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# How do I repair a scratched game disc?

I have kids, which means I have scratched game discs that my systems can't read.

Several months ago, I watched a video demonstrating how to repair scratched game discs using car polish. I tried that, and it didn't work. After a little more research, I found and purchased this plastic polishing kit from Amazon. Following the instructions (and using some ultra fine sandpaper to sand out the really bad scratches), I was able polish and sand out the scratches on one disc, while another remains unplayable, despite repeated repair attempts.

Using the plastic polishing kit requires a lot of time and effort. I'm lazy and want it to be easier and simpler.

Is this the best way to repair a disc? Are there any repair tools that are generally accepted, known, and proven to work? Do any game publishers support replacing damaged discs?

• I've had a lot of success by visiting game shops that do repairs. The one I go to uses a very interesting machine... but I don't actually know how it works. But, it was able to fix a critical scratch, so it was beyond worth it. – Grace Note Feb 8 '11 at 23:06
• It's not as well known, but some publishing companies will allow you to send the damaged disc to them and will send you another one out for a very small fee. Check the game's instruction manual for a telephone number and give it a try. – Andy E Feb 9 '11 at 10:04
• You get Steam :) – OddCore Jan 12 '12 at 11:45
• scratched game discs are just normal discs with data on them. Question off-topic here. I suggest moving this to superuser – DrFish Feb 17 '12 at 8:00
• your best bet is to bring it to a shop that has a disc resurfacing machine. there are many gimmicky machines out there, like the hand cranked ones you find at bestbuy or gamestop. those work for very mild scratches, but for a thorough resurfacing you need a place that has one of these: azuradisc.com/s.nl/it.A/id.2601/.f -- here's a video of it in action: youtube.com/watch?feature=player_embedded&v=OFDUydVq4Go – Patoshi パトシ Jul 15 '13 at 14:25

Go to your local game shop. That's usually the safest way to have a disc repaired, as they have a precision machine that can remove just enough of the plastic.

Otherwise, I've always used toothpaste and a glass cleaning cloth. If you take off too much of the plastic, you'll ruin the disk.

• I'll call around. I'm not too worried about taking off too much plastic: that's the problem, polishing doesn't take off enough. – splattered bits Feb 8 '11 at 23:15
• I've taken a few discs now with pretty good success. The game I originally tried to fix by hand still won't work, but I blame my polishing-by-hand. – splattered bits Nov 9 '11 at 11:50
• everytime i use toothpaste to repair my scratched disks, it will NEVER work. people say it does work but i never got it to work for me – user16597 Dec 17 '11 at 4:23
• I once repaired a disc with toothpaste. The cut was deep and short. By applying toothpaste, I was able to smooth the cut and the disc was readable again. – Vincent Robert Jul 9 '12 at 16:02

When a disc is scratched, the data usually isn't touched (if it gets down to the data layer, then that's a seriously deep gouge). Rather, what's happened is that the clear lacquer over the data layer has been scratched, and the scratch screws up the laser trying to read the data underneath.

The best way of repairing a scratched disk is to find a material with similar refractive index, and use that to fill in the scratch.

• Do you have any material suggestions? – splattered bits Feb 8 '11 at 23:16
• @splattered bits: The clear material is polycarbonate, which has a refractive index of ~1.585. Ideally you'd want something with the same RI that you can dissolve in a solvent, fill the scratch with, and then let the solvent evaporate. – Anon. Feb 8 '11 at 23:27
• Novus Fine Scratch Remover #2 – Mazura Apr 18 '15 at 3:10

I am a father, I have unreadable discs that cost between $30 and$60. I watched all the popular videos and this is what I found.

Discs are made of poly-carbonate layers with a reflective data layer sandwiched in between. When the plastic gets scratched it causes the laser to refract (bend) and hit the wrong section of data. This means the data is out of order and missing pieces for the player even though all the data is there in perfect condition (as long as the scratches don't reach that far. This would be obvious since that's a VERY deep scratch).

Toothpaste, petroleum jelly, car polishes, and even bananas are suggested to fill these scratches and stop the refraction but that rarely actually helps. Games that play after this were probably more dirty than scratched but even if the scratch was filled none of these are more than a very temporary fix since they aren't hard enough to permanently fill the scratch.

I am starting a conspiracy theory regarding the irresponsible use of toothpaste as either a plot by toothpaste manufacturers or perhaps an evil dentist union.

The only way to repair scratches is with a professional disc repair machine. Full disclosure I own and operate one of these as a mail in service. There are many such services but when I used a very popular one and it took 5 weeks to get my kid's games back I decided there was a market for another one.

Try local shops if they are close. Many play and trades will have a machine like this and will repair it on the spot for about $5. Full disclosure: I run one such place. • The toothpaste trick has it's roots in removing scratches from pieces of glass. Making the same thing work on discs is trickier, but uses the same principle (polishing the edges away so they won't be noticed that bad). Definitely no conspiracy here. – Mast Feb 4 '15 at 8:18 • I’ve tried that before with little success. It definitely depends on the disc, the nature of the scratch, the toothpaste, and the toothbrush/cloth/etc. However I have read enough vouches for it that it’s worth trying. – Synetech Dec 17 '11 at 20:25 I've seen folks have reasonable success with machines like Skip Doctor, which does the disc resurfacing for you. It's what I've seen them use at places like GameStop. Figure worst case scenario, the disc wasn't playable before and it ends up... still unplayable. • We've had luck using a similar device with Wii games that my neighbor's kids left out and got scratched up, and recovered some other CDs and DVDs (some computer software). It's so much easier than trying to hand polish, although I've only done the hand-polish thing on screens (cellphone, DS, etc.) – Joe Feb 9 '11 at 14:27 Okay, so I tried the hair conditioner and the toothpaste method neither worked for me, however, what did work was putting the disc in a sink full of lukewarm water and johnsons baby bath oil, and leaving it for about 10 seconds then using a soft face flannel to dry it, put it in the PS2 and voila! It worked :D I've heard that rubbing peanut oil on the disc is a good way to smooth out scratches. That said, I've never had occasion to try it and you'd want to be careful about gumming up your drive. • Actually, one time I had a CD that was kind of scratched and scuffed up and giving me trouble. After basically giving up on it, I—for whatever reason—rubbed it with an oily paper towel that had some kitchen grease (eg chicken/bacon/vegetable/etc.) on it. After then wiping it off with a bit of clean toilet paper, surprisingly, I found that the CD was suddenly readable! I’ve tried it again several times since then but have not had quite as much success as the first time. – Synetech Dec 17 '11 at 20:29 Some games manufacturers will replace damaged discs, however they charge a fee for this. For example, EA will replace games for between$13 and \$20. In the UK they charge £7.50 to £10.

Another option is insurance which is offered by some stores. For example, in the UK HMV will insure a game for one year for £1.

1. Get the disc that is broken then put it in your bathroom sink.
2. You'll need to get some alcohol and a glass cleaning rag.
3. Pour some alcohol on the disc(make sure you have enough to cover up the disc, and block the drain in the sink)
4. Put some water in the alcohol.
5. Let it soak for about 15 mins.
6. Let dry for 10 mins. Then wipe off excess with glass cleaning rag. And you are done. Plus if you want the lasers to work better you can gently wipe the cd off with a clorox cleaning wipe.

This always did wonders for my disks: http://howtofixstuff.blogspot.com/2012/01/how-to-fix-scratched-cd.html, especially the shoe polish.

Repair Using A Banana

• Open up a banana and apply it to the disk.
• Wipe the excess banana pieces down with the banana peel. The wax from the peel will help polish and further clean the disk.
• Take a clean cotton cloth and wipe the entire surface of the disk. Be sure to apply moderate pressure while moving in a circular motion. This should be done for around 5 minutes.
• Spray the disc with glass cleaner and wipe it clean.

