Jupiter's orbit. Together with the Sun, Jupiter's great gravitational influence helped form the Sun's system. The orbits of most planets of the system are closer to Jupiter's orbital plane than the Sun's equatorial plane (Mercury is the only planet that is closer to the Sun's equator in the orbital angle), Kirkwood's zone in the asteroid belt is mainly caused by Jupiter, and may have been responsible for the late hard bombing of the internal Sun's system in the past.

Interaction with the Sun's system "Trojans" and "Greeks" in Jupiter's orbit.

Together with the Sun, Jupiter's great gravitational influence helped form the Sun's system.

Together with its moons, Jupiter's gravitational field controls numerous asteroids that have settled in the Lagrangie point region in Jupiter's orbit around the Sun.

Question: where are asteroids located in jupiter's orbit around the sun

Together with its moons, Jupiter's gravitational field controls numerous asteroids that have settled in the Lagrangie point region in Jupiter's orbit around the Sun.

where are asteroids located in jupiter's orbit around the sun

Question: in which region of jupiter's orbit around the sun do asteroids settle

in which region of jupiter's orbit around the sun do asteroids settle

Question: what does jupiter's gravitational field control

what does jupiter's gravitational field control

Question: what is the name of the planet in our solar system

what is the name of the planet in our solar system

Question: where are jupiter's moons located

Question: what controls asteroids that settle in the lagrangie point region of jupiter's orbit

polje kontrolira brojne asteroide koji su se naselili u regije Lagrangieove točke u Jupiterovoj orbiti oko Sunca

what controls asteroids that settle in the lagrangie point region of jupiter's orbit

Question: what controls asteroids in jupiter's orbit around the sun

Jupiterovo gravitacijsko polje kontrolira brojne asteroide koji su se naselili u regije Lagrangieove točke u Jupiterovoj orbiti oko Sunca

what controls asteroids in jupiter's orbit around the sun

Together with its moons , Jupiter 's gravitational field controls numerous asteroids that have settled in the Lagrangie point region in Jupiter 's orbit around the Sun .

Zajedno sa svojim mjesecima, Jupiterovo gravitacijsko polje kontrolira brojne asteroide koji su se naselili u regije Lagrangieove točke u Jupiterovoj orbiti oko Sunca.

Zajedno sa svojim mjesecima, Jupiterovo gravitacijsko polje kontrolira brojne asteroide koji su se naselili u regije Lagrangieove točke u Jupiterovoj orbiti oko Sunca.

Together with its moons, Jupiter's gravitational field controls numerous asteroids that have settled in the Lagrangie point region in Jupiter's orbit around the Sun.

Together with its moons, Jupiter's gravitational field controls numerous asteroids that have settled in the Lagrangie point region in Jupiter's orbit around the Sun.

Due to the size of Jupiter's mass, the weight between it and the Sun lies directly above the Sun's surface.

Jupiter, the fifth planet from the sun, gas giant, and subject of the Juno mission, is huge. Huge.
It's so huge, in fact, that it doesn't actually orbit the sun. Not exactly. With 2.5 times the mass of all the other planets in the solar system combined, it's big enough that the center of gravity between Jupiter and the sun doesn't actually reside inside the sun — rather, at a point in space just above the sun's surface.
Here's how that works.
When a small object orbits a big object in space, the less massive one doesn't really travel in a perfect circle around the larger one. Rather, both objects orbit a combined center of gravity.
In situations we're familiar with — like Earth orbiting the much-larger sun — the center of gravity resides so close to the center of the larger object that the impact of this phenomenon is negligible. The bigger object doesn't seem to move, and the smaller one draws a circle around it.
But reality is always more complicated.
For example: When the International Space Station (ISS) orbits the Earth, both the Earth and the space station orbit their combined center of gravity. But that center of gravity is so absurdly close to the center of the Earth that the planet's motion around the point is impossible to spot — and the ISS describes a near-perfect circle around the whole planet.
The same truth holds when most planets orbit the sun. Sol is just so much larger than Earth, Venus, Mercury, or even Saturn that their centers of mass with the sun all lie deep within the star itself.
Not so with Jupiter.
The gas giant is so big that its center of mass with the sun, or barycenter, actually lies 1.07 solar radii from the middle of the sun — or 7% of a sun-radius above the sun's surface. Both the Sun and Jupiter orbit around that point in space.
This not-to-scale gif from NASA illustrates the effect:
That is, in essence, how Jupiter and the sun move through space together — though the distances and sizes are far different. Jupiter is still only a fraction of the sun's size.
But next time someone asks you for a crazy space fact you'll know: Jupiter is so massive, it doesn't orbit the sun.

Question: where is the weight between jupiter and the sun located

Due to the size of Jupiter's mass, the weight between it and the Sun lies directly above the Sun's surface.

where is the weight between jupiter and the sun located

Question: why is jupiter so close to the sun

Question: where is jupiter located on the solar system

where is jupiter located on the solar system

Question: which planet lies directly between the sun and the moon

which planet lies directly between the sun and the moon

Question: where is jupiter located on the sun

Question: what is the difference between jupiter and the sun

what is the difference between jupiter and the sun

Due to the size of Jupiter 's mass , the weight between it and the Sun lies directly above the Sun 's surface .

Zbog veličine Jupiterove mase, težište između njega i Sunca leži neposredno iznad Sunčeve površine.

Zbog veličine Jupiterove mase, težište između njega i Sunca leži neposredno iznad Sunčeve površine.

Due to the size of Jupiter's mass, the weight between it and the Sun lies directly above the Sun's surface.

Due to the size of Jupiter's mass, the weight between it and the Sun lies directly above the Sun's surface.

Infrared screenshots of the Shoemaker-Levy 9 (left) comet hit Jupiter (center).

The lighting point on the right side is Io.

Question: what is the brightest comet on jupiter's right side

Infrared screenshots of the Shoemaker-Levy 9 (left) comet hit Jupiter (center).

The lighting point on the right side is Io.

what is the brightest comet on jupiter's right side

Question: io is the brightest comet on which planet

io is the brightest comet on which planet

Question: what kind of light is jupiter in

Question: what is the name of the comet that hit jupiter

what is the name of the comet that hit jupiter

Question: which side of jupiter is io on

Question: what is io

Question: where is io in relation to jupiter

Question: what is on the right side of jupiter

Infracrvena snimka udara kometa Shoemaker - Levy 9 ( lijevo ) u Jupiter ( sredina

Infrared screenshots of the Shoemaker - Levy 9 ( left ) comet hit Jupiter ( center ) .

The lighting point on the right side is Io .

Udari Infracrvena snimka udara kometa Shoemaker-Levy 9 (lijevo) u Jupiter (sredina). Svijetla točka na desnoj strani je Io.

Udari Infracrvena snimka udara kometa Shoemaker-Levy 9 (lijevo) u Jupiter (sredina).

Infrared screenshots of the Shoemaker-Levy 9 (left) comet hit Jupiter (center). The lighting point on the right side is Io.

Infrared screenshots of the Shoemaker-Levy 9 (left) comet hit Jupiter (center).

The lighting point on the right side is Io.

Question: what is the name of the cloud that jupiter protects the earth from

what is the name of the cloud that jupiter protects the earth from

Question: where do some scientists think jupiter pulls comets toward earth

where do some scientists think jupiter pulls comets toward earth

Question: what perturbates the orbits of jupiter's comets

what perturbates the orbits of jupiter's comets

Question: which planet in our solar system does not cause a net decrease in the number of com

which planet in our solar system does not cause a net decrease in the number of com

Question: what perturbates the orbits of jupiter

Question: what is jupiter responsible for passing through our solar system

what is jupiter responsible for passing through our solar system

Question: what cloud does jupiter protect the earth from

what cloud does jupiter protect the earth from

However , recent computing simulations suggest that Jupiter does not cause a net decrease in the number of comets passing through the inner solar system , as its gravity pertubates their orbits within approximately as often as it accumulates or expands them .

This topic remains controversial among scientists , because some think it pulls comets toward Earth from the Kuiper belt , while others think Jupiter protects the Earth from the alleged Oort cloud .

Ova tema ostaje sporna među znanstvenicima, jer neki misle da on vuče komete prema Zemlji iz Kuiperovog pojasa, dok drugi misle da Jupiter štiti Zemlju od navodnog Oortovog oblaka.

However, recent computing simulations suggest that Jupiter does not cause a net decrease in the number of comets passing through the inner solar system, as its gravity pertubates their orbits within approximately as often as it accumulates or expands them. This topic remains controversial among scientists, because some think it pulls comets toward Earth from the Kuiper belt, while others think Jupiter protects the Earth from the alleged Oort cloud.

The fireball was photographed by Voyager 1 during the meeting with Jupiter in March 1979.

