0_Wizard
I love the color yellow.  Sunlight has a slight yellow due due to the temperature of the sun.
Sunlight has a slight yellowish hue, due to the surface temperature of the sun.
chosen_Yellow_0
Yellow
chosen_topic_0_Yellow
Yellow
Yellow is the color between green and orange on the spectrum of visible light. It is evoked by light with a dominant wavelength of roughly 570590 nm. It is a primary color in subtractive color systems, used in painting or color printing. In the RGB color model, used to create colors on television and computer screens, yellow is a secondary color made by combining red and green at equal intensity. Carotenoids give the characteristic yellow color to autumn leaves, corn, canaries, daffodils, and lemons, as well as egg yolks, buttercups, and bananas. They absorb light energy and protect plants from photodamage.
Sun
The Sun is the star at the center of the Solar System. It is a nearly perfect sphere of hot plasma, with internal convective motion that generates a magnetic field via a dynamo process. It is by far the most important source of energy for life on Earth. Its diameter is about 1.39 million kilometers, i.e. 109 times that of Earth, and its mass is about 330,000 times that of Earth, accounting for about 99.86% of the total mass of the Solar System. About three quarters of the Sun's mass consists of hydrogen (~73%); the rest is mostly helium (~25%), with much smaller quantities of heavier elements, including oxygen, carbon, neon, and iron.
Fansub
A fansub (short for fan-subtitled) is a version of a foreign film or foreign television program which has been translated by fans (as opposed to an officially licensed translation done by professionals) and subtitled into a language other than that of the original. The practice of making fansubs is called fansubbing and is done by a fansubber. Fansubbers typically form groups and divide the work up. The first distribution media of fansubbed material was VHS and Betamax tapes. Early fansubs were produced using analog video editing equipment. First, a copy of the original source material or raw was obtained, most commonly from a commercial laserdisc.
Color temperature
The color temperature of a light source is the temperature of an ideal black-body radiator that radiates light of a color comparable to that of the light source. Color temperature is a characteristic of visible light that has important applications in lighting, photography, videography, publishing, manufacturing, astrophysics, horticulture, and other fields. In practice, color temperature is meaningful only for light sources that do in fact correspond somewhat closely to the radiation of some black body, i.e., those on a line from reddish/orange via yellow and more or less white to blueish white; it does not make sense to speak of the color temperature of, e.g., a green or a purple light.
Atmospheric optics
Atmospheric optics deals with how the unique optical properties of Earth's atmosphere cause a wide range of spectacular optical phenomena. The blue color of the sky is a direct result of Rayleigh scattering, which redirects higher frequency (blue) sunlight back into the field of view of the observer. Because blue light is scattered more easily than red light, the Sun takes on a reddish hue when it is observed through a thick atmosphere, as during a sunrise or sunset. Additional particulate matter in the sky can scatter different colors at different angles, creating colorful, glowing skies at dusk and dawn.
Ultraviolet
Ultraviolet (UV) is an electromagnetic radiation with a wavelength from 10 nm to 400 nm, shorter than that of visible light but longer than X-rays. UV radiation constitutes about 10% of the total light output of the Sun, and is thus present in sunlight. It is also produced by electric arcs and specialized lights, such as mercury-vapor lamps, tanning lamps, and black lights. Although it's not considered an ionizing radiation because its photons lack the energy to ionize atoms, long-wavelength ultraviolet radiation can cause chemical reactions and causes many substances to glow or fluoresce. Consequently, the chemical and biological effects of UV are greater than simple heating effects, and many practical applications of UV radiation derive from its interactions with organic molecules.
Passive solar building design
In passive solar building design, windows, walls, and floors are made to collect, store, and distribute solar energy in the form of heat in the winter and reject solar heat in the summer. This is called passive solar design because, unlike active solar heating systems, it does not involve the use of mechanical and electrical devices. The key to design a passive solar building is to best take advantage of the local climate performing an accurate site analysis. Elements to be considered include window placement and size, and glazing type, thermal insulation, thermal mass, and shading. Passive solar design techniques can be applied most easily to new buildings, but existing buildings can be adapted or "retrofitted".
1_Apprentice
So is the sun not really yellow? Does it have other colors?