Repair using Toothpaste

• Clean the disc with a mild soap and warm water. This will remove any oils and finger marks.
• Dry the disc with a lint-free cloth.
• Apply the toothpaste on the disk.
• Rub the toothpaste on the disc in a straight motion (not in a circular motion) from the center to the outer edges.
• Let it sit for 2-3 minutes.
• Remove the toothpaste and dry the disk. Make sure to dry with care so not to scratch the disk further.

You can also try furniture polish.such as Pledge on a soft cloth and buff till dry & shiney. The wax in the polish fills in the scratches so the laser on your dvd player will glide right over them.

If all else fails, you can go to your local video store and for 5 bucks they will fix it for you.

• Could you elaborate on the content of that article? – fredley Jan 12 '12 at 15:03

Rub the disc that will not read with brasso vigorously for about 1 minute then wipe with polishing cloth (yellow duster) with small amount of spit (or water if this disturbs you) then use the toothpaste method, then repeat the brasso for best results. Now install the game (if possible) this should work 9 times out of 10.

I had been using toothpaste, but it made my CD even worse so I thought vaseline (petroleum jelly) might work. Well it didn't - so I put water and dishwashing detergent in a container, put in the cd and left it for about 15 minutes.

Afterwards I rinsed the cd with warm water and dried it with paper towels. Then I put it in the Wii console and finally it was working!

Hope it helps!

• This answer adds nothing that has not already been said or discussed. So I have to downvote and report it as being a bad subjective answer. – Ramhound Jul 9 '12 at 16:03
• @Ramhound bad subjective, just because it repeats? I don't think that is entirely the right way to go about that. – Ash Jul 10 '12 at 3:52
• @Ramhound You should never feel obligated to downvote and flag a post. A downvote is sufficient if you feel it's not a great post, but it's not a rule that you have to do so, and it's certainly not a rule that you have to flag things because they've been said in some form already. – GnomeSlice Jul 10 '12 at 3:53

Hair conditioner. I used "Head and Shoulders", but can't speak for other brands. It only works temporarily. Apply the conditioner by starting from the center of the disc and rubbing towards the outside in a straight line.

It doesn't totally remove the scratches; some scratching will still be visible. Still, it will play well for a few days and it is an easy at-home fix.

## protected by badpAug 1 '13 at 11:26

Thank you for your interest in this question. Because it has attracted low-quality or spam answers that had to be removed, posting an answer now requires 10 reputation on this site (the association bonus does not count).


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# what chloride salts are not soluble?