An amateur astronomer reported the visual detection of a fireball on Jupiter at 11:35 UT (September 10 2012) last night. It was confirmed on a video recorded from Texas. This is the 6th impact of Jupiter detected so far.
Astronomer Dan Petersen saw today September 10 2012 at 11:35 UT a bright flash on Jupiter which lasted 1 or 2 seconds. It estimated its position to be in the system I Longitude = 335 and Latitude = +12 deg. The report was sent to Richard Schmude of the Association of Lunar and Planetary Observers (ALPO) and forwarded to us by John H. Rogers, Jupiter Section Director at the British Astronomical Association.
A video of the flash was revealed a few hours later by George Hall, an amateur astronomer located in Dallas Texas. He used a webcam mounted on a MEADE 12″ LX200GPS. An image extracted from the video is attached above and it looks quite similar to the flash observed on August 20 2010.
This is the 6th impact observed on Jupiter. The most famous one was the predicted, and intensively observed, impact of the comet Shoemaeker-Levy 9 (S-L 9) which broke apart and collide on Jupiter in July 1994. An fireball was photographed by Voyager 1 during its encounter on March 1979 with Jupiter. More recently, thanks to the intensive monitoring of amateur astronomer and the improvement in image quality providing by cheap webcam plugged on small telescopes, several small impacts were detected and followed up by amateur and professional astronomers together:
Because the impactors were small (a few meters) the 2010 impacts were not big explosions driving a giant plume, as we have seen for S-L 9 and the 2009 impact. The absence of scar, or “black spots” on Jupiter, observed for the 2010 events implies that there was no debris field, so they were most likely just meteors. To characterize the type of impact that was observed a few hours ago, the area of the impact will be monitored using large facilities. If a scar is detected in the visible light, it will be definitely an interesting event which will be followed up by amateurs and professional astronomers.
These impacts or meteors are not only a distraction for planetary astronomers. They give us an opportunity to better understand the internal structure of Jupiter since the energetic ones reveal the lower deck of clouds and provide clues on its composition. Additionally, the complex pattern of jet stream winds at various latitudes can be also directly measured by monitoring the evolution of a scar over a long period of time like it was done for the 2009 impact.
It is also a way to assess the rate of large meteoroid impacts on the planets and understand the role of Jupiter in shielding the inner part of the solar system. This idea remains controversial (see Jupiter: Friend or Foe?) and a direct measurements of the flux of meteors and impact rate may help to provide a better answer to this question.
Finally, even if this flash ends up being “just a meteor”, it is remarkable that amateur astronomers are today capable of monitoring almost permanently the planet Jupiter. These organized network teams are a great asset for professional astronomers since they can detect these events and quickly warn others.
Clear skies,
Franck Marchis
[Edited at 11:04pm to include the Voyager impact. Thanks to Kunio Sayanagi for his comments]
[Edited at 1:04 pn on Sep 11 – link to the video was added]
11 Comments
[…] – Vu en premier chez Alan Boyle et Franck Marchis […]
Here’s Jupiter imaged a few minutes ago from Slooh’s Canary Islands Observatory: http://goo.gl/wurvr
Thanks a lot Paul
Very O Futuristic..perhaps, the planet is evolving or recreating to be inhabited. Why now? There has been no activity before the 70’s? Timing is important. Something definitely cause the flare. No freak accident.
[…] um 11:35:30 UTC ist es wieder passiert: Amateurastronomen – diesmal Zeitzonen-bedingt in den USA – beobachteten und filmten […]
G’Day! Franck,
Neat Post, when they say the fireball “slammed” into jupiter, is there really anything in that bigass sphere to slam into? do we know what’s inside jupiter? is there really any solid surface anywhere in it at all? what’s a more likely scenario for what happened to the fireball when it entered jupiter’s atmosphere? just curious. thanks
Good Job!
[…] Franck Marchis has more at his blog with a pretty good analysis. Worth checking out! Posted in Jupiter, Solar System Tagged impact, Jupiter […]
[…] är inte första gången som vi sett sådant här drabba Jupiter. Planetforskaren Franck Marchis skriver om händelsen på sin blogg och om de andra gånger som vi sett saker störta mot Jupiter.Kometen Shoemaker-Levy 9 bröt upp […]
From the looks of the video, Monday night would not have been a very jovial night to spend on Jupiter. Two amateur astronomers saw a bright white flash for a few seconds just inside Jupiter’s eastern limb, which was probably a fireball a hundred miles in diameter caused by an asteroid or comet impacting Jupiter’s atmosphere.
[…] Marchis (2012-09-10). “Another fireball on Jupiter?”. Cosmic Diary blog. Retrieved […]

Question: when was jupiter photographed by voyager 1

The fireball was photographed by Voyager 1 during the meeting with Jupiter in March 1979.

when was jupiter photographed by voyager 1

Question: who photographed the fireball that was jupiter in 1979

who photographed the fireball that was jupiter in 1979

Question: which planet was photographed by voyager 1 in 1979

which planet was photographed by voyager 1 in 1979

Question: what was photographed by voyager 1 in 1979

what was photographed by voyager 1 in 1979

Question: in what year was jupiter photographed by voyager 1

in what year was jupiter photographed by voyager 1

Question: what was photographed by voyager 1 during the meeting with jupiter in 1979

what was photographed by voyager 1 during the meeting with jupiter in 1979

Question: when was the fireball photographed by voyager 1

when was the fireball photographed by voyager 1

The fireball was photographed by Voyager 1 during the meeting with Jupiter in March 1979 .

Vatrenu kuglu fotografirao je Voyager 1 tijekom susreta s Jupiterom u ožujku 1979.

Vatrenu kuglu fotografirao je Voyager 1 tijekom susreta s Jupiterom u ožujku 1979.

The fireball was photographed by Voyager 1 during the meeting with Jupiter in March 1979.

The fireball was photographed by Voyager 1 during the meeting with Jupiter in March 1979.

Comet Shoemaker-Levy Collision with Jupiter
Twenty years ago, Comet Shoemaker-Levy 9 (SL9) impacted Jupiter. I created this website in June 1994 on a voluntary basis, and it was my first public website. I was immensely interested in this unique comet since its discovery in 1993 - a comet that was not only captured into Jupiter orbit, but had broken up into several pieces which were about to hit Jupiter in July 1994. There were a lot of speculation about how the impacts would appear on Jupiter, and this website documents each impact as they occurred. Also note: back in 1994, websites were relatively unknown and somewhat of a novelty. This website became the first big Web event, and was key in raising the awareness of websites to the mainstream public, which we now take for granted today.
Here's a good summary of the Comet Shoemaker-Levy 9 events published the "JPL Universe" on January 13, 1995.
JPL Universe article
This website will remain up as an archive and I hope you enjoy the images.
Ron Baalke
From July 16 through July 22, 1994, pieces of an object designated as Comet P/Shoemaker-Levy 9 collided with Jupiter. This is the first collision of two solar system bodies ever to be observed, and the effects of the comet impacts on Jupiter's atmosphere have been simply spectacular and beyond expectations. Comet Shoemaker-Levy 9 consisted of at least 21 discernable fragments with diameters estimated at up to 2 kilometers.
Access Count to this Home Page: 7,618,325 . Click here for more details.
The Comet Shoemaker-Levy Home Page (JPL) has been rated in the top 5 percent of all World Wide Web sites in an external review by Point Communications.

Question: what comet collided with the southern peninsula of jupiter in 1994

what comet collided with the southern peninsula of jupiter in 1994

Question: when was jupiter's fireball photographed by voyager 1

when was jupiter's fireball photographed by voyager 1

Question: who photographed the fireball that jupiter experienced in 1979

who photographed the fireball that jupiter experienced in 1979

Question: how many fragments of shoemaker-levy 9 collided with the southern peninsula of j

how many fragments of shoemaker-levy 9 collided with the southern peninsula of j

Question: the comet shoemaker-levy 9 collided with which planet in 1994

the comet shoemaker-levy 9 collided with which planet in 1994

Question: where did the comet shoemaker-levy 9 collide with

Jupiterovom južnom polutkom , pružajući prvo izravno promatranje sudara između dva objekta Sunčevog

where did the comet shoemaker-levy 9 collide with

During the period from 16 July 1994 to 22 July 1994 , more than 20 fragments of the comet Shoemaker - Levy 9 collided with the Southern Peninsula of Jupiter , providing the first direct observation of the collision between the two objects of the Solar System .

The fireball was photographed by Voyager 1 during the meeting with Jupiter in March 1979. During the period from 16 July 1994 to 22 July 1994, more than 20 fragments of the comet Shoemaker-Levy 9 collided with the Southern Peninsula of Jupiter, providing the first direct observation of the collision between the two objects of the Solar System.

Because of this collision, a lot is known about the composition of Jupiter's atmosphere.

On 19 July 2009, a place of collision at a length of approximately 216 degrees was detected in the system II.

This impact left behind it a black spot in Jupiter's atmosphere, similar to the size of the Oval BA.

Amateur astronomer discovers Jupiter collision
An amateur astronomer from the small village of Murrumbateman, north of Canberra, has made a rare discovery that has NASA scientists excited.
Computer programmer Anthony Wesley captured images showing a massive comet or asteroid had collided with the planet Jupiter.
Mr Wesley made the discovery in the early hours of yesterday morning using a telescope in his backyard.
He says he immediately realised its significance.
"By two o'clock I'd come back up to the house and was sending alerts to all the people I could think of that should be looking at this and especially the professional astronomers with specialised instrument for measuring this," he said.
"The sooner they could see this the more interesting and more useful science they can get from it."
His discovery has been confirmed by NASA and has caught the attention of astronomers around the world.
Mr Wesley says it is only the second time such a discovery has been made.
"There was pretty much widespread excitement as soon as everybody realised that another one of these impact has happened," he said.
"It's a dream really for anyone who takes photographs of the planets and photographs of Jupiter to take a photograph of this type, really it's a dream come true for me."

Question: what is the length of jupiter's atmosphere

Because of this collision, a lot is known about the composition of Jupiter's atmosphere.

On 19 July 2009, a place of collision at a length of approximately 216 degrees was detected in the system II.

This impact left behind it a black spot in Jupiter's atmosphere, similar to the size of the Oval BA.

what is the length of jupiter's atmosphere

Question: in which system of jupiter's atmosphere was a collision on 19 july 2009

in which system of jupiter's atmosphere was a collision on 19 july 2009

Question: when was the last time jupiter had a collision

when was the last time jupiter had a collision

Question: how many degrees is jupiter's atmosphere

how many degrees is jupiter's atmosphere

Question: what is the name of the oval in jupiter's atmosphere

what is the name of the oval in jupiter's atmosphere

Question: what did the impact of jupiter's collision in july 2009 produce

what did the impact of jupiter's collision in july 2009 produce

Question: what was left behind by the impact of jupiter's collision in july 2009

what was left behind by the impact of jupiter's collision in july 2009

Because of this collision , a lot is known about the composition of Jupiter 's atmosphere .

On 19 July 2009 , a place of collision at a length of approximately 216 degrees was detected in the system II .

This impact left behind it a black spot in Jupiter 's atmosphere , similar to the size of the Oval BA .

Zbog tog sudara mnogo je saznato o sastavu Jupiterove atmosfere.

19. srpnja 2009. u sustavu II otkriveno je mjesto udara na dužini od približno 216 stupnjeva.

Ovaj utjecaj ostavio je iza sebe crnu mrlju u Jupiterovoj atmosferi, sličnu veličinu kao Oval BA.

Because of this collision, a lot is known about the composition of Jupiter's atmosphere. On 19 July 2009, a place of collision at a length of approximately 216 degrees was detected in the system II. This impact left behind it a black spot in Jupiter's atmosphere, similar to the size of the Oval BA.

Because of this collision, a lot is known about the composition of Jupiter's atmosphere.

On 19 July 2009, a place of collision at a length of approximately 216 degrees was detected in the system II.

This impact left behind it a black spot in Jupiter's atmosphere, similar to the size of the Oval BA.