0_Wizard
I have seen pictures of the solar flares of hot plasma that show red
It is a nearly perfect sphere of hot plasma, with internal convective motion that generates a magnetic field via a dynamo process. It is by far the most important source of energy for life on Earth.
self_Sun_1
Sun
self_1_Sun
Corona
A corona (Latin, 'crown') is an aura of plasma that surrounds the Sun and other stars. The Sun's corona extends millions of kilometres into space and is most easily seen during a total solar eclipse, but it is also observable with a coronagraph. The word "corona" is a Latin word meaning "crown", from the Ancient Greek κορώνη (korōnè, “garland, wreath”). The high temperature of the Sun's corona gives it unusual spectral features, which led some in the 19th century to suggest that it contained a previously unknown element, "coronium". Instead, these spectral features have since been explained by highly ionized iron (Fe-XIV).
Solar phenomena
Solar phenomena are the natural phenomena occurring within the magnetically heated outer atmospheres in the Sun. These phenomena take many forms, including solar wind, radio wave flux, energy bursts such as solar flares, coronal mass ejection or solar eruptions, coronal heating and sunspots. These phenomena are generated by a helical dynamo near the center of the Sun's mass that generates strong magnetic fields and a chaotic dynamo near the surface that generates smaller magnetic field fluctuations. The total sum of all solar fluctuations is referred to as solar variation. The collective effect of all solar variations within the Sun's gravitational field is referred to as space weather.
Solar cycle 24
Solar Cycle 24 is the 24th solar cycle since 1755, when extensive recording of solar sunspot activity began. It is the current solar cycle, and began in December 2008 with a smoothed minimum of 2.2 (SIDC formula). There was only minimal activity until early 2010. It reached its maximum in April 2014 with smoothed sunspot number only 116.4, the lowest in over a century. Prior to the minimum between the end of Solar Cycle 23 and the beginning of Solar Cycle 24, there were essentially two competing theories about how strong Solar Cycle 24 would be. The two camps could be distinguished by those postulating the Sun retained a long memory (Solar Cycle 24 would be active) or whether it had a short memory (Solar Cycle 24 would be quiet).
Sun
The Sun is the star at the center of the Solar System. It is a nearly perfect sphere of hot plasma, with internal convective motion that generates a magnetic field via a dynamo process. It is by far the most important source of energy for life on Earth. Its diameter is about 1.39 million kilometers, i.e. 109 times that of Earth, and its mass is about 330,000 times that of Earth, accounting for about 99.86% of the total mass of the Solar System. About three quarters of the Sun's mass consists of hydrogen (~73%); the rest is mostly helium (~25%), with much smaller quantities of heavier elements, including oxygen, carbon, neon, and iron.
Superflare
Superflares are very strong explosions observed on stars with energies up to ten thousand times that of typical solar flares. The stars in this class satisfy conditions which should make them solar analogues, and would be expected to be stable over very long time scales. The original nine candidates were detected by a variety of methods. No systematic study was possible until the launch of the Kepler satellite, which monitored a very large number of solar-type stars with very high accuracy for an extended period. This showed that a small proportion of stars had violent outbursts, up to 10,000 times as powerful as the strongest flares known on the Sun.
Solar flare
A solar flare is a sudden flash of increased Sun's brightness, usually observed near its surface. Flares are often, but not always, accompanied by a coronal mass ejection. Solar flares fall on a very broad spectrum of emissions, an energy release of typically 10 joules of energy is considered to be the median for a well-observed event, while a major event can emit up to 10 joules  The flare ejects clouds of electrons, ions, and atoms along with the electromagnetic waves through the Sun's corona into outer space. The phenomenon therefore provides an early example of multi-messenger astronomy. If ejection is in the direction of the Earth the particles hitting the upper atmosphere can cause bright auroras, and may even disrupt long range radio communication.
X-ray astronomy
X-ray astronomy is an observational branch of astronomy which deals with the study of X-ray observation and detection from astronomical objects. X-radiation is absorbed by the Earth's atmosphere, so instruments to detect X-rays must be taken to high altitude by balloons, sounding rockets, and satellites. X-ray astronomy is the space science related to a type of space telescope that can see farther than standard light-absorption telescopes, such as the Mauna Kea Observatories, via x-ray radiation. X-ray emission is expected from astronomical objects that contain extremely hot gases at temperatures from about a million kelvin (K) to hundreds of millions of kelvin (MK).