The solubility of salts depends on the types of interactions they can have with water molecules. Here, the dissolution of the salt forms ionic species in water, which makes the newly formed aqueous solution highly conductive. Most of the precipitation reactions that we will deal with involve aqueous salt solutions. read more. 1 decade ago. 3. In addition to the above, the water molecules can form intermolecular attractions with the ions of soluble salts, but there are no intermolecular interactions between insoluble salts and water. An example of a soluble salt is table salt or sodium chloride. KCl. 1. 2. Compare the Difference Between Similar Terms. ... Salt (sodium chloride) is made from positive sodium ions bonded to negative chloride ions. SOLUBILITY RULES. 6 Answers. The key difference between soluble and insoluble … Drug Names and Their Pharmaceutical Salts - Clearing Up the Confusion. Note concerning #7 just above: Some older sources might include ammonium hydroxide (NH 4 OH) as a soluble hydroxide. We can divide salt compounds into two types depending on their water solubility. Reactions of chloride. They are soluble and insoluble salts. The sulfate (SO 4 2-) ion generally forms soluble salts. Source: middleschoolchemistry.com. Chloride ions can destabilize passive surface oxide films; however, the fluxing action is not as severe as fluoride salts. However, some combinations will not produce such a product. Therefore, a salt essentially contains an anion (comes from the acid) and a cation (comes from the base). Most chlorides (Cl- ), and sulfates (SO42-) are soluble. Define sparingly soluble salts Solubility product (K sp ) When a sparingly soluble salt is placed in water, a very small amount of the salt dissolves in the water and a solution is formed. Anonymous. Plain old table salt or sea salt (sodium chloride). Although soluble salts may inhibit plant growth, these effects can be controlled through proper monitoring of the greenhouse. In contrast, insoluble salts are nonpolar. This complete equation may be rewritten in ionic form by using the solubility rules. How insoluble salts are prepared? The method of preparing and purifying the salt depends on whether or not it is soluble in water. If solutions of sodium nitrate and ammonium chloride are mixed, no reaction occurs. Sodium chloride, for example, has a solubility of 357 g/L at 0°C, which corresponds to a chloride ion concentration of 220,000 ppm. Examples Of Soluble Salts. Water … Some chlorides, e.g., antimony chloride and bismuth chloride, decompose in water, forming oxychlorides. Quoting from a previously published article, “Five Key Factors in Understanding the Role of Soluble Salts in Coatings Failures, "the chloride ion is more corrosion-inducing than the sulfate, for example: Knowing what anionic species is present and its concentration (amount) is important and directly related to the outcome of the coating performance." leadchloride is sparingly soluble or insoluble in cold water but soluble in warm water. All compounds containing Na+, K+, or NH4+ ions are soluble in water. This energy will be supplied by the formation of hydrogen bonds with water molecules. A good example of an insoluble salt is silver chloride (AgCl). 4. Most metal chloride salts are soluble in water 1 3 meaning they dissolve and do from CHEM 106.LB at Hunter College, CUNY “Insoluble Salts.” Salts-Tripod, Available here. “Definition of Insoluble Salts (Precipitates).” Cehmicool Dictionary, Available here. You’ve given the pharmacist a prescription for your new diabetes medication called metformin hydrochloride, but when you receive your bottle and look it up on the internet, all you see is “metformin”, not “ Is lead chloride (PbCl₂) soluble in water? Salts are composed of related numbers of cations (positively charged ions) and anions (negatively charged ions) so that the product is electrically neutral (without a net charge). The key difference between soluble and insoluble salts is that soluble salts can dissolve in water at room temperature, whereas insoluble salts cannot dissolve in water at room temperature. Washing soda (sodium carbonate) is another, as is sodium bicarbonate (baking soda). 5. Lead sulfate is insoluble in cold water whereas most of the sulfates are soluble in cold water. Hard-hard and soft-soft interactions tend to be favorable; mixed interactions are not as favorable. 1. Sodium chloride is an ionic compound. Silver acetate is sparingly soluble. HgI2 is insoluble in water. Anonymous. You have to use crown ether to make inorganic salts soluble in organic solvents i.e.Use phase transfer catalyst like Benzo-18-crown 6 or Benzo-15-crown-5. Like other barium salts, it is toxic and imparts a … Therefore, there are no intermolecular interactions between water molecules and insoluble salt compounds. Summary. We can divide salt compounds into two types depending on their water solubility. Chloride can be oxidized but not reduced. Actually it isn't really magic at all, although it is still cool. These salt compounds dissolve in water because they can form intermolecular attractions with water molecules. Because NaCl is an ionic substance, while paraffin is not (non-polar). A… The chloride ion / ˈ k l ɔːr aɪ d / is the anion (negatively charged ion) Cl −.It is formed when the element chlorine (a halogen) gains an electron or when a compound such as hydrogen chloride is dissolved in water or other polar solvents. Soluble salts can be made by reacting acids with soluble or insoluble reactants. Unlike soluble salts, mixing insoluble salts with water does not make water conductive. Example: AgNO3 + NaCl = AgCl + NaNO3 Silver chloride is an insoluble, white salt. The chloride salts most frequently found on buildings and monuments are listed. Cool, it's magic! On the atomic scale, the ionic lattice of an insoluble salt remains intact; the ionic lattice does not break up to allow the salt ions to be surrounded by water molecules and so form a solution. recall the general rules for predicting the solubility of salts in water: i all common Sodium, Potassium and Ammonium salts are soluble. 1. We can divide salt compounds into two types depending on their water solubility. Hydroxide salts of Group II elements (Ca, Sr, and Ba) are slightly soluble. 0 0. all chloride and nitrate salt also soluble. chloride salts are usually soluble, but with silver it is not soluble. iii common Chlorides are soluble, except Silver Chloride. What are Insoluble Salts Question: Is NaCl ( sodium chloride ) Soluble or Insoluble in water ? not all salts are soluble in water!! Most chlorides are soluble in water, except mercurous and silver chlorides. Why is salt - NaCl - soluble in distilled water, but not paraffin oil? The problem with the reaction of a soluble base reaction with acid is that once all the acid has reacted any excess base will not … Sodium chloride is a soluble salt. N.B. Aim: To prepare a pure sample of copper(II) nitrate by mixing an acid with a metal oxide. Insoluble salts are salt compounds that are insoluble in water at room temperature. If solutions of sodium nitrate and ammonium chloride are mixed, no reaction occurs. 0 0. Cu(NO₃)₂. In aqueous solution, chloride is bound by the protic end of the water molecules. 1. Potassium Hydroxide- Soluble in water, group 1 metal salts are soluble. Soluble salt limits. The method of preparing and purifying the salt depends on whether or not it is soluble in water. She knew exactly what two colorless solutions to mix together to produce a yellow solid. Sodium Chloride - Soluble in water, group 1 metal salts are soluble. 1 decade ago . Furthermore, the dissolution of soluble salts in water makes a highly conductive aqueous solution because the ions dissolved in water can conduct electricity through it. In chemistry, a salt is a chemical compound consisting of an ionic assembly of cations and anions. What are Soluble Salts Some important exceptions are silver chloride (AgCl), barium sulfate (BaSO4), and lead sulfate (PbSO4) which are insoluble. The general table salt: sodium chloride, and potassium chlorideothers include Ammonium nitrate and calcium nitrate. It is one of the most common water-soluble salts of barium. Since salts are ionic compounds, they dissolve in water because water molecules tend to attract the ions in the compound, which makes them separate from each other, resulting in the dissolution of the salt. Exceptions to this rule include salts of the Pb 2+, Hg 2 2+, Ag +, and Cu + ions. They are soluble and insoluble salts. Most common chloride salts are soluble in water except silver chloride (AgCl), lead (II) chloride (PbCl2). “Insoluble Salts.” Chemistry LibreTexts, Libretexts, 5 June 2019, Available here. chloride Salt of hydrochloric acid or some organic compounds containing chlorine, especially those with the negative ion Cl −.The best-known example is common salt, sodium chloride (NaCl). NaCl, K 2 SO 4, NH 4 NO 3; All nitrate salts are soluble e.g. Performance & security by Cloudflare, Please complete the security check to access. Similarly, when a salt like sodium chloride dissolves in water, the sodium and chloride ions are released, and they will interact with polar water molecules. NH₄Cl. ZnCl 2 is soluble, but CuBr is not. My question: Medically reviewed by Leigh Ann Anderson, PharmD.Last updated on Apr 10, 2020. 2. 0 0. Soluble (all potassium salts are soluble in water) Is calcium hydroxide (Ca(OH)₂) soluble in water? Anonymous. Side by Side Comparison – Soluble vs Insoluble Salts in Tabular Form Sodium Chloride - Soluble in water, group 1 metal salts are soluble. Exceptions to this rule include salts of the Pb 2+, Hg 2 2+, Ag +, and Cu + ions. Favorite Answer. Cite 1st Feb, 2018 SOLUBILITY RULES. Hydroxide salts of Group I elements are soluble. In contrast, insoluble salts are nonpolar. Furthermore, insoluble salts are nonpolar compounds. Ammonium Chloride -Soluble in water, Ammonium salts are soluble. Most common sulfate salts are soluble in water e xcept, lead (II) sulfate (PbSO4), barium sulfate (BaSO4) and calcium sulfate (CaSO4). One could write a molecular equation showing a double-replacement reaction, but both products, sodium chloride and ammonium nitrate, are soluble and would remain in the solution as ions. The key difference between soluble and insoluble salts is that soluble salts can dissolve in water at room temperature, whereas insoluble salts cannot dissolve in water at room temperature. Bond breakages need energy. PbCl2, PbBr2, and PbI2 The chloride (Cl-), bromide (Br-), and iodide (I-) ions generally form soluble salts. Water molecules are polar. Here is What I know: Gold(III) chloride is Highly Hygroscopic [1] and is highly soluble in water, I don't know which salts are not soluble never researched it, maybe Gold-Mercury amalgam is not soluble in water but its not a salt.. [1] = absorbing or attracting moisture from the air. Completing the CAPTCHA proves you are a human and gives you temporary access to the web property. Sulfur sources such as Na 2 S, thioacetamide, and thiourea are usually preferred. Overview and Key Difference 3. Slightly soluble . Moreover, soluble salts are polar; that’s why they can dissolve in water, which is a polar solvent. Sulfur sources such as Na 2 S, thioacetamide, and thiourea are usually preferred. Chloride salts such as sodium chloride are often very soluble in water. You see, Shelley understands all about the solubility of common salts. 1 decade ago. chloride Salt of hydrochloric acid or some organic compounds containing chlorine, especially those with the negative ion Cl −.The best-known example is common salt, sodium chloride (NaCl). No, the correct way of putting it is $$\mathrm{Almost~all~of~the~\mathbf{inorganic}~nitrate~salts~are~soluble~in~water. Soluble compounds are defined as those that dissolve to the extent of 1 g or more per 100 g water. It is one of the most common water-soluble salts of barium. They provide a ready source of fluoride ions. Another way to prevent getting this page in the future is to use Privacy Pass. Although soluble salts may inhibit plant growth, these effects can be controlled through proper monitoring of the greenhouse. If you are on a personal connection, like at home, you can run an anti-virus scan on your device to make sure it is not infected with malware. • Difference Between Slaked Lime and Lime Water, Difference Between Silica and Silicon Dioxide, Side by Side Comparison – Soluble vs Insoluble Salts in Tabular Form, Difference Between Coronavirus and Cold Symptoms, Difference Between Coronavirus and Influenza, Difference Between Coronavirus and Covid 19, Difference Between Ionization and Dissociation, Difference Between Gravimetric and Titrimetric Analysis, Difference Between Orthoboric Acid and Metaboric Acid, Difference Between Regeneration and Fibrosis, Difference Between Culture and Media in Microbiology, Difference Between Oxirane Glycidyl and Epoxy Groups, Difference Between Filgrastim and Lenograstim. Terms of Use and Privacy Policy: Legal. Calcium Carbonate- Insoluble, All carbonates are insoluble. Copper Nitrate - Soluble in water, nitrate salts are soluble. Sodium chloride and sodium bromide being less soluble in acetone get precipitated from the solution and can be removed by filtration. Insoluble salts are ionic compounds that are insoluble in water: the salt continues to exist as a solid rather than dissolving in the liquid. iv common Sulphates are soluble, except those of Barium and Calcium. Pb(II)Cl i.e. 4 years ago. Moreover, soluble salts are polar; that’s why they can dissolve in water, which is a polar solvent. Ariel Kenneth. There are many many soluble salts. The nitrates, chlorates, and acetates of all metals are soluble in water. Soluble (all sodium salts are soluble in water) The first oxidation, as employed in the chlor-alkali process, is conversion to … Lv 5. One could write a molecular equation showing a double-replacement reaction, but both products, sodium chloride and ammonium nitrate, are soluble and would remain in the solution as ions. NaCl = sodium chloride. You may need to download version 2.0 now from the Chrome Web Store. They are soluble and insoluble salts. How come salt (sodium chloride) is soluble in water? ii all Nitrates are soluble. The salts made in neutralisation reactions can be either soluble or insoluble. This substance does not exist; it cannot be isolated as a pure substance. An aqueous solution of table salt contains sodium ions and chloride ions. Insoluble (one of the few exceptions, most chloride salts are soluble) Is sodium carbonate (Na₂CO₃) soluble in water? Unlike soluble salts, the mixing of insoluble salts with water does not make the solution conductive because the salt does not separate into ions. The chloride (Cl-), bromide (Br-), and iodide (I-) ions generally form soluble salts. There are many many soluble salts. Soluble salt accumulations often result from the use of poor-quality irrigation water, overfertilization, or growing in a medium with a naturally high salt content. They are soluble and insoluble salts. Lead chloride is also insoluble in cold water but is soluble in hot water. In water, it breaks into Na+ ions and Cl- … If you are at an office or shared network, you can ask the network administrator to run a scan across the network looking for misconfigured or infected devices. @media (max-width: 1171px) { .sidead300 { margin-left: -20px; } } Cloudflare Ray ID: 6102d06ae96ee502 Unlike soluble salts, mixing insoluble salts with water does not make water conductive. Barium chloride is the inorganic compound with the formula BaCl2. Your IP: 64.34.219.21 4 years ago. Why? Every ion is a spectator ion and there is not net ionic equation at all. 4. Therefore, water is a polar solvent, and polar salts can dissolve in water. Because of this process, sugar is well soluble in water. First of all, depends which reaction you would like to do. 3. all chloride and nitrate salt also soluble. NaNO 3, Mg(NO 3) 2, Al(NO 3) 3, NH 4 NO 3; Some ethanoate salts are soluble e.g. • 3. The key difference between soluble and insoluble salts is that the soluble salts can dissolve in water at room temperature, whereas the insoluble salts cannot dissolve in water at room temperature. 3. Water is a hard solvent. Rule 2 confirms that lead(II) nitrate is soluble and therefore dissociated. The method of preparing and purifying the salt depends on whether or not it is soluble in water. Explanation: Ksp for AgCl is 1.8 × 10−10, for P bCl2, 5.9× 10−5, for H g2Cl2, 1.3 ×10−18. Thus, Cu(NO 3) 2 and Fe(NO 3) 3 are soluble. Relevance. Let me introduce you to Shelley. 0 0. }$$ The families of organic nitrate salts are typically nitrates of azoles and imidazoles. Anonymous. Examples Of Soluble Salts. Solubility Solubility is the property of a solid, liquid, or gaseous chemical substance called solute to dissolve in a solid, liquid, or gaseous solvent. CH 3 COONa; Common chloride salts are soluble except those of silver and lead e.g. KOH. Preparing Soluble Salts Experiment 2. 2. Lead ion is a borderline acid in the context of hard-soft acid-base theory. Thus, Fe(OH) 3, Al(OH) 3, Co(OH) 2 are not soluble. Salts are composed of related numbers of cations (positively charged ions) and anions (negatively charged ions) so that the product is electrically neutral (without a net charge). (2) Preparation of sodium chloride : Experimental sheet for the preparation of sodium chloride. Figure 02: Silver Chloride Precipitate in Water. (adsbygoogle = window.adsbygoogle || []).push({}); Copyright © 2010-2018 Difference Between. Source(s): https://shrinkurl.im/a9Yqn. “Sodium chloride” By Chemicalinterest – Own work (Public Domain) via Commons Wikimedia A precipitate is an insoluble solid salt separating from the solution. Most chloride salts are readily soluble in water, but mercurous chloride (calomel) and silver chloride are insoluble, and lead chloride is only slightly soluble. General rules which describe the solubility of common types of compounds in water: All common sodium, potassium and ammonium salts are soluble e.g. As products, sodium nitrate is predicted to be soluble (rules 1 and 2) and will be dissociated. The salts made in neutralisation reactions can be either soluble or insoluble. It is also hygroscopic. Washing soda (sodium carbonate) is another, as is sodium bicarbonate (baking soda). ZnCl 2 is soluble, but CuBr is not. 4. All rights reserved. You have also learned that not all salts are soluble. The chlorides, bromides, and iodides of all metals except lead, silver, and mercury(I) are soluble in water. These are insoluble in water because water molecules cannot attract the ions in the salt compound. Your cytidine.HCl salt is of course not soluble in dry organic solvent and your reaction would not work well. It is best prepared by a titration method using a neutralisation reaction between an acid and an alkali. 4. Thus, Cu(NO 3) 2 and Fe(NO 3) 3 are soluble. Silver chloride, on the other hand, is one of the few chloride salts that have low solubility: 0.89 mg/L at 10°C, or 0.22 ppm chloride ion concentration. In chemistry, a salt is a chemical compound consisting of an ionic assembly of cations and anions. 0 0. : This method of preparation is used when any and all sodium or potassium salts are made.. Not only that, but she also knew just what was going on in the reaction. In synthesis, water-soluble salts such as perchlorate and chloride are generally used as metal initiators. 2. Chloride salts include sodium chloride (common salt), potassium chloride, calcium chloride, and ammonium chloride. Answer Save. However, some combinations will not produce such a product. Hygroscopic means water absorption. Shelley is a really ace chemist; she can mix two colorless solutions and produce a bright yellow solid. With a mind rooted firmly to basic principals of chemistry and passion for ever evolving field of industrial chemistry, she is keenly interested to be a true companion for those who seek knowledge in the subject of chemistry. Most chloride salts are readily soluble in water, but mercurous chloride (calomel) and silver chloride are insoluble, and lead chloride is only slightly soluble. Anonymous. Most of the precipitation reactions that we will deal with involve aqueous salt solutions. If solutions of sodium nitrate and ammonium chloride are mixed, no reaction occurs. Cuprous chloride is also reasonably insoluble, Ksp = 1.72× 10−7, but it does not generally appear on the standard tables of solubility. 0 0. All sodium, potassium and ammonium salts are soluble. (INSOLUBLE IN WATER) EngMary; Aug 27, 2016 at 4:18am. Table 1. Rule 1 says the same about NaCl. 0 0. Sodium chloride is an example of soluble salts, whereas silver chloride is an example for insoluble salt. So, this is another significant difference between soluble and insoluble salts. NaCl . Slightly soluble (one of the few exceptions, most chlorides are soluble) Is lead sulfate (PbSO₄) soluble in water? Summary – Soluble vs Insoluble Salts. Hydroxide salts of transition metals and Al 3 + are insoluble. 2. Answer: NaCl ( sodium chloride ) is Soluble in water What is Soluble and Insoluble ? The lead(II) chloride, however, is insoluble (rule 3). Insoluble salts are the products of some chemical reactions. Insoluble salts are made by precipitation reactions. Like other barium salts, it is toxic and imparts a yellow-green coloration to a flame. Plain old table salt or sea salt (sodium chloride). This also prevents the backward reaction to occur according to Le Chatelier's principle. Insoluble salts are ionic compounds that are insoluble in water: the salt continues to exist as a solid rather than dissolving in the liquid. These component ions can be inorganic, such as chloride (Cl −), or organic, such as acetate (CH “Silver chloride (AgCl)” By Luisbrudna – Own work (CC BY-SA 4.0) via Commons Wikimedia. Most chlorides are soluble in water, except mercurous and silver chlorides. When ammonia gas (NH 3) is bubbled through water, it dissolves and a small number of ammonia molecules react with the water to produce NH 4 + and OH¯ ions. The sulfate (SO 4 2-) ion generally forms soluble salts. All nitrates (NO3-) are soluble in water. Titration must be used if the reactants are soluble. 3. CaCO₃ . All sodium, potassium, and ammonium salts are soluble in water. Madhu is a graduate in Biological Sciences with BSc (Honours) Degree and currently persuing a Masters Degree in Industrial and Environmental Chemistry. Please enable Cookies and reload the page. However, most of the NH 3 molecules remain as … 0 0. Most hydroxide salts are only slightly soluble. Figure 01: Sodium Chloride is a Soluble Salt. Barium chloride is the inorganic compound with the formula BaCl2. The salts made in neutralisation reactions can be either soluble or insoluble. Source(s): https://shrinkurl.im/a9Yqn. Answer link. We can divide salt compounds into two types depending on their water solubility at room temperature. Domain ) via Commons Wikimedia 2 warm water an aqueous solution highly conductive in warm water perchlorate chloride. Also knew just what was going on in the future is to use crown ether to inorganic. As favorable ionic form by using the solubility rules: i all common sodium potassium! Typically nitrates of azoles and imidazoles as favorable perchlorate and chloride are generally as... = AgCl + NaNO3 silver chloride ( Cl- ), bromide ( Br-,... Of preparation is used when any and all sodium or potassium salts are soluble e.g \mathrm. 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I- ) ions generally form soluble salts, it is still cool ammonium and! ( Herz salts ) gives benzo-1,2,3-thiaselenazolium salts, mixing insoluble salts are soluble of the most water-soluble... Conversion to … not all salts are soluble in water at room temperature unlike soluble salts, which is borderline... That not all salts are soluble... salt ( sodium carbonate ) is in... Copper ( II ) chloride, and acetates of all, depends which reaction you like. By Luisbrudna – Own work ( CC BY-SA 4.0 ) via Commons Wikimedia 2 Luisbrudna – Own work Public! Sodium chloride is an ionic assembly of cations and anions may be rewritten in ionic form using... Distilled water, which is a polar solvent course not soluble in water can conduct electricity it.: sodium chloride ) is soluble in water Salts. ” chemistry LibreTexts, 5 2019... Leigh Ann Anderson, PharmD.Last updated on Apr 10, 2020 combinations will not produce such a product process! 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• ### Giant planets around FGK stars form probably through core accretion(1805.02721)