Jupiter sports new 'bruise' from impact
Something has smashed into Jupiter, leaving behind a black spot in the planet’s atmosphere, scientists confirmed on Monday.
This is only the second time such an impact has been observed. The first was almost exactly 15 years ago, when more than 20 fragments of comet Shoemaker-Levy 9 collided with the gas giant.
“This has all the hallmarks of an impact event, very similar to Shoemaker-Levy 9,” said Leigh Fletcher, an astronomer at NASA’s Jet Propulsion Lab in Pasadena, California. “We’re all extremely excited.”
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The impact was discovered by amateur astronomer Anthony Wesley in Murrumbateman, Australia at about 1330 GMT on Sunday. Wesley noticed a black spot in Jupiter’s south polar region (see image) – but he very nearly stopped observing before he saw it.
“By 1am I was ready to quit … then changed my mind and decided to carry on for another half hour or so,” he wrote in his observation report. Initially he suspected he was seeing one of Jupiter’s moons or a moon’s shadow on the planet, but the location, size and speed of the spot ruled out that possibility.
‘Stroke of luck’
After checking images taken two nights earlier and not seeing the spot, he realised he had found something new and began emailing others.
Among the people he contacted were Fletcher and Glenn Orton, also at JPL. They had serendipitously scheduled observing time on NASA’s InfraRed Telescope Facility in Hawaii for that night.
“It was a fantastic stroke of luck,” Orton told New Scientist.
Their team began observations at about 1000 GMT on 20 July, and after six hours of observing confirmed that the spot was an impact and not a weather event.
“It’s completely unlike any of the weather phenomena that we observe on Jupiter,” Orton says.
Splash
The first clue was a near-infrared image of the upper atmosphere above the impact site. An impact would make a splash like a stone thrown into a pool, scattering material in the atmosphere upwards. This material would then reflect sunlight, appearing as a bright spot at near-infrared wavelengths.
And that’s exactly what the team saw. “Our first image showed a really bright object right where that black scar was, and immediately we knew this was an impact,” Orton says. “There’s no natural phenomenon that creates a black spot and bright particles like that.”
Supporting evidence came from measurements of Jupiter’s temperature. Thermal images also showed a bright spot where the impact took place, meaning the impact warmed up the lower atmosphere in that area.
The researchers have also found hints of higher-than-normal amounts of ammonia in the upper atmosphere. Extra ammonia had been churned up by the previous Shoemaker-Levy comet impact.
Exotic chemistry
The Shoemaker-Levy impact also introduced some exotic chemistry into Jupiter’s atmosphere. The energy from the collision fused some of the original atmospheric components into new molecules, such as hydrogen cyanide.
Scientists hope this new impact has done the same thing, since that would allow them to follow the new materials and learn how the atmosphere moves with time.
So what was the impactor? “Not a clue,” Orton says. He speculates that it could have been a block of ice from somewhere in Jupiter’s neighborhood, or a wandering comet that was too faint for astronomers to detect before the impact.
“We don’t know if the impact was produced by a comet or an asteroid,” agrees Franck Marchis, an astronomer at the University of California, Berkeley, and the SETI Institute, who was part of a team that observed the spot on Sunday with the Keck Observatory in Hawaii (see image). If the object was large enough to be visible before impact, current surveys of asteroids may not have been looking in the right direction to find it, he says, adding that future surveys will spot more of the solar system’s uncatalogued objects.
Asteroid or comet
Spectra collected by various observatories may help identify what the impactor was, since a large amount of water at the impact location would hint at a comet as the source. “We will also compare the observations with those collected during [Shoemaker-Levy 9] 15 years ago,” since that was a known comet, Marchis says.
Without having seen it, scientists can’t tell how large the object was. “But the impact scar we’re seeing is about the same size as one of Jupiter’s big storms, Oval BA, Fletcher told New Scientist. “That, I believe, is about the size of the Earth.”
Marchis says Jupiter may be protecting Earth from getting hit by such objects. “The solar system would have been a very dangerous place if we did not have Jupiter,” he told New Scientist. “We should thank our Giant Planet for suffering for us. Its strong gravitational field is acting like a shield protecting us from comets coming from the outer part of the solar system.”
More on these topics:

June 4, 2010
Planetary imager and longtime Astronomy
magazine contributor Christopher Go from Cebu, Philippines, and amateur astronomer Anthony Wesley from Murrumbateman, Australia, have captured yet another impact on Jupiter. The fireball appeared in the giant planet's atmosphere June 3 at 20h30m Universal Time (4:30 P.M. EDT).
In an e-mail to Astronomy
that includes impact images and even a video, Go writes, "Today was supposed to be a routine imaging run. Seeing [a measure of atmospheric steadiness] was perfect. The boring side of Jupiter [the one away from the Great Red Spot] was facing Earth. On my second image sequence using a blue filter, I luckily imaged an impact. I did not see this when it happened, but Anthony Wesley saw this in Australia. Anthony sent an alert on this suspected impact and I was able to confirm this with my video."
This impact occurred within Jupiter's recently faded South Equatorial Belt
. Go said that this is good timing because it will make it easier to find a dark remnant from the blast, if one appears. He finished his e-mail by saying, "I would like congratulate my friend Anthony Wesley for having such a sharp eye on this historic find!"
Jupiter has been the target of several impactors within the last two decades. In July 1994, 21 fragments of Comet Shoemaker-Levy 9 hit the planet. More recently, a 0.3-mile-wide (0.5 kilometer) asteroid struck Jupiter July 18, 2009
. Wesley also was the first to spot that impact, which galvanized the astronomical community into studying the collision site.

Question: what was the length of the collision between jupiter and shoemaker-levy 9

what was the length of the collision between jupiter and shoemaker-levy 9

Question: when did the comet shoemaker-levy 9 collide with jupiter

when did the comet shoemaker-levy 9 collide with jupiter

Question: where did shoemaker-levy 9 collide with in 1994

Jupiterovom južnom polutkom , pružajući prvo izravno promatranje sudara između dva objekta Sunčevog

where did shoemaker-levy 9 collide with in 1994

During the period from 16 July 1994 to 22 July 1994, more than 20 fragments of the comet Shoemaker-Levy 9 collided with the Southern Peninsula of Jupiter, providing the first direct observation of the collision between the two objects of the Solar System. Because of this collision, a lot is known about the composition of Jupiter's atmosphere. On 19 July 2009, a place of collision at a length of approximately 216 degrees was detected in the system II.

U Jupiter udario ogromni meteor, pogledajte snimku
S OBZIROM na to da Jupiter ovih noći krasi nebo nad sjevernom polutkom, mnogi astronomi amateri usmjerili su svoje teleskope prema njemu kako bi uhvatili Jupiterove karakteristične pruge ili čak snimili Veliku crvenu pjegu.
No, jedan astrofotograf je ovih dana snimio prizor koji mnogi neće uspjeti uhvatiti cijeli svoj život – eksploziju u gornjim slojevima atmosfere tog divovskog planeta, piše Science Alert.
U srijedu, 7. kolovoza, Ethan Chappel iz Teksasa snimio je udar meteora u daleki Jupiter.
"Snimao sam noćas Jupiter. Ovo jako podsjeća na bljesak prilikom udara“, napisao je Chappel na Twitteru.
Meteor izuzetnog sjaja
Udari bolida, odnosno meteora vrlo visokog sjaja, nisu tako rijedak događaj na Jupiteru. Prilično su česti i na Zemlji, samo je naš planet manje privlačna meta, u gravitacijskom smislu, od ovog plinovitog diva pa se takvi događaji ipak zbivaju nešto rjeđe.
Prema studiji iz 1998. godine, vjerojatnost da će neki objekt udariti u Jupiter je između 2.000 i 8.000 puta veća od mogućnosti udara u Zemlju.
No, to ne znači da se tako nešto može lako uočiti, a stvarno je mala vjerojatnost da će kamere zabilježiti točan trenutak udara, odnosno eksplozije.
"Radi se o brzom događaju, sve traje nekoliko sekundi“, rekao je astronom Jonti Horner sa Sveučilišta South Queensland u Australiji.
"Možda to ne biste ni primijetili da gledate kroz teleskop. Puno puta takvi događaji prođu neopaženo, a polovica njih dogodi se na drugoj strani planeta“, dodao je.
Možda je ostao ožiljak
"Usmjerio sam teleskop prema nebu i gledao Perzeide kada se to dogodilo, tako da vizualno nisam ni primijetio bljesak", rekao je astronom amater Chappel.
"Eksploziju sam uočio tek nakon obrade snimke u softveru DeTeCt koji je posebno dizajniran za pronalaženje takvih bljeskova", objasnio je.
Postoji mogućnost da je ovaj udar ostavio svojevrsni ožiljak na Jupiteru koji će se kasnije moći analizirati drugim instrumentima, primjerice pomoću svemirske letjelice Juno.
Prema prvim izvješćima, radi se o premalom objektu za stvaranje dugotrajnijeg ožiljka, ali nikad se ne zna. Očito je meteor bio dovoljno velik da se ovakav događaj snimi sa Zemlje.
Za one koji žele promatrati Jupiter
Ako nakon čitanja ovog članka netko poželi iskušati sreću sa snimanjem Jupitera, Chappel je na Twitteru dao popis opreme koju je koristio prilikom snimanja, što može biti podosta korisno.
U slučaju da to poželite učiniti već ovih dana, možda će vam dobro doći informacija da nad Hrvatskom Jupiter danas izlazi iznad horizonta oko 16 sati, a zalazi oko 00:50. Možete promatrati i Saturn i njegove prstenove; on danas izlazi oko 18:20, a zalazi oko 3 sata ujutro. Mjesec će biti vidljiv od 15:30 pa sve do 1 u noći.

observation of Jupiter through an amateur telescope.

Jupiter is usually the fourth brightest object on the sky (after the Sun, the Moon and Venus); sometimes Mars is brighter than Jupiter.