1_Apprentice
Oh my! What causes those solar flares?
0_Wizard
Solar flare are emissions of energy release
Solar flares fall on a very broad spectrum of emissions, an energy release of typically 10 joules of energy is considered to be the median for a well-observed event, while a major event can emit up to 10 joules  The flare ejects clouds of electrons, ions, and atoms along with the electromagnetic waves through the Sun's corona into outer space.
self_Solar_flare_2
Solar flare
self_5_Solar_flare
Solar cycle 24
Solar Cycle 24 is the 24th solar cycle since 1755, when extensive recording of solar sunspot activity began. It is the current solar cycle, and began in December 2008 with a smoothed minimum of 2.2 (SIDC formula). There was only minimal activity until early 2010. It reached its maximum in April 2014 with smoothed sunspot number only 116.4, the lowest in over a century. Prior to the minimum between the end of Solar Cycle 23 and the beginning of Solar Cycle 24, there were essentially two competing theories about how strong Solar Cycle 24 would be. The two camps could be distinguished by those postulating the Sun retained a long memory (Solar Cycle 24 would be active) or whether it had a short memory (Solar Cycle 24 would be quiet).
Solar flare
A solar flare is a sudden flash of increased Sun's brightness, usually observed near its surface. Flares are often, but not always, accompanied by a coronal mass ejection. Solar flares fall on a very broad spectrum of emissions, an energy release of typically 10 joules of energy is considered to be the median for a well-observed event, while a major event can emit up to 10 joules  The flare ejects clouds of electrons, ions, and atoms along with the electromagnetic waves through the Sun's corona into outer space. The phenomenon therefore provides an early example of multi-messenger astronomy. If ejection is in the direction of the Earth the particles hitting the upper atmosphere can cause bright auroras, and may even disrupt long range radio communication.
Solar phenomena
Solar phenomena are the natural phenomena occurring within the magnetically heated outer atmospheres in the Sun. These phenomena take many forms, including solar wind, radio wave flux, energy bursts such as solar flares, coronal mass ejection or solar eruptions, coronal heating and sunspots. These phenomena are generated by a helical dynamo near the center of the Sun's mass that generates strong magnetic fields and a chaotic dynamo near the surface that generates smaller magnetic field fluctuations. The total sum of all solar fluctuations is referred to as solar variation. The collective effect of all solar variations within the Sun's gravitational field is referred to as space weather.
Superflare
Superflares are very strong explosions observed on stars with energies up to ten thousand times that of typical solar flares. The stars in this class satisfy conditions which should make them solar analogues, and would be expected to be stable over very long time scales. The original nine candidates were detected by a variety of methods. No systematic study was possible until the launch of the Kepler satellite, which monitored a very large number of solar-type stars with very high accuracy for an extended period. This showed that a small proportion of stars had violent outbursts, up to 10,000 times as powerful as the strongest flares known on the Sun.
Coronal mass ejection
A coronal mass ejection (CME) is a significant release of plasma and magnetic field from the solar corona. They often follow solar flares and are normally present during a solar prominence eruption. The plasma is released into the solar wind, and can be observed in coronagraph imagery. Coronal mass ejections are often associated with other forms of solar activity, but a broadly accepted theoretical understanding of these relationships has not been established. CMEs most often originate from active regions on the Sun's surface, such as groupings of sunspots associated with frequent flares. Near solar maxima, the Sun produces about three CMEs every day, whereas near solar minima, there is about one CME every five days.
Reuven Ramaty High Energy Solar Spectroscopic Imager
Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI, originally High Energy Solar Spectroscopic Imager or HESSI) is a NASA solar flare observatory. It is the sixth mission in the Small Explorer program, selected in October 1997 and launched on 5 February 2002. Its primary mission is to explore the physics of particle acceleration and energy release in solar flares. HESSI was renamed to RHESSI on 29 March 2002 in honor of Reuven Ramaty, a pioneer in the area of high energy solar physics. RHESSI is the first space mission named after a NASA scientist. RHESSI was built by Spectrum Astro for Goddard Space Flight Center and is operated by the Space Sciences Laboratory in Berkeley, California.