May 7, 2018 astro-ph.EP
We present a statistical study of the planet-metallicity (P-M) correlation, by comparing the 744 stars with candidate planets (SWPs) in the Kepler field which have been observed with LAMOST, and a sample of distance-independent, fake "twin" stars in the Kepler field with no planet reported (CKSNPs) yet. With the well-defined and carefully-selected large samples, we find for the first time a turn-off P-M correlation of Delta [Fe/H]_(SWPs-SNPs), which in average increases from ~0.00+-0.03 dex to 0.06+-0.03 dex, and to 0.12+-0.03 for stars with Earth, Neptune, Jupiter-sized planets successively, and then declines to ~-0.01+-0.03 dex for more massive planets or brown dwarfs. Moreover, the percentage of those systems with positive Delta[Fe/H] has the same turn-off pattern. We also find FG-type stars follow this general trend, but K-type stars are different. Moderate metal enhancement (~0.1-0.2 dex) for K-type stars with planets of radii between 2 to 4 Earth radius as compared to CKSNPs is observed, which indicates much higher metallicities are required for Super-Earths, Neptune-sized planets to form around K-type stars. We point out that the P-M correlation is actually metallicity-dependent, i.e., the correlation is positive at solar and super-solar metallicities, and negative at subsolar metallicities. No steady increase of Delta[Fe/H] against planet sizes is observed for rocky planets, excluding the pollution scenario as a major mechanism for the P-M correlation. All these clues suggest that giant planets probably form differently from rocky planets or more massive planets/brown dwarfs, and the core-accretion scenario is highly favoured, and high metallicity is a prerequisite for massive planets to form.
• ### Broadband calibration-free cavity-enhanced complex refractive index spectroscopy using a frequency comb(1805.00799)