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Jupiter is the largest planet in the solar system. Its diameter is 88,846 miles
(142,984 kilometers), more than 11 times that of Earth, and about one-tenth that
of the sun. It would take more than 1,000 Earths to fill up the volume of the
giant planet. When viewed from Earth, Jupiter appears brighter than most stars.
It is usually the second brightest planet -- after Venus.
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The layers of dense clouds around Jupiter
appear in a photograph of the planet taken by the Voyager 1 space probe.
The large, oval-shaped mark on the clouds is the Great Red Spot. The spot
is believed to be an intense atmospheric disturbance. Image credit: Jet Propulsion
Laboratory
Jupiter is the fifth planet from the sun. Its mean (average) distance from the
sun is about 483,780,000 miles (778,570,000 kilometers), more than five times
Earth's distance. Ancient astronomers named Jupiter after the king of the Roman
gods.
Astronomers have studied Jupiter with telescopes based on Earth and aboard
artificial satellites in orbit around Earth. In addition, the United States has
sent six space probes (crewless exploratory craft) to Jupiter.
Astronomers witnessed a spectacular event in July 1994, when 21 fragments of a
comet named Shoemaker-Levy 9 crashed into Jupiter's atmosphere. The impacts
caused tremendous explosions, some scattering debris over areas larger than the
diameter of Earth.
Physical features of Jupiter
Jupiter is a giant ball of gas and liquid with little, if any, solid surface.
Instead, the planet's surface is composed of dense red, brown, yellow, and white
clouds. The clouds are arranged in light-colored areas called zones and darker
regions called belts that circle the planet parallel to the equator.
Orbit and rotation
Jupiter travels around the sun in a slightly elliptical
(oval-shaped) orbit. The planet completes one orbit in 4,333 Earth days, or
almost 12 Earth years.
As Jupiter orbits the sun, the planet rotates on its axis, an imaginary line
through its center. The axis is tilted about 3¡. Scientists measure tilt relative
to a line at a right angle to the orbital plane, an imaginary surface touching
all points of the orbit.
Jupiter rotates faster than any other planet. It takes 9 hours 56 minutes to spin
around once on its axis, compared with 24 hours for Earth. Scientists cannot
measure the rotation of the interior of the giant planet directly, so they have
calculated the speed from indirect measurements. They first calculated the speed
using an average of the speeds of the visible clouds that move with interior
currents, except for a more rapid zone near the equator.
Jupiter sends out radio waves strong enough to be picked up by radio telescopes
on Earth. Scientists now measure these waves to calculate Jupiter's rotational
speed. The strength of the waves varies under the influence of Jupiter's magnetic
field in a pattern that repeats every 9 hours 56 minutes. Because the magnetic
field originates in Jupiter's core, this variation shows how fast the plant's
interior spins.
Jupiter's rapid rotation makes it bulge at the equator and flatten at the poles.
The planet's diameter is about 7 percent larger at the equator than at the poles.
Mass and density
Jupiter is heavier than any other planet. Its mass (quantity of
matter) is 318 times larger than that of Earth. Although Jupiter has a large
mass, it has a relatively low density. Its density averages 1.33 grams per cubic
centimeter, slightly more than the density of water. The density of Jupiter is
about 1/4 that of Earth. Because of Jupiter's low density, astronomers believe
that the planet consists primarily of hydrogen and helium, the lightest elements.
Earth, on the other hand, is made up chiefly of metals and rock. Jupiter's mix of
chemical elements resembles that of the sun, rather than that of Earth.
Jupiter may have a core made up of heavy elements. The core may be of about the
same chemical composition as Earth, but 20 or 30 times more massive.
The force of gravity at the surface of Jupiter is up to 2.4 times stronger than
on Earth. Thus, an object that weighs 100 pounds on Earth would weigh as much as
240 pounds on Jupiter.
The atmosphere of Jupiter is composed of about 86 percent hydrogen, 14 percent
helium, and tiny amounts of methane, ammonia, phosphine, water, acetylene,
ethane, germanium, and carbon monoxide. The percentage of hydrogen is based on
the number of hydrogen molecules in the atmosphere, rather than on their total
mass. Scientists have calculated these amounts from measurements taken with
telescopes and other instruments on Earth and aboard spacecraft.
These chemicals have formed colorful layers of clouds at different heights. The
highest white clouds in the zones are made of crystals of frozen ammonia. Darker,
lower clouds of other chemicals occur in the belts. At the lowest levels that can
be seen, there are blue clouds. Astronomers had expected to detect water clouds
about 44 miles (70 kilometers) below the ammonia clouds. However, none have been
discovered at any level.
Jupiter's most outstanding surface feature is the Great Red Spot, a swirling mass
of gas resembling a hurricane. The widest diameter of the spot is about three
times that of Earth. The color of the spot usually varies from brick-red to
slightly brown. Rarely, the spot fades entirely. Its color may be due to small
amounts of sulfur and phosphorus in the ammonia crystals.
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The planet Jupiter's Great Red Spot is
a huge mass of swirling gas. At its widest, it is about three times the
diameter of the Earth. Image credit: NASA
The edge of the Great Red Spot circulates at a speed of about 225 miles (360
kilometers) per hour. The spot remains at the same distance from the equator but
drifts slowly east and west.
The zones, belts, and the Great Red Spot are much more stable than similar
circulation systems on Earth. Since astronomers began to use telescopes to
observe these features in the late 1600's, the features have changed size and
brightness but have kept the same patterns.
Temperature
The temperature at the top of Jupiter's clouds is about -230 degrees F (-145
degrees C). Measurements made by ground instruments and spacecraft show that
Jupiter's temperature increases with depth below the clouds. The temperature
reaches 70 degrees F (21 degrees C) -- "room temperature" -- at a level where
the atmospheric pressure is about 10 times as great as it is on Earth. Scientists
speculate that if Jupiter has any form of life, the life form would reside at
this level. Such life would need to be airborne, because there is no solid surface
at this location on Jupiter. Scientists have discovered no evidence for life
on Jupiter.
Near the planet's center, the temperature is much higher. The core temperature
may be about 43,000 degrees F (24,000 degrees C) -- hotter than the surface
of the sun.
Jupiter is still losing the heat produced when it became a planet. Most
astronomers believe that the sun, the planets, and all the other bodies in the
solar system formed from a spinning cloud of gas and dust. The gravitation of the
gas and dust particles packed them together into dense clouds and solid chunks of
material. By about 4.6 billion years ago, the material had squeezed together to
form the various bodies in the solar system. The compression of material produced
heat. So much heat was produced when Jupiter formed that the planet still
radiates about twice as much heat into space as it receives from sunlight.
Magnetic field
Like Earth and many other planets, Jupiter acts like a giant
magnet. The force of its magnetism extends far into space in a region surrounding
the planet called its magnetic field. Jupiter's magnetic field is about 14 times
as strong as Earth's, according to measurements made by spacecraft. Jupiter's
magnetic field is the strongest in the solar system, except for fields associated
with sunspots and other small regions on the sun's surface.
Scientists do not fully understand how planets produce magnetic fields. They
suspect, however, that the movement of electrically charged particles in the
interior of planets generates the fields. Jupiter's field would be so much
stronger than Earth's because of Jupiter's greater size and faster rotation.
Jupiter's magnetic field traps electrons, protons, and other electrically charged
particles in radiation belts around the planet. The particles are so powerful
that they can damage instruments aboard spacecraft operating near the planet.
Within a region of space called the magnetosphere, Jupiter's magnetic field acts
as a shield. The field protects the planet from the solar wind, a continuous flow
of charged particles from the sun. Most of these particles are electrons and
protons traveling at a speed of about 310 miles (500 kilometers) per second. The
field traps the charged particles in the radiation belts. The trapped particles
enter the magnetosphere near the poles of the magnetic field. On the side of the
planet away from the sun, the magnetosphere stretches out into an enormous
magnetic tail, often called a magnetotail, that is at least 435 million miles
(700 million kilometers) long.
Radio waves given off by Jupiter reach radio telescopes on Earth in two forms
-- bursts of radio energy and continuous radiation. Strong bursts occur when
Io, the closest of Jupiter's four large moons, passes through certain regions
in the planet's magnetic field. Continuous radiation comes from Jupiter's surface
as well as from high-energy particles in the radiation belts.
Satellites
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Callisto, a moon of Jupiter, is covered with craters produced when asteroids and comets struck its icy surface. Beneath the surface may be an ocean of salty liquid water. Image credit: NASA
Jupiter has 16 satellites that measure at least 6 miles (10 kilometers) in diameter.
It also has many smaller satellites. Jupiter's four largest satellites, in order
of their distance from Jupiter, are Io, Europa, Ganymede, and Callisto. These
four moons are called the Galilean satellites. The Italian astronomer Galileo
discovered them in 1610 with one of the earliest telescopes.
Io has many active volcanoes, which produce gases containing sulfur. The yellow-orange
surface of Io probably consists largely of solid sulfur that was deposited by
the eruptions. Europa ranks as the smallest of the Galilean satellites, with
a diameter of 1,945 miles (3,130 kilometers). Europa has a smooth, cracked,
icy surface.
The largest Galilean satellite is Ganymede, with a diameter of 3,273 miles
(5,268 kilometers). Ganymede is larger than the planet Mercury. Callisto, with
a diameter of 2,986 miles (4,806 kilometers), is slightly smaller than Mercury.
Ganymede and Callisto appear to consist of ice and some rocky material. The
two satellites have many craters.
Jupiter's remaining satellites are much smaller than the Galilean moons. Amalthea
and Himalia are the next largest. Potato-shaped Amalthea is about 163 miles (262
kilometers) in its long dimension. Himalia is 106 miles (170 kilometers) in
diameter. Most of the remaining satellites were discovered by astronomers using
large telescopes on Earth. Scientists discovered Metis and Adrastea in 1979 by
studying pictures that had been taken by the Voyager spacecraft.
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Ganymede, a moon of Jupiter, has craters and cracks on its surface. Asteroids and comets that hit Ganymede made the craters. The cracks are due to expansion and contraction of the surface. Image credit: NASA
Rings
Jupiter has three thin rings around its equator. They are much fainter
than the rings of Saturn. Jupiter's rings appear to consist mostly of fine dust
particles. The main ring is about 20 miles (30 kilometers) thick and more than
4,000 miles (6,400 kilometers) wide. It circles the planet inside the orbit of
Amalthea.
The impact of Comet Shoemaker-Levy 9
In March 1993, astronomers Eugene Shoemaker, Carolyn Shoemaker, and David H. Levy
discovered a comet near Jupiter. The comet, later named Shoemaker-Levy 9,
probably once orbited the sun independently, but had been pulled by Jupiter's
gravity into an orbit around the planet. When the comet was discovered, it had
broken into 21 pieces. The comet probably had broken apart when it passed close
to Jupiter.
Calculations based on the comet's location and velocity showed that the fragments
would crash into Jupiter's atmosphere in July 1994. Scientists hoped to learn
much about the effects of a collision between a planet and a comet.
Astronomers at all the major telescopes on Earth turned their instruments toward
Jupiter at the predicted collision times. Scientists also observed Jupiter with
the powerful Hubble Space Telescope, which is in orbit around Earth; and the
remotely controlled space probe Galileo, which was on its way to Jupiter.
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Scars from the crash of Comet Shoemaker-Levy 9 appear on Jupiter's surface as a series of maroon blotches in this photo. The comet broke into 21 pieces before it hit Jupiter in 1994.
Image credit: Hubble Space Telescope Comet Team and NASA
The fragments fell on the back side of Jupiter as viewed from Earth and the
Hubble Space Telescope. But the rotation of Jupiter carried the impact sites
around to the visible side after less than half an hour. Scientists estimate that
the largest fragments were about 0.3 to 2.5 miles (0.5 to 4 kilometers) in
diameter. The impacts were directly observable from Galileo, which was within
about 150 million miles (240 million kilometers) from Jupiter. However, damage to
certain of the probe's instruments limited its ability to record and send data.
The impacts caused large explosions, probably due to the compression, heating,
and rapid expansion of atmospheric gases. The explosions scattered comet debris
over large areas, some with diameters larger than that of Earth. The debris
gradually spread into a dark haze of fine material that remained suspended for
several months in Jupiter's upper atmosphere. If a similar comet ever collided
with Earth, it might produce a haze that would cool the atmosphere and darken the
planet by absorbing sunlight. If the haze lasted long enough, much of Earth's
plant life could die, along with the people and animals that depend on plants.
Flights to Jupiter
The United States has sent six space probes to Jupiter: (1) Pioneer 10, (2)
Pioneer-Saturn, (3) Voyager 1, (4) Voyager 2, (5) Ulysses, and (6) Galileo.
Pioneer 10 was launched in 1972 and flew within 81,000 miles (130,000 kilometers)
of Jupiter on Dec. 3, 1973. The probe revealed the severe effects of Jupiter's
radiation belt on spacecraft. Pioneer 10 also reported the amount of hydrogen and
helium in the planet's atmosphere. In addition, the probe discovered that Jupiter
has an enormous magnetosphere.
Pioneer-Saturn flew within 27,000 miles (43,000 kilometers) of Jupiter in
December 1974. The craft provided close-up photographs of Jupiter's polar regions
and data on the Great Red Spot, the magnetic field, and atmospheric temperatures.
Voyager 1 and Voyager 2 flew past Jupiter in March and July 1979, respectively.
These craft carried more sensitive instruments than did the Pioneers, and
transmitted much more information. Astronomers used photographs taken by the
Voyagers to make the first detailed maps of the Galilean satellites. The Voyagers
also revealed sulfur volcanoes on Io, discovered lightning in Jupiter's clouds,
and mapped flow patterns in the cloud bands.
Ulysses was launched in October 1990 and passed by Jupiter in February 1992. The
European Space Agency, an organization of Western European nations, had built the
probe mainly to study the sun's polar regions. Scientists used the tremendous
gravitational force of Jupiter to put Ulysses into an orbit that would take it
over the sun's polar regions. As Ulysses passed by Jupiter, it gathered data
indicating that the solar wind has a much greater effect on Jupiter's
magnetosphere than earlier measurements had suggested.
Galileo began its journey to Jupiter in October 1989. The craft released an
atmospheric probe in July 1995. In December 1995, the probe plunged into
Jupiter's atmosphere. The probe penetrated deep into the cloud layers and
measured the amount of water and other chemicals in the atmosphere. Also in
December 1995, Galileo went into orbit around Jupiter. Over the next several
years, the craft monitored Jupiter's atmosphere and observed the planet's major
satellites. Galileo's mission was extended in 1997 and again in 1999. Eventually,
however, the craft ran low on fuel. In September 2003, mission managers
intentionally crashed Galileo into Jupiter's atmosphere to avoid any risk of the
craft crashing into and contaminating Jupiter's moon Europa. Galileo's
observations of Europa had shown that it might have an ocean below its surface
capable of supporting life.
Contributors: Peter J. Gierasch, Ph.D., Professor of Astronomy,
Cornell University. Philip D. Nicholson, Ph.D., Professor of Astronomy, Cornell
University.
How to cite this article: To cite this article, World Book recommends the
following format: Gierasch, Peter J., and Philip D. Nicholson. "Jupiter." World
Book Online Reference Center. 2004. World Book, Inc.
(http://www.worldbookonline.com/wb/Article?id=ar293080.)

Question: what is the fourth brightest object in the sky

observation of Jupiter through an amateur telescope.

Jupiter is usually the fourth brightest object on the sky (after the Sun, the Moon and Venus); sometimes Mars is brighter than Jupiter.

what is the fourth brightest object in the sky

Question: which planet is the fourth brightest in the sky

which planet is the fourth brightest in the sky

Question: what kind of telescope is used to observe jupiter

what kind of telescope is used to observe jupiter

Question: where is jupiter in the sky brightest

Question: what are the 4 brightest objects in the sky

what are the 4 brightest objects in the sky

Question: what is the fourth brightest object in the sky, after the sun, the moon and

what is the fourth brightest object in the sky, after the sun, the moon and

observation of Jupiter through an amateur telescope .

Jupiter is usually the fourth brightest object on the sky ( after the Sun , the Moon and Venus ) ; sometimes Mars is brighter than Jupiter .

Promatranje Jupiter kroz amaterski teleskop. Jupiter je obično četvrti najsvjetliji objekt na nebu (nakon Sunca, Mjeseca i Venere); ponekad je Mars svjetliji od Jupitera.

Promatranje Jupiter kroz amaterski teleskop.

Jupiter je obično četvrti najsvjetliji objekt na nebu (nakon Sunca, Mjeseca i Venere); ponekad je Mars svjetliji od Jupitera.

observation of Jupiter through an amateur telescope. Jupiter is usually the fourth brightest object on the sky (after the Sun, the Moon and Venus); sometimes Mars is brighter than Jupiter.

observation of Jupiter through an amateur telescope.

Jupiter is usually the fourth brightest object on the sky (after the Sun, the Moon and Venus); sometimes Mars is brighter than Jupiter.

Since Jupiter’s orbit is outside that Earth, the phase angle of Jupiter viewed from Earth never exceeds 11.5°: Jupiter always appears almost fully illuminated when viewed through Earth’s telescopes.

[139] DURING THE MONTHS of November and December of 1973, Pioneer 10 sent back over 500 images of Jupiter. Most of these were taken from a comparatively large distance from the planet and show very little detail compared to pictures that have already been taken with telescopes based on Earth. However, those pictures that were obtained within 48 hours of the closest approach of the spacecraft to Jupiter are considerably better than any seen previously. Not only is the resolution greater, thereby revealing hitherto unseen details on the planet, but Jupiter has now been seen from viewpoints not available to observers based on Earth.
Because Jupiter is many times further from the Sun than the Earth, the angle subtended by the Earth and the Sun at Jupiter, i.e., the phase angle, never exceeds 11.5 degrees. Astronomers can see the planet only as a fully illuminated disc. From Earth, it is not possible to see Jupiter illuminated from the side or from behind as the Moon can be seen, with its crescent and half-moon shapes. Pioneer 10 provided the first opportunity to view Jupiter under varying illumination conditions, and this chapter presents some of the images obtained.
Figure 8-1 shows the trajectory of the spacecraft for 20 hours before and after its closest approach to Jupiter. As it approached the planet, the spacecraft was below the equatorial plane. Later it....
...crossed this plane and departed from the planet north of the plane. The lower part of the illustration shows schematically the change in the illumination of the disc of Jupiter, as seen from the spacecraft, at times corresponding to the positions of the spacecraft shown on the trajectory.
At 20 hours before closest approach, the dark limb is at the left of the planet. At 12 hours, it is under the planet as the spacecraft approaches below the equatorial plane. Just before closest approach, the dark limb slips around to the right side of the planet. Then the terminator rapidly sweeps across the view of the planet from the spacecraft, until the whole disc is dark as the spacecraft plunges into the planet's shadow. As Pioneer 10 emerges from the shadow, its images reveal a crescent Jupiter, the beginning of a unique series of pictures.
In the following pages, the images taken within four days of closest approach are designated with a code, such as A28 or B17. "A" images are before closest approach (periapsis) and "B" images are after closest approach. A fuller explanation of the code and a listing of the significant information about each image is given in Appendix 2. All dates and times used in this chapter are Universal Time (UT) which is the same as Greenwich Mean Time (GMT). DOY stands for day of year, i.e., January 1 is DOY 1, and December 31 is DOY 365.
The series of blue-channel pictures on this and the facing page was taken at two-day intervals, starting on DOY 321, 17 days before Pioneer 10's closest approach to Jupiter. None of these pictures has resolution as good as that which can be obtained from Earth. The scan lines, because they are so few, are quite evident.
The Great Red Spot and the banded structure are clearly visible even at these great distances, which range from 16 to 7.5 million km (10 to 4.7 million mi.). The terminator is on the west side of the disc of the planet and displaced slightly toward the south.
It is interesting to note that the detail, as seen by the IPP, is approximately the same as that which would be seen by the unaided human eye at [141] the same distance from Jupiter. All the pictures reproduced in this chapter show Jupiter as it might have been seen by an astronaut in a manned spacecraft, flying by Jupiter along the path of Pioneer 10.
The pictures on this and the facing page have all been reproduced to the same angular scale. The relative sizes are exactly as they would have appeared to an observer on the spacecraft as it approached Jupiter. These blue channel images have been selected to show Jupiter at approximately one day intervals, starting six days before periapsis. The last image shown in this series has a resolution comparable with that obtainable from Earth when the "seeing" conditions are good. Many of the pictures obtained over this period of time show satellites in the field of view. They are, however, too far away from the spacecraft to be resolved into detail and usually too far from the planet's disc to be seen in the pictures shown here. One satellite appears in the last frame of this series, slightly below and to the left of the disc of the planet.
Figure
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8-2(a)
321:01:36
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10.0
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329:06:46
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Figure
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8-3(a)
332:16:02
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333:01:44
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This spectacular series of consecutive pictures was taken over a period of four hours, between 44-1/2 and 40-1/2 hours before periapsis. The Great Red Spot is prominent, and the shadow of Io traverses the disc of the planet. Cosmetic enhancement as described in Chapter 7 was applied to all these images, especially to A49. A49 is shown before and after cosmetic enhancement in Figure 7-7.
Figure
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8-4(a)
A51
336:06:55
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A50
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A48
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A46
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[143] The series of pictures, A39, A35, A31, and A28 on the next four pages shows one complete rotation of the planet. The final picture in the series is the last picture possible before the planet overfilled the field of view. Part of the data used to create A35 is missing. This results in the comb-like truncation of the northwest limb. This same effect occurs in several pictures in this chapter.
The gross morphology of belts and zones, with structures showing turbulence and convective cells in the middle latitudes of the planet, is clearly seen. The small white spots surrounded by dark rings, seen mainly in the southern hemisphere, indicate regions of intense vertical convective activity, somewhat similar to cumulonimbus or thunderclouds.
In places where the clouds are relatively featureless and have a bluish coloration, the IPP image provides a look down into the deepest and warmest parts of the atmosphere. These are called "blue festoons."
Figure
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8-5(a)
A39
336:14:33
22.3
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[148] At the head of this bright plume is a rising column of warm particles from a source deep within the clouds. The tail is to the left because the atmosphere moves more slowly at the upper regions than lower down. The southerly deflection of the plume, and the scalloped edges of the belt above the plume, support the theory that there is strong convective circulation between the lower and middle latitude belts and zones.
A color picture is shown together with the black and white images of the blue and red channels from which the colored image was constructed.
Figure
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8-6
A22
337:08:52
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17.8
[150] Red spots, other than the Great Red Spot, have been observed from the ground on previous occasions. This first close look at a northern hemisphere red spot shows convincingly the great morphological similarity between it and the wellknown and much studied Great Red Spot in the southern hemisphere. Ground-based observations indicate that this particular feature is very young- probably not more than 1 8-months old at the time of the passage of Pioneer 10.
Figure
.
8-7
A-16
337:11:23
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16.0
The pictures on this and the facing page are of similar areas of Jupiter and provide the best coverage of this enormously turbulent region. The "hooks" are several thousands of kilometers in extent. The belt structure is unstable at higher
latitudes. At the top of the pictures, a belt fragment, the darker elongated feature, can be seen in the transition zone between the belts and the relatively smooth looking polar region.
Figure
.
8-8
A9
337:14:47
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On this and the facing page is shown the type of fine detail revealed in the cloud photographs that will help scientists to unravel the complex behavior of the Jovian atmosphere.
In all the images, gross differences between the red and blue images are apparent. The fine repetitive wave-like structure discernible in the red channel image, which shows up as a bluish ripple on the colored image, is not real and should be ignored.
Figure
.
8-10
A7
337:16:19
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The differences between the red and blue channel images are not only intriguing, but also important from the scientific analysis standpoint. This image shows again the plume conspicuous on Figure 8-6. But the detail is very much improved on this picture, which is one of the best close encounter pictures. Here features are seen that can be only glimpsed from Earth. Unfortunately, Pioneer 10 flew by so quickly that movements in the clouds cannot be detected between one picture and another. Even so, the nature of the detail enables inferences to be drawn concerning the dynamic properties of the Jovian atmosphere from these images.
Figure
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8-12
A5
337:18:28
72.6
45.1
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.
While receding from Jupiter, Pioneer 10 showed Jupiter from a viewpoint never before seen by man: sunrise on a crescent-shaped planet. This series of images shows the northern hemisphere red spot, the Great Red Spot, and parts of the large plume. Contrast is lower in this crescent phase-a fact that can be explained in terms of the way in which the cloud particles scatter light. Irregularities in the profile of Jupiter are caused by a characteristic of the mechanism that drives the telescope.
The final picture in this series is the last one taken by the Pioneer 10 spacecraft on its epic journey, on New Year's Eve 1973.
Figure
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8-13(a)
B11
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B23
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B69
341:17:08
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--
365:18:08
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99 5
97.0