May 2, 2018 physics.optics
We present broadband cavity-enhanced complex refractive index spectroscopy (CE-CRIS), a technique for calibration-free determination of the complex refractive index of entire molecular bands via direct measurement of transmission modes of a Fabry-Perot cavity filled with the sample. The measurement of the cavity transmission spectrum is done using an optical frequency comb and a mechanical Fourier transform spectrometer with sub-nominal resolution. Molecular absorption and dispersion spectra (corresponding to the imaginary and real parts of the refractive index) are obtained from the cavity mode broadening and shift retrieved from fits of Lorentzian profiles to the individual cavity modes. This method is calibration-free because the mode broadening and shift are independent of the cavity parameters such as the length and mirror reflectivity. In this first demonstration of broadband CE-CRIS we measure simultaneously the absorption and dispersion spectra of three combination bands of CO2 in the range between 1525 nm and 1620 nm and achieve good agreement with theoretical models. This opens up for precision spectroscopy of the complex refractive index of several molecular bands simultaneously.
• ### Two new Super Li-rich core He-burning giants: A new twist to the long tale of Li enhancement in K giants(1804.10955)

April 29, 2018 astro-ph.SR
In this paper we report two new super Li-rich K giants: KIC 2305930 and KIC 12645107 with Li abundances exceeding that of ISM (A(Li) $\geq$ 3.2 dex). Importantly, both the giants have been classified as core He-burning red clump stars based on asteroseismic data from Kepler mission. Also, both the stars are found to be low mass (M $\approx$ 1.0 M$_{\odot}$) which, together with an evidence of their evolutionary status of being red clump imply that the stars have gone through both the luminosity bump and He-flash during their RGB evolution. Stars' large Li abundance and evolutionary phase suggest that Li enrichment occurred very recently probably at the tip of RGB either during He-flash, an immediate preceding event on RGB, or by some kind of external event such as merger of RGB star with white dwarf. The findings will provide critical constraints to theoretical models for understanding of Li enhancement origin in RGB stars.
• ### Carbon stars identified from LAMOST DR4 using Machine Learning(1712.07784)

Jan. 31, 2018 astro-ph.SR
In this work, we present a catalog of 2651 carbon stars from the fourth Data Release (DR4) of the Large Sky Area Multi-Object Fiber Spectroscopy Telescope (LAMOST). Using an efficient machine-learning algorithm, we find out these stars from more than seven million spectra. As a by-product, 17 carbon-enhanced metal-poor (CEMP) turnoff star candidates are also reported in this paper, and they are preliminarily identified by their atmospheric parameters. Except for 176 stars that could not be given spectral types, we classify the other 2475 carbon stars into five subtypes including 864 C-H, 226 C-R, 400 C-J, 266 C-N, and 719 barium stars based on a series of spectral features. Furthermore, we divide the C-J stars into three subtypes of CJ( H), C-J(R), C-J(N), and about 90% of them are cool N-type stars as expected from previous literature. Beside spectroscopic classification, we also match these carbon stars to multiple broadband photometries. Using ultraviolet photometry data, we find that 25 carbon stars have FUV detections and they are likely to be in binary systems with compact white dwarf companions.
• ### The odd-isotope fractions of Barium in the strongly r-process enhanced (r-II) stars(1801.07919)

Jan. 24, 2018 astro-ph.SR
We determined the \fodd\ values, $0.46\pm0.08$, $0.51\pm0.09$, $0.50\pm0.13$, $0.48\pm0.12$, which correspond to the r-contribution 100\% for four r-II stars, \cs, \hen, \hes\, and \het, respectively. Our results suggest that almost all of the heavy elements (in the range from Ba to Pb) in r-II stars have a common origin, that is, from a single r-process (the main r-process). We found that the \fodd\ has a intrinsic nature, and should keep constant value of about 0.46 in the main r-process yields, which is responsible for the heavy element enhancement of r-II stars and of our Galaxy chemical enhancement. In addition, except the abundance ratio [Ba/Eu] the \fodd\ is also an important indicator, which can be used to study the relative contributions of the r- and s-process during the chemical evolution history of the Milky Way and the enhancement mechanism in stars with peculiar abundance of heavy elements.
• ### Stellar activity with LAMOST - II. Chromospheric activity in open clusters(1801.07410)