Question: what is the phase angle of jupiter from earth

what is the phase angle of jupiter from earth

Question: where is jupiter almost completely illuminated

where is jupiter almost completely illuminated

Question: where is jupiter's orbit located on earth

where is jupiter's orbit located on earth

Question: how is jupiter seen from earth

Question: how does jupiter always appear

almost fully illuminated when viewed through Earth’s telescopes

almost fully illuminated when viewed through Earth ’s telescopes

Question: where can you see jupiter from earth

Question: when is jupiter almost completely illuminated

when is jupiter almost completely illuminated

Question: what is the difference between earth and jupiter

what is the difference between earth and jupiter

Since Jupiter ’s orbit is outside that Earth , the phase angle of Jupiter viewed from Earth never exceeds 11.5 ° : Jupiter always appears almost fully illuminated when viewed through Earth ’s telescopes .

A small telescope will usually show Jupiter’s four Galilean satellites as the light points of that zone and the connective clouds in Jupiter’s atmosphere.

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Jupiter is the largest planet in our Solar System. It is one of the ‘Gas Giants’ and the fifth planet from the sun. To put the size of Jupiter in perspective, it takes it almost 12 years to fully orbit its sun. It is known for its large Great Red Spot and contrasting dark and light cloud belts. It is one of the brightest objects in the sky after the sun, the moon and the planet Venus. For several months each year Jupiter shines brightly for several hours before and after midnight, thanks to its huge size. Many people enjoy looking for Jupiter in the sky and it is a great way for a beginner without expensive equipment to enjoy observing the beauty of distant planets.
Steps
Part 1
Part 1 of 4:Getting Equipped
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- 1Get a sky map. Before you start looking for Jupiter, you should get hold of a sky map which can show you where in the sky to start looking. For more advanced astronomers, there are numerous sophisticated maps of the sky which show the position and trajectory of the planets. For those inexperienced in reading these paper maps there are a number of smart phone apps which you can download which will help you to find Jupiter and the other planets and stars in the sky.
- With some smartphone apps all that you have to do is hold the phone up to the sky and it will identify the stars and planets for you.
- 2Ready some binoculars. Jupiter is so massive and bright in the sky that it can be viewed with a good pair of binoculars. Binoculars that magnify seven times human eyesight will be effective and will reveal Jupiter as a small white disk in the sky. [1] X Research source If you don’t know what strength your binoculars are look at numbers on the side, if it says 7x another number then they magnify seven times and will enable to observe Jupiter.Advertisement
- 3Get a telescope. To really get a good view of the Jupiter’s spectacular features, your observations will be improved with even an entry-level telescope. This equipment will help you to see Jupiter’s famous belts, all four of its moons, and potentially even the Great Red Spot. The range of telescopes available is huge, but for beginners a 60 or 70mm refractor telescope is a good place to start.[2] X Research source
Part 2
Part 2 of 4:Preparing for your Observation
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- 1Get to know good seeing conditions. You can save time and avoid fruitless hours by learning to identify good viewing conditions quickly. Before setting up the telescope take a look at the stars. Ask yourself if the stars are twinkling brightly through the sky. If so, this suggests that there is a turbulent atmosphere. Such conditions make planet observation more difficult, instead you want calm night-sky. In a steady night with good seeing conditions, the sky might appear somewhat hazy. [4] X Research source
- 2Find the right time of the day or night. The best time to observe planets is at night, but Jupiter is so bright that it can sometimes be seen shortly after dusk, and shortly before dawn. At dusk it will rise in the east, but as night goes on Jupiter will appear to travel westwards through the sky. At mid-northern latitudes it will set in the west a little before the sun rises in the east each morning.[6] X Research source
- 3Pick your spot and be ready to wait. Be sure to set yourself up in a good place where it is dark and quiet so you can concentrate on your planet gazing. Your backyard is perfect, but remember that observing planets can be a slow and engrossing business, so be sure to wrap up warm and be prepared for a lengthy wait. If you are planning on documenting your observation have any materials with you so you don’t have to leave your observation post.
Part 3
Part 3 of 4:Observing Jupiter
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- 1Find Jupiter with binoculars. Find a comfortable and steady position and if possible mount your binoculars on a camera tripod, or something else steady and fixed so they won’t shake as you use them. With the binoculars you should be able to see Jupiter as a white disk.
- You may also be able to see up to four distinct specs of light near Jupiter, these are its four Galilean moons. Jupiter has at least 63 moons in orbit. In 1610, Galileo named the four main moons Io, Europa, Ganymede, and Callisto. How many you can see will depend on their position orbiting Jupiter.
- Even if you have a telescope, it can be helpful to use binoculars to spot Jupiter in the sky before moving on to the telescope for a more detailed observation.
- 2Take a closer look with a telescope. Once you have spotted Jupiter, you can begin a more detailed observation of the planet’s surface through your telescope and identify some of its key features. Jupiter is famous for its darker cloud belts and lighter zones which are appear laterally across the planet’s surface. Try to identify the central light area known as the equatorial zone and the darker equatorial belts north and south of it.[7] X Research source
- When searching for the belts, keep trying. It takes time to learn how to spot the belts through a telescope. It's a good idea to try this with someone who is already familiar with spotting them.
- 3Find the Great Red Spot. One of Jupiter’s most fascinating features is its Great Red Spot. This giant oval storm, larger than Earth, has been observed on Jupiter for more than 300 years. You can locate it at the outer edge of the south equatorial belt. The spot shows clearly how fast surface of the planet is changing; within the space of only an hour, you should be able to see the spot clearly move across the planet.
- The intensity of the Great Red Spot varies, and it can’t always be seen.
- It isn’t really that red, but more of orange or a pale pink colour.
Part 4
Part 4 of 4:Documenting your Observations
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- 1Try to sketch what you see. Once you have a good view of Jupiter you can document your astronomical observations by drawing Jupiter and recording its appearance. This is essentially a less high-tech version of what astronomy is all about, observing, documenting and analysing what you see in the sky. Jupiter is ever-changing so try to sketch it in around twenty minutes. You’ll be following in a great tradition of astronomical drawing.[8] X Research source
- 2Do some Jupiter Photography. If you prefer a more technologically advanced method of recording your observations you could try photographing Jupiter. Much like telescopes, the camera you use can be very powerful or more basic and still get results. Some star-gazers use charged coupled device cameras or even cheap and lightweight webcams for photographing planets with telescopes.[9] X Research source
- 3Make a Jupiter Movie. One great way to track the constant change on the surface of Jupiter and the position of its moons is to film it. You can do this in much the same way as you would photograph it.
- Use your notes to compare different observations to keep track of changes on the surface of the planet and to find things of interest.
- The clouds are turbulent and the planet's appearance can change dramatically in just a few days.
Community Q&A
- QuestionWhat time is best to see Jupiter?MattiskyCommunity AnswerIt depends on your location and where Jupiter is right now. There are a lot of apps out there that can help you to prepare your observations (for Android: Star Walk, for PC/Mac/Linux: Stellarium). You can enter your location and see where the the planets are from your point of view.
- QuestionHow can I be assured that it is the planet?MattiskyCommunity AnswerStars appear as points, no matter how large you magnify them. For planets, and especially Jupiter because of its size, you'll see that you can actually magnify it to a circle.
- QuestionWhy can't I see Jupiter at night?Community AnswerJupiter can be seen by the naked eye only on cloudless nights, away from light pollution. It can be sometimes mistaken for a star.
Tips
- Always observe from a dark area, such as your backyard.
- NASA information on Jupiter can be found at: https://www.nasa.gov/jupiter, and NASA information on the spacecraft Galileo's legacy can be found at: http://solarsystem.nasa.gov/galileo/.
- Download the Google Sky Map app on your phone, it will be much easier to spot it that way.
Warnings
- While sky gazing, pay attention the weather and dress appropriately to keep yourself protected from the elements.Thanks!
Things You'll Need
- Pair of binoculars (optional)
- Telescope (optional)
- Sky guide or chart
References
- ↑ http://www.skyandtelescope.com/astronomy-news/observing-news/jupiter-big-bright-andbeautiful/
- ↑ http://www.astronomyhints.com/observing_jupiter.html
- ↑ http://www.telescope.com/Observing-Planets/p/99808.uts
- ↑ http://www.telescope.com/Observing-Planets/p/99808.uts
- ↑ https://skyandtelescope.org/observing/jupiter-an-observing-guide/
- ↑ http://earthsky.org/astronomy-essentials/visible-planets-tonight-mars-jupiter-venus-saturn-mercury
- ↑ http://www.telescope.com/Observing-Planets/p/99808.uts
- ↑ https://skyandtelescope.org/observing/jupiter-an-observing-guide/
- ↑ http://www.astronomyhints.com/observing_jupiter.html

Question: how many galilean satellites are in jupiter's atmosphere

A small telescope will usually show Jupiter’s four Galilean satellites as the light points of that zone and the connective clouds in Jupiter’s atmosphere.

how many galilean satellites are in jupiter's atmosphere

Question: what kind of clouds are in jupiter's atmosphere

what kind of clouds are in jupiter's atmosphere

Question: what type of telescope is usually used to view jupiter's four galilean satellites

what type of telescope is usually used to view jupiter's four galilean satellites

Question: what is used to show the light points of jupiter's four galilean satellites

what is used to show the light points of jupiter's four galilean satellites

Question: how many Galilean satellites are visible from a telescope

how many Galilean satellites are visible from a telescope

Question: which planet has four galilean satellites

which planet has four galilean satellites

Question: what are the light points of jupiter's atmosphere

what are the light points of jupiter's atmosphere

Question: where are the connective clouds located on jupiter

where are the connective clouds located on jupiter

A small telescope will usually show Jupiter ’s four Galilean satellites as the light points of that zone and the connective clouds in Jupiter ’s atmosphere .

Mali teleskop obično će pokazivati Jupiterova četiri galilejanska satelita kao svjetle točkice te zone i pojaseve oblaka u Jupiterovoj atmosferi.

Mali teleskop obično će pokazivati Jupiterova četiri galilejanska satelita kao svjetle točkice te zone i pojaseve oblaka u Jupiterovoj atmosferi.

A small telescope will usually show Jupiter’s four Galilean satellites as the light points of that zone and the connective clouds in Jupiter’s atmosphere.

A small telescope will usually show Jupiter’s four Galilean satellites as the light points of that zone and the connective clouds in Jupiter’s atmosphere.