Jan. 23, 2018 astro-ph.SR
We use the LAMOST spectra of member stars in Pleiades, M34, Praesepe, and Hyades to study how chromospheric activity vary as a function of mass and rotation at different age. We measured excess equivalent widths of H$\alpha$, H$\beta$, and Ca~{\sc ii} K based on estimated chromospheric contributions from old and inactive field dwarfs, and excess luminosities are obtained by normalizing bolometric luminosity, for more than 700 late-type stars in these open clusters. Results indicate two activity sequences in cool spot coverage and H$\alpha$ excess emission among GK dwarfs in Pleiades and M dwarfs in Praesepe and Hyades, paralleling with well known rotation sequences. A weak dependence of chromospheric emission on rotation exists among ultra fast rotators in saturated regime with Rossby number Ro$\lesssim0.1$. In the unsaturated regime, chromospheric and coronal emission show similar dependence on Ro, but with a shift toward larger Ro, indicating chromospheric emission gets easily saturated than coronal emission, and/or convective turnover time-scales based on X-ray data do not work well with chromospheric emission. More interestingly, our analysis show fully convective slow rotators obey the rotation-chromospheric activity relation similar to hotter stars, confirming the previous finding. We found correlations among H$\alpha$, H$\beta$, and Ca~{\sc ii} K emissions, in which H$\alpha$ losses are more important than Ca~{\sc ii} K for cooler and more active stars. In addition, a weak correlation is seen between chromospheric emission and photospheric activity that shows dependency on stellar spectral type and activity level, which provides some clues on how spot configuration vary as a function of mass and activity level.
• ### Enormous Li-enhancement preceding red giant phases in low-mass stars in the Milky Way halo(1801.00090)

Dec. 30, 2017 astro-ph.SR
Li abundances in the bulk of low-mass metal-poor stars are well reproduced by stellar evolution models adopting a constant initial abundance. However, a small number of stars have exceptionally high Li abundances, for which no convincing models have been established. We report on the discovery of 12 very metal-poor stars that have large excesses of Li, including an object having more than 100 times higher Li abundance than the values found in usual objects, which is the the largest excess in metal-poor stars known to date. The sample is distributed over a wide range of evolutionary stages, including five unevolved stars, showing no abundance anomaly in other elements. The results indicate the existence of an efficient process to enrich Li in a small fraction of low-mass stars at the main-sequence or subgiant phase. The wide distribution of Li-rich stars along the red giant branch could be explained by dilution of surface Li by mixing that occurs when the stars evolve into red giants. Our study narrows down the problem to be solved to understand the origins of Li-excess found in low-mass stars, suggesting the presence of unknown process that affects the surface abundances preceding red giant phases.
• ### Stellar Stream Candidates in the Solar Neighborhood Found in the LAMOST DR3 and TGAS(1708.01695)

Aug. 5, 2017 astro-ph.GA
We have cross-matched the LAMOST DR3 with the Gaia DR1 TGAS catalogs and obtained a sample of 166,827 stars with reliable kinematics. A technique based on the wavelet transform was applied to detect significant overdensities in velocity space among five subsamples divided by spatial position. In total, 16 significant overdensities of stars with very similar kinematics were identified. Among these, four are new stream candidates and the rest are previously known groups. Both the U-V velocity and metallicity distributions of the local sample show a clear gap between the Hercules structure and the Hyades-Pleiades structure. The U-V positions of these peaks shift with the spatial position. Following a description of our analysis, we speculate on possible origins of our stream candidates.
• ### Sensitive and broadband measurement of dispersion in a cavity using a Fourier transform spectrometer with kHz resolution(1705.04729)

Optical cavities provide high sensitivity to dispersion since their resonance frequencies depend on the index of refraction. We present a direct, broadband, and accurate measurement of the modes of a high finesse cavity using an optical frequency comb and a mechanical Fourier transform spectrometer with a kHz-level resolution. We characterize 16000 cavity modes spanning 16 THz of bandwidth in terms of center frequency, linewidth, and amplitude. We retrieve the group delay dispersion of the cavity mirror coatings and pure N${_2}$ with 0.1 fs${^2}$ precision and 1 fs${^2}$ accuracy, as well as the refractivity of the 3{\nu}1+{\nu}3 absorption band of CO${_2}$ with 5 x 10${^{-12}}$ precision. This opens up for broadband refractive index metrology and calibration-free spectroscopy of entire molecular bands.
• ### Chemical Composition of Young Stars in the Leading Arm of the Magellanic System(1701.00590)

Jan. 3, 2017 astro-ph.GA, astro-ph.SR
Chemical abundances of eight O- and B-type stars are determined from high-resolution spectra obtained with the MIKE instrument on the Magellan 6.5m Clay telescope. The sample is selected from 42 candidates of membership in the Leading Arm of the Magellanic System. Stellar parameters are measured by two independent grids of model atmospheres and analysis procedures, confirming the consistency of the stellar parameter results. Abundances of seven elements (He, C, N, O, Mg, Si, and S) are determined for the stars, as are their radial velocities and estimates of distances and ages. Among the seven B-type stars analyzed, the five that have radial velocities compatible with membership to the LA have an average [Mg/H] of $-0.42\pm0.16$, significantly lower than the average of the remaining two [Mg/H] = $-0.07\pm0.06$ that are kinematical members of the Galactic disk. Among the five LA members, four have individual [Mg/H] abundance compatible with that in the LMC. Within errors, we can not exclude the possibility that one of these stars has a [Mg/H] consistent with the more metal-poor, SMC-like material. The remaining fifth star has a [Mg/H] close to MW values. Distances to the LA members indicate that they are at the edge of the Galactic disk, while ages are of the order of $\sim 50-70$ Myr, lower than the dynamical age of the LA, suggesting a single star-forming episode in the LA. V$_{\rm LSR}$ the LA members decreases with decreasing Magellanic longitude, confirming the results of previous LA gas studies.
• ### Nuclear Fusion in Laser-Driven Counter-Streaming Collisionless Plasmas(1611.03951)

Nuclear fusion reactions are the most important processes in nature to power stars and produce new elements, and lie at the center of the understanding of nucleosynthesis in the universe. It is critically important to study the reactions in full plasma environments that are close to true astrophysical conditions. By using laser-driven counter-streaming collisionless plasmas, we studied the fusion D$+$D$\rightarrow n +^3$He in a Gamow-like window around 27 keV. The results show that astrophysical nuclear reaction yield can be modulated significantly by the self-generated electromagnetic fields and the collective motion of the plasma. This plasma-version mini-collider may provide a novel tool for studies of astrophysics-interested nuclear reactions in plasma with tunable energies in earth-based laboratories.
• ### A possible formation channel for blue hook stars in globular cluster - II. Effects of metallicity, mass ratio, tidal enhancement efficiency and helium abundance(1609.09169)