Astronomical Division of the Physical Society of Split – Jupiter

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1. Jupiter (Voyager 1979) - kontrast je naknadno
uvećan.
2. Velika crvena pjega je najveća i najdugotrajnija
oluja na Jupiteru.
3. Velika crvena pjega
4. HST
je snimio pojavu aurore na Jupiteru u UV (ultraljubičastom) svjetlu.
5. Na fotogtafiju Jupitera su nadodani prstenovi
i njihovi pastirski sateliti
6. Glavni prsten
7. Jupiterovi unutrašnji sateliti: Metis, Adrasteja,
Amalteja i Tebe.
8. Jupiterovi galilejanski sateliti: Io, Europa,
Ganimed i Kalisto
9. Io i Europa ispred Jupitera
10. Komet Shoemaker-Levy 9, rastrgan jupiterovim
plimnim silama, putuje prema Jupiteru
11. Posljedice udara kometa Shoemaker-Levy 9
u Jupiter: u vidljivom svjetlu ...
12. ... i u infracrveom svjetlu. Gore lijevo
je Io.
13. Jupiter, snimila letjelica Cassini u studenom
2003.
Jupiter je jedan od planeta poznat
od prapovijesti. U rimskoj mitologiji, Jupiter je vrhovni bog.
Grčki pandan Saturnu je Zeus. Zeus je sin Kronosa (Saturna).
Sadržaj:
Osnovni podaci
Povijest istraživanja
Fizička svojstva
Magnetsko polje
Atmosfera
Jupiterovi prstenovi
Jupiterovi sateliti
Udar
kometa Shoemaker-Levy 9 u Jupiter
Još o Jupiteru na našim stranicama:
Galerija slika: Jupiter
i sateliti
Sunčev Sustav u teleskopu: Promatranje
Jupitera
Osnovni podaci
Jupiter je najveći planet sunčeva
sustava, s masom na koju otpada 71% ukupne planetne mase. Peti
je po udaljenosti od Sunca.
Jupiter (uz Saturna, Urana
i Neptuna) spada u plinovite
divove, planete vanjskog dijela sunčeva sustava. Saturn i Jupiter se još
nazivaju pravi divovi. Jupiter obilazi Sunce na prosječnoj udaljenosti
od 778 413 000 km, t.j. 5.21 puta dalje od Zemlje.
U stvarnosti, ta udaljenost varira od 4.95 do 5.5 a.j. (zbog eliptičnosti
putanje). Jedna jupiterova godina t.j. obilazak
oko Sunca, traje 11.86 godine. Okrene se oko
svoje osi za 9 sati i 50 minuta. Periodi rotacije se razlikuju od sloja
do sloja zbog različitih atmosferskih gibanja. Ekvatorski
polumjer Jupitera iznosi 71 492 km, a polarni mu je, zbog brze
rotacije, oko 4% manji. Masa mu je 1.8988x1027 kg, ili
oko 318 masa Zemlje.
Jupiter je jedan od najsvijetlijih objekata na nebu (iza Sunca, Mjeseca
i Venere) pa je zato i poznat od davnina. Mali teleskop
je dovoljan da se ugledaju galilejanski sateliti (slika
4.): Io, Europa, Ganimed i Kalisto,
a oni s boljim vidom će zamijetiti zone i pojaseve paralelne ekvatoru,
te veliku crvena pjegu (slika 2.).
Povijest istraživanja
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13. Galilei
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Jupiter je, zbog svog sjaja, prepoznat još u prapovijesti.
Galileo Galilei (slika
13.) je, 1610. godine, prvi uperio teleskop
prema njemu te otkrio 4 njegova satelita (Io,
Europa, Ganimed
i Kalisto), koji se
po njemu zovu galilejanski (slika 8.).
To je bio dokaz kopernikove heliocentrične teorije jer se dokazalo da
se ne vrti sve oko Zemlje.
Istraživanja Jupitera provedena su letjelicama Pioneer
10 i 11, Voyager 1 i 2, Ulysses, Galileo i Cassini (na putu prema
Saturnu), a fotografirao ga je i HST.
Fizička svojstva
Mjerenja gravitacijskog polja ukazuju
na postojanje značajne koncentracije stjenovitog i ledenog materijala
u jupiterovoj unutrašnjosti, vjerojatno jezgre mase
10-15 masi Zemlje. Tlak u unutrašnjosti Jupitera dostiže više od
desetaka milijuna bara.
Na moguću kameno-ledenu jezgru nastavlja se debeli
sloj metalnog vodika. Naime, pri tlaku od oko 2x1011
Pa (paskala), vodik prelazi u metalno tekuće stanje. To je stanje pri
kojem su molekule vodika tako gusto složene da pojedine atome susjedna
molekula privlači jednako kao i atom partner u istoj molekuli. Posljedica
toga je razbijanje molekula. Pored toga događa se da i elektrone
u ljuskama privlače susjedne jezgre, pa dolazi do ionizacije
(odvajanja elektrona od jezgri). Vodik postaje vrlo vodljiv (slično metalima),
pa se zato ovo stanje zove metalni tekući vodik. Ovaj sloj vjerojatno
sadrži i primjese helija i raznog leda. Postojanje metalnog vodika je
dokazano u laboratorijima na Zemlji 1996. godine.
Na sloj metalnog vodika se u blagom prelazu nastavlja
sloj vodika i helija u molekularnom obliku koji iz tekućeg stanja
(dublje) prelazi u plinovito (bliže površini). Atmosfera koju vidimo je
samo vanjski dio ovog sloja. Ovaj sloj sadrži i manje količine vode, ugljik-dioksida,
metana i drugih jednostavnih spojeva.
Jupiter je po sastavu 90% vodik i 10% helij (po masenom
udjelu), sa tragovima vode, metana i amonijaka. Taj sastav približno
odgovara i sastavu prvotnog oblaka od kojeg je i nastao Sunčev Sustav.
Jupiterova unutrašnjost je vrlo vruća, temperature
u središtu su čak 20 000 K,
pa Jupiter 1.5 puta više energije zrači u svemir nego što je prima od
Sunca. Ravnotežna temperatura (ona koju bi imao da ga grije samo Sunce)
za Jupiter iznosi 140 K, ali je stvarna temperatura njegovih vanjskih
dijelova oko 160 K. To se objašnjava Kelvin-Helmholtzovim mehanizmom (potencijalna
energija gravitacijskog polja sažimanjem prelazi u unutarnju energiju).
Za opaženu količinu energije bi bilo dovoljno da se Jupiter sažme za 1
mm godišnje. Iako velik, Jupiter je po dimenzijama
vrlo daleko od zvijezda ili smeđih
patuljaka. Trebala bi mu 80 puta veća masa da u njegovu središtu
započnu nuklearne reakcije i tako postane zvijezda.
Magnetsko polje
Jupiter nije mjesto u čijoj blizini bi ljudi mogli boraviti.
Još je 1955. godine otkrivena radio-emisija s Jupitera, što je upućivalo
na jako magnetsko polje. Jako magnetsko polje Jupitera
posljedica je debelog sloja metalnog vodika i brze rotacije. Magnetska
je os priklonjena za 11° prema osi rotacije.
U atmosferi, ono iznosi oko 10-3 T (4000
puta jače od Zemljinog).
Jupiterovo magnetsko polje je oko 100 puta veće od
zemljinog. Proteže se nekoliko milijuna kilometara u smjeru Sunca
i čak oko 650 milijuna km u suprotnom pravcu, te doseže
i do saturnove putanje. Magnetsko polje stvara jake struje visoko-energetskih
čestica koje su 10 puta jače od onih u Van
Allenovim pojasevima.
Ono obuhvaća i putanje jupiterovih satelita, pa se time djelomično objašnjava
velika vulkanska aktivnost na Iou.
Između Jupitera i Ioa izmjerena je električna struja jakosti 5 milijuna
Ampera (5 MA). Naelektrizirane čestice ubrzane do vrlo velikih brzina
udaraju u Iovu površinu i izbijaju atome s površine. Izbijeni atomi čine
Iov Torus, veliki prstenasti oblak električni nabijenih čestica oko Iove
putanje.
Jupiterovo magnetsko polje uzrokuje i polarnu svjetlost (slika
4.).
Atmosfera
Kroz teleskop se na Jupiteru
mogu lako uočiti zone i pojasevi (slika 1.)
paralelni ekvatoru, te nekoliko pjega (slika
2.) od kojih je najpoznatija Velika Crvena
Pjega (slika 3.). Blijedožućkaste
zone predstavljaju područja gdje plin izvire, a crvenkasto-smeđi pojasevi
mjesta gdje plin ponire. Razlike u boji potječu od temperaturnih i kemijskih
razlika. Zone su toplije, a boja im potječe od kristala amonijaka (NH3).
Pojasevi su hladniji, a boju im daju kristali amonijeva hidrosulfida (NH4SH).
Vjetrovi koji dosežu i do 530 km/h imaju u
zonama i pojasevima suprotne smjerove. Sonda sa letjelice Galileo je detektirala
vjetrove do dubine od nekoliko tisuća kilometara u dubinu, gdje je prestala
funkcionirati usljed velikog pritiska. Jupiterova je atmosfera vrlo turbulentna.
Izvor energije za to ne potječe od Sunca, već od Jupiterove unutarnje
energije.
Oblaci u živopisnim bojama koji daju karakterističan
izgled Jupiteru ograničeni su na dubine do samo 0.1 do 0.3% jupiterova
radijusa. Smatra se da su kemijski spojevi elemenata (osobito sumpora)
kojih ima u tragovima u gornjim dijelovima atmosfere odgovorni za ovakvu
šarolikost Jupitera.
Vjeruje se da postoje tri sloja oblaka na Jupiteru,
koje možemo razlikovati i po boji. Najdonji su plavi
oblaci od kristala amonijakovog leda. Iznad njih se nalaze bijeli
i smeđi oblaci od kristala amonij-hidrosulfida. Na vrhu atmosfere
se nalaze crveni oblaci od mješavine leda i
vode. Sonda sa letjelice Galileo je uočila samo slabašne naznake oblaka.
Međutim, novija promatranja pokazuju da je mjesto na koje je sonda ušla
u jupiterovu atmosferu bilo vrlo netipično (najtoplije i s najmanje oblaka
u to doba).
Velika Crvena Pjega je veliki (12 000 x 25
000 km) oval koja može narasti i do veličine od 3 Zemljina promjera. Boju
joj daju kristali fosfora. Smatra se da je to zapravo područje
visokog tlaka (anticiklona). Vrhovi oblaka Velike Crvene Pjege
značajno su viši i hladniji od okoline. Prvi put je
viđena prije više od 300 godina. Zasluge za njeno otkriće se najčešće
pripisuju Cassiniju i Robertu Hookeu.
Slične pojave postoje i na Saturnu
i Neptunu, ali nije zabilježena
nijedna ovako dugovječna.
Jupiterova atmosfera visoka je oko 1000 km,
a pretežno je građena od vodika (75.5%) i helija (23.8%),
a zastupljeni su i spojevi poput metana, amonijaka, vodene pare i sl.
Podaci s "Galilea" su pokazali da kisika ima mnogo manje od očekivanog
(manje nego na Suncu). Tlak, temperatura i gustoća prema središtu rastu,
te na dubini od 10 000 km ispod vrhova oblaka gustoća atmosfere narasta
do gustoće vode. Na razini sa tlakom od 150 milibara postoji inverzijski
sloj, toplije područje iznad hladnijeg, kakvo postoji i u Zemljinoj
stratosferi.
Za razliku od letjelica Pioneer 10 i 11, Voyageri 1 i 2 su u jupiterovoj
ionosferi izmjerili visoke temperature od 830°C (1003 K)
Jupiterovi prstenovi
Godine 1979 letjelica Voyager je otkrila Jupiterove prstenove
(slika 6.). Prstenovi
se uglavnom sastoje od mikrometarskih čestica prašine, a prostiru se sve
do površine planeta. Najbliži Jupiteru je Halo prsten, širok oko
20 000 km, koji ima oblik torusa (slika 5.).
Na Halo se nastavlja 7 000 km široki glavni prsten. Unutar glavnog prstena
se nalaze (slika 5.) i Jupiterovi sateliti
Metis i Adrasteja (slika 7.). Smatra se
da su ova dva satelita izvor materijala (udari meteorita
izbacuju krhotine u svemir) za glavni pojas, dok su druga dva mala unutarnja
satelita - Amalteja i Tebe
(slika 7.) - izvori materijala za vrlo
rijetke Amalthea Gossamer (unutar Amaltejine putanje) i Thebe Gossamer
(između putanja Amajteje i Tebe) prstenove (slika
5.) koji se nastavljaju na glavni prsten.
Letjelica Galileo prošla je 5. studenog 2002. godine
kroz Gossamer prsten. Rezultati mjerenja očekuju se tek za nekoliko
mjeseci jer letjelica još nije stigla poslati sve podatke prema Zemlji.
Podaci o svojstvima ovih i drugih planetnih prstenova nalaze se na stranici:
Usporedba planetnih prstenova.
Jupiterovi sateliti
Jupiter, kao i svi plinoviti
divovi (Jupiterova skupina planeta: Jupiter, Saturn, Uran i Neptun) ima
mnoštvo satelita, ukupno
61 , koji su podijeljeni u nekoliko grupa.
U prvu grupu spadaju 4 mala, podosta kružna satelita
sa kružnim putanjama u ravnini jupiterova ekvatora. To su: Metis,
Adrasteja (Adrestea), Amalteja
(Amalthea) i Tebe (Thebe) (slika
7.).
Drugu grupu čine galilejanski sateliti - 4
velika satelita koje je 1610. otkrio Galileo Galilei kada je prvi put
promatrao Jupiter uz pomoć teleskopa. Tu spadaju (slika
8.): Io, Europa,
Ganimed i Kalisto.
Putanju su im u ravnini ekvatora. Sva četiri imaju sinkronu rotaciju.
Za razliku od ostalih staelita u Sunčevom Sustavu čija svojstva najviše
ovise o masi pojedinih satelita, na svojstva Galilejanskih satelita više
utječe udaljenost od Jupitera.
Io, koji je od ova 4 satelita najbliži Jupiteru, ima najjaču vulkansku
aktivnost u Sunčevu Sustavu, a stoga i vrlo mladu površinu (do 100 milijuna
godina). Europa je ledeni svijet, sa sivkastim prugama koje su nastale
usljed plimnih sila. Vrlo je vjerojatno da se ispod površine nalazi polutekući
(bljuzgavica) ocean, no nažalost vrlo duboko ispod ledene kore. Ganimed,
najveći satelit u Sunčevu sustavu, ima geološki raznoliku površinu sa
starijim tamnijim i novijim svijetlijim područjima. Ističe se područje
Regio Galileo promjera 4000 km.
Izvan putanje Kalista oko Jupitera kruži još
53 mala satelita s nepravilnim putanjama. Najbližih
7 satelita su u progradnim (direktnim) orbitama, dok se daljih
46 gibaju retrogradno.
Udar kometa Shoemaker-Levy 9 u Jupiter
Komet Shoemaker-Levy 9 su otkrili
Carolyn i Gene Shoemaker te David Levy na fotografiji snimljenoj
18. ožujka 1993. Komet je već tada bio u orbiti oko Jupitera s periodom
od oko 2 godine, rastrgnut (slika 10.) jupiterovim
plimnim silama. Raspad se vjerojatno dogodilo tokom prolaza perihelom
u srpnju 1992. godine. Dvadesetdva fragmenta su nazvana slovima A do W
(bez I i O). Vjeruje se da je komet prije prije otkrića bio o urbiti oko
Jupitera najmanje 20 godina. Ubrzo je postalo jasno da će komet udariti
u Jupiter (slika 11.) već za slijedećeg
perihela.
Prvi fragment (A) je pao na Jupiter 16. srpnja 1994,
a posljednji (Q) 6 dana kasnije. Svi su fragmenti pali na južnu
hemisferu, jednako udaljeni od ekvatora, ali na različite jovijanske širine
(zbog brze jupiterive rotacije). Fragmenti su dolazili pod kutom od 83°
u odnosu na Jupiterovu ekvatorsu ravninu (skoro direktno iz pravca juga),
a udarili su pod kutem od oko 45°. Zbog nepovoljnog
položaja mjesta udara (6.5° iza ruba) u odnosu na Zemlju, nije
se moglo direktno pratiti pad kometa. Jupiteru je trebalo oko 11
minuta da nam pokaže ožiljke od udara (slika
11. i 12.), ako ne računamo 48 minuta koliko je svjetlosti bilo
potrebno da stigne do Zemlje. Fotografije Galilea i HST-a
su potpomogle u praćenju ovog događaja.

Question: where is jupiter located in the solar system

Astronomical Division of the Physical Society of Split – Jupiter

where is jupiter located in the solar system

Question: what is the name of the planet jupiter

Question: what division of the physical society of Split is jupiter in

what division of the physical society of Split is jupiter in

Question: who is the astronomical division of jupiter

who is the astronomical division of jupiter

Question: in which european city is jupiter located

in which european city is jupiter located

Astronomical Division of the Physical Society of Split – Jupiter

Astronomska sekcija Fizikalnog društva Split – Jupiter

Astronomska sekcija Fizikalnog društva Split – Jupiter

Astronomical Division of the Physical Society of Split – Jupiter

Astronomical Division of the Physical Society of Split – Jupiter