Sept. 29, 2016 astro-ph.SR
Employing tidally enhanced stellar wind, we studied in binaries the effects of metallicity, mass ratio of primary to secondary, tidal enhancement efficiency and helium abundance on the formation of blue hook (BHk) stars in globular clusters (GCs). A total of 28 sets of binary models combined with different input parameters are studied. For each set of binary model, we presented a range of initial orbital periods that is needed to produce BHk stars in binaries. All the binary models could produce BHk stars within different range of initial orbital periods. We also compared our results with the observation in the Teff-logg diagram of GC NGC 2808 and {\omega} Cen. Most of the BHk stars in these two GCs locate well in the region predicted by our theoretical models, especially when C/N-enhanced model atmospheres are considered. We found that mass ratio of primary to secondary and tidal enhancement efficiency have little effects on the formation of BHk stars in binaries, while metallicity and helium abundance would play important roles, especially for helium abundance. Specifically, with helium abundance increasing in binary models, the space range of initial orbital periods needed to produce BHk stars becomes obviously wider, regardless of other input parameters adopted. Our results were discussed with recent observations and other theoretical models.
• ### Stellar activity with LAMOST. I. Spot configuration in Pleiades(1608.05452)

Aug. 18, 2016 astro-ph.SR
We use the spectra of Pleiades and field stars from LAMOST DR2 archive to study how spottedness and activity vary as a function of mass at young ages. We obtained standard TiO band strength by measuring TiO bands near 7050 $\AA$ from LAMOST spectra (R$\approx$1800) for large sample of field GKM dwarfs with solar metallicity. Analysis show that active dwarfs, including late G- and early K-type, have extra TiO absorption compare to inactive counterparts, indicating the presence of cool spots on their surface. Active late K- and M-dwarfs show deeper TiO2 and shallower TiO4 compare to inactive stars at a given TiO5, which could be partly explained through cool spots. We estimated cool spot fractional coverage for 304 Pleiades candidates by modelling their TiO2 (&TiO5) band strength with respect to standard value. Results show that surface of large fraction of K- and M-type members have very large spot coverage ($\sim$50%). We analysed a correlation between spot coverage, rotation and the amplitude of light variation, and found spot coverage on slow rotators ($R_{o}$ > 0.1) increases with decreasing Rossby Number $R_{o}$. Interestingly, we detected a saturation-like feature for spot coverage in fast rotators with a saturation level of 40%-50%. In addition, spot distribution in hotter fast rotators show more symmetrical compare to slow rotators. More interestingly, we detected large spot coverage in many M type members with no or little light variation. In bigger picture, these results provide important constraints for stellar dynamo on these cool active stars.
• ### The odd-isotope fractions of Barium in CEMP-r/s star HE 0338-3945 and r-II star CS 31082-001(1606.09318)

June 30, 2016 astro-ph.SR
We report the first measurement of the odd-isotope fractions for barium, \fodd\, in two extremely metal-poor stars: a CEMP-r/s star \he\ (\feh\,$=-2.42\pm0.11$) and an r-II star \cs\ (\feh\,$=-2.90\pm0.13$). The measured \fodd\ values are $0.23\pm0.12$ corresponding to $34.3\pm34.3$\% of the r-process contributions for \he\ and $0.43\pm0.09$ corresponding to $91.4\pm25.7$\% of the r-process contribution to Ba production for \cs. The high r-process signature of barium in \cs\ ($91.4\pm25.7\%$) suggests that the majority of the heavy elements in this star were synthesised via an r-process path, while the lower r-process value ($34.3\pm34.3\%$) found in \he\ indicates that the heavy elements in this star formed through a mix of s-process and r-process synthesis. These conclusions are consistent with studies based on AGB model calculations to fit their abundance distributions.
• ### Carbon stars from LAMOST DR2 data(1606.08932)

June 29, 2016 astro-ph.GA, astro-ph.SR
In this work, we present the new catalog of carbon stars from the LAMOST DR2 catalog. In total, 894 carbon stars are identified from multiple line indices measured from the stellar spectra. Combining the CN bands in the red end with \ctwo\ and other lines, we are able to identify the carbon stars. Moreover, we also classify the carbon stars into spectral sub-types of \ch, \CR, and \cn. These sub-types approximately show distinct features in the multi-dimensional line indices, implying that in the future we can use them to identify carbon stars from larger spectroscopic datasets. Meanwhile, from the line indices space, while the \cn\ stars are clearly separated from the others, we find no clear separation between \CR\ and \ch\ sub-types. The \CR\ and \ch\ stars seem to smoothly transition from one to another. This may hint that the \CR\ and \ch\ stars may not be different in their origins but look different in their spectra because of different metallicity. Due to the relatively low spectral resolution and lower signal-to-noise ratio, the ratio of $^{12}$C/$^{13}$C is not measured and thus the \cj\ stars are not identified.
• ### Calibration of LAMOST Stellar Surface Gravities Using the Kepler Asteroseismic Data(1604.05496)

April 19, 2016 astro-ph.SR
Asteroseismology is a powerful tool to precisely determine the evolutionary status and fundamental properties of stars. With the unprecedented precision and nearly continuous photometric data acquired by the NASA Kepler mission, parameters of more than 10$^4$ stars have been determined nearly consistently. However, most studies still use photometric effective temperatures (Teff) and metallicities ([Fe/H]) as inputs, which are not sufficiently accurate as suggested by previous studies. We adopted the spectroscopic Teff and [Fe/H] values based on the LAMOST low-resolution spectra (R~1,800), and combined them with the global oscillation parameters to derive the physical parameters of a large sample of stars. Clear trends were found between {\Delta}logg(LAMOST - seismic) and spectroscopic Teff as well as logg, which may result in an overestimation of up to 0.5 dex for the logg of giants in the LAMOST catalog. We established empirical calibration relations for the logg values of dwarfs and giants. These results can be used for determining the precise distances to these stars based on their spectroscopic parameters.
• ### Self-Seeded FEL Wavelength Extension with High-Gain Harmonic Generation(1604.01492)

April 6, 2016 physics.acc-ph
We study a self-seeded high-gain harmonic generation (HGHG) free-electron laser (FEL) scheme to extend the wavelength of a soft X-ray FEL. This scheme uses a regular self-seeding monochromator to generate a seed laser at the wavelength of 1.52 nm, followed by a HGHG configuration to produce coherent, narrow-bandwidth harmonic radiations at the GW level. The 2nd and 3rd harmonic radiation are investigated with start-to-end simulations. Detailed studies on the FEL performance and shot-to-shot fluctuations are presented.
• ### A non-LTE study of silicon abundances in giant stars from the Si I infrared lines in the zJ-band(1603.06305)

March 21, 2016 astro-ph.SR
We investigate the feasibility of the Si I infrared (IR) lines as Si abundance indicators for giant stars. We find that Si abundances obtained from the Si I IR lines based on the local thermodynamic equilibrium (LTE) analysis show large line-to-line scatter (mean value of 0.13dex), and are higher than those from the optical lines. However, when the non-LTE effects are taken into account, the line-to-line scatter reduces significantly (mean value of 0.06dex), and the Si abundances are consistent with those from the optical lines. The typical average non-LTE correction of [Si/Fe] for our sample stars is about $-$0.35dex. Our results demonstrate that the Si I IR lines could be reliable abundance indicators provided that the non-LTE effects are properly taken into account.
• ### A Pair of Giant Planets around the Evolved Intermediate-Mass Star HD 47366: Multiple Circular Orbits or a Mutually Retrograde Configuration(1601.04417)

Jan. 18, 2016 astro-ph.EP
We report the detection of a double planetary system around the evolved intermediate-mass star HD 47366 from precise radial-velocity measurements at Okayama Astrophysical Observatory, Xinglong Station, and Australian Astronomical Observatory. The star is a K1 giant with a mass of 1.81+-0.13M_sun, a radius of 7.30+-0.33R_sun, and solar metallicity. The planetary system is composed of two giant planets with minimum mass of 1.75^{+0.20}_{-0.17}Mjup and 1.86^{+0.16}_{-0.15}Mjup, orbital period of 363.3^{+2.5}_{-2.4} d and 684.7^{+5.0}_{-4.9} d, and eccentricity of 0.089^{+0.079}_{-0.060} and 0.278^{+0.067}_{-0.094}, respectively, which are derived by a double Keplerian orbital fit to the radial-velocity data. The system adds to the population of multi-giant-planet systems with relatively small orbital separations, which are preferentially found around evolved intermediate-mass stars. Dynamical stability analysis for the system revealed, however, that the best-fit orbits are unstable in the case of a prograde configuration. The system could be stable if the planets were in 2:1 mean-motion resonance, but this is less likely considering the observed period ratio and eccentricity. A present possible scenario for the system is that both of the planets have nearly circular orbits, namely the eccentricity of the outer planet is less than ~0.15, which is just within 1.4sigma of the best-fit value, or the planets are in a mutually retrograde configuration with a mutual orbital inclination larger than 160 degree.
• ### Atomic Data: Division B / Commission 14 / Working Group Atomic Data(1510.08591)

Oct. 29, 2015 physics.atom-ph
This report summarizes laboratory measurements of atomic wavelengths, energy levels, hyperfine and isotope structure, energy level lifetimes, and oscillator strengths. Theoretical calculations of lifetimes and oscillator strengths are also included. The bibliography is limited to species of astrophysical interest. Compilations of atomic data and internet databases are also included. Papers are listed in the bibliography in alphabetical order, with a reference number in the text. Comprehensive lists of references for atomic spectra can be found in the NIST Atomic Spectra Bibliographic Databases http://physics.nist.gov/asbib.
• ### High-resolution spectroscopic studies of ultra metal-poor stars found in LAMOST survey(1506.05684)

June 18, 2015 astro-ph.SR
We report on the observations of two ultra metal-poor (UMP) stars with [Fe/H]~-4.0 including one new discovery. The two stars are studied in the on-going and quite efficient project to search for extremely metal-poor (EMP) stars with LAMOST and Subaru. Detailed abundances or upper limits of abundances have been derived for 15 elements from Li to Eu based on high-resolution spectra obtained with Subaru/HDS. The abundance patterns of both UMP stars are consistent with the "normal-population" among the low-metallicity stars. Both of the two program stars show carbon-enhancement without any excess of heavy neutron-capture elements, indicating that they belong to the subclass of CEMP-no stars, as is the case of most UMP stars previously studied. The [Sr/Ba] ratios of both CEMP-no UMP stars are above [Sr/Ba]~-0.4, suggesting the origin of the carbon-excess is not compatible with the mass transfer from an AGB companion where the s-process has operated. Lithium abundance is measured in the newly discovered UMP star LAMOST J125346.09+075343.1, making it the second UMP turnoff star with Li detection. The Li abundance of LAMOST J125346.09+075343.1 is slightly lower than the values obtained for less metal-poor stars with similar temperature, and provides a unique data point at [Fe/H]~-4.2 to support the "meltdown" of the Li Spite-plateau at extremely low metallicity. Comparison with the other two UMP and HMP (hyper metal-poor with [Fe/H]<-5.0) turnoff stars suggests that the difference in lighter elements such as CNO and Na might cause notable difference in lithium abundances among CEMP-no stars.
• ### Discovery of a strongly r-process enhanced extremely metal-poor star LAMOST J110901.22+075441.8(1506.05200)

June 17, 2015 astro-ph.SR
We report the discovery of an extremely metal-poor (EMP) giant, LAMOST J110901.22+075441.8, which exhibits large excess of r-process elements with [Eu/Fe] ~ +1.16. The star is one of the newly discovered EMP stars identified from LAMOST low-resolution spectroscopic survey and the high-resolution follow-up observation with the Subaru Telescope. Stellar parameters and elemental abundances have been determined from the Subaru spectrum. Accurate abundances for a total of 23 elements including 11 neutron-capture elements from Sr through Dy have been derived for LAMOST J110901.22+075441.8. The abundance pattern of LAMOST J110901.22+075441.8 in the range of C through Zn is in line with the "normal" population of EMP halo stars, except that it shows a notable underabundance in carbon. The heavy element abundance pattern of LAMOST J110901.22+075441.8 is in agreement with other well studied cool r-II metal-poor giants such as CS 22892-052 and CS 31082-001. The abundances of elements in the range from Ba through Dy well match the scaled Solar r-process pattern. LAMOST J110901.22+075441.8 provides the first detailed measurements of neutron-capture elements among r-II stars at such low metallicity with [Fe/H]<-3.4, and exhibits similar behavior in the abundance ratio of Zr/Eu as well as Sr/Eu and Ba/Eu as other r-II stars.
• ### Using the Rossiter-McLaughlin effect to observe the transmission spectrum of Earth's atmosphere(1506.04456)

June 15, 2015 astro-ph.SR, astro-ph.EP
Due to stellar rotation, the observed radial velocity of a star varies during the transit of a planet across its surface, a phenomenon known as the Rossiter-McLaughlin (RM) effect. The amplitude of the RM effect is related to the radius of the planet which, because of differential absorption in the planetary atmosphere, depends on wavelength. Therefore, the wavelength-dependent RM effect can be used to probe the planetary atmosphere. We measure for the first time the RM effect of the Earth transiting the Sun using a lunar eclipse observed with the ESO HARPS spectrograph. We analyze the observed RM effect at different wavelengths to obtain the transmission spectrum of the Earth's atmosphere after the correction of the solar limb-darkening and the convective blueshift. The ozone Chappuis band absorption as well as the Rayleigh scattering features are clearly detectable with this technique. Our observation demonstrates that the RM effect can be an effective technique for exoplanet atmosphere characterization. Its particular asset is that photometric reference stars are not required, circumventing the principal challenge for transmission spectroscopy studies of exoplanet atmospheres using large ground-based telescopes.
• ### 19 low mass hyper-velocity star candidates from the first data release of LAMOST survey(1506.01818)

June 9, 2015 astro-ph.GA
Hyper-velocity stars are believed to be ejected out from the Galactic center through dynamical interactions between (binary) stars and the central massive black hole(s). In this paper, we report 19 low mass F/G/K type hyper-velocity star candidates from over one mil- lion stars of the first data release of the LAMOST general survey. We determine the unbound probability for each candidate using a Monte-Carlo simulation by assuming a non-Gaussian proper-motion error distribution, Gaussian heliocentric distance and radial velocity error dis- tributions. The simulation results show that all the candidates have unbound possibilities over 50% as expected, and one of them may even exceed escape velocity with over 90% probabili- ty. In addition, we compare the metallicities of our candidates with the metallicity distribution functions of the Galactic bulge, disk, halo and globular cluster, and conclude that the Galactic bulge or disk is likely the birth place for our candidates.
• ### Palladium and silver abundances in stars with [Fe/H] > -2.6(1505.04356)

May 17, 2015 astro-ph.SR
Palladium (Pd) and silver (Ag) are the key elements for probing the weak component in the rapid neutron-capture process (r-process) of stellar nucleosynthesis. We performed a detailed analysis of the high-resolution and high signal-to-noise ratio near-UV spectra from the archive of HIRES on the Keck telescope, UVES on the VLT, and HDS on the Subaru Telescope, to determine the Pd and Ag abundances of 95 stars. This sample covers a wide metallicity range with -2.6 $\lesssim$ [Fe/H] $\lesssim$ +0.1, and most of them are dwarfs. The plane-parallel LTE MAFAGS-OS model atmosphere was adopted, and the spectral synthesis method was used to derive the Pd and Ag abundances from Pd I {\lambda} 3404 {\AA} and Ag I {\lambda} 3280/3382 {\AA} lines. We found that both elements are enhanced in metal-poor stars, and their ratios to iron show flat trends at -0.6 < [Fe/H] < +0.1. The abundance ratios of [Ag/H] and [Pd/H] are well correlated over the whole abundance range. This implies that Pd and Ag have similar formation mechanisms during the Galactic evolution.