Solar observation
Solar observation is the scientific endeavor of studying the Sun and its behavior and relation to the Earth and the remainder of the Solar System. Deliberate solar observation began thousands of years ago. That initial era of direct observation gave way to telescopes in the 1600s followed by satellites in the twentieth century. Stratigraphic data suggest that solar cycles have occurred for hundreds of millions of years, if not longer; measuring varves in precambrian sedimentary rock has revealed repeating peaks in layer thickness corresponding to the cycle. It is possible that the early atmosphere on Earth was more sensitive to solar irradiation than today, so that greater glacial melting (and thicker sediment deposits) could have occurred during years with greater sunspot activity.
1_Apprentice
The sun must be just a huge ball of energy. I wonder why it doesn't burn itself away?
0_Wizard
The sun produces about three CME (coronal mass ejections) a day and eventually, it will burn out.
Near solar maxima, the Sun produces about three CMEs every day, whereas near solar minima, there is about one CME every five days.
self_Coronal_mass_ejection_5
Coronal mass ejection
self_4_Coronal_mass_ejection
Coronal mass ejection
A coronal mass ejection (CME) is a significant release of plasma and magnetic field from the solar corona. They often follow solar flares and are normally present during a solar prominence eruption. The plasma is released into the solar wind, and can be observed in coronagraph imagery. Coronal mass ejections are often associated with other forms of solar activity, but a broadly accepted theoretical understanding of these relationships has not been established. CMEs most often originate from active regions on the Sun's surface, such as groupings of sunspots associated with frequent flares. Near solar maxima, the Sun produces about three CMEs every day, whereas near solar minima, there is about one CME every five days.
Solar phenomena
Solar phenomena are the natural phenomena occurring within the magnetically heated outer atmospheres in the Sun. These phenomena take many forms, including solar wind, radio wave flux, energy bursts such as solar flares, coronal mass ejection or solar eruptions, coronal heating and sunspots. These phenomena are generated by a helical dynamo near the center of the Sun's mass that generates strong magnetic fields and a chaotic dynamo near the surface that generates smaller magnetic field fluctuations. The total sum of all solar fluctuations is referred to as solar variation. The collective effect of all solar variations within the Sun's gravitational field is referred to as space weather.
Solar cycle 24
Solar Cycle 24 is the 24th solar cycle since 1755, when extensive recording of solar sunspot activity began. It is the current solar cycle, and began in December 2008 with a smoothed minimum of 2.2 (SIDC formula). There was only minimal activity until early 2010. It reached its maximum in April 2014 with smoothed sunspot number only 116.4, the lowest in over a century. Prior to the minimum between the end of Solar Cycle 23 and the beginning of Solar Cycle 24, there were essentially two competing theories about how strong Solar Cycle 24 would be. The two camps could be distinguished by those postulating the Sun retained a long memory (Solar Cycle 24 would be active) or whether it had a short memory (Solar Cycle 24 would be quiet).
Solar cycle
The solar cycle or solar magnetic activity cycle is the nearly periodic 11-year change in the Sun's activity (including changes in the levels of solar radiation and ejection of solar material) and appearance (changes in the number and size of sunspots, flares, and other manifestations). They have been observed (by changes in the sun's appearance and by changes seen on Earth, such as auroras) for centuries. The changes on the Sun cause effects in space, in the atmosphere, and on Earth's surface. While it is the dominant variable in solar activity, aperiodic fluctuations also occur. Solar cycles have an average duration of about 11 years.
Corona
A corona (Latin, 'crown') is an aura of plasma that surrounds the Sun and other stars. The Sun's corona extends millions of kilometres into space and is most easily seen during a total solar eclipse, but it is also observable with a coronagraph. The word "corona" is a Latin word meaning "crown", from the Ancient Greek κορώνη (korōnè, “garland, wreath”). The high temperature of the Sun's corona gives it unusual spectral features, which led some in the 19th century to suggest that it contained a previously unknown element, "coronium". Instead, these spectral features have since been explained by highly ionized iron (Fe-XIV).
Solar wind
The solar wind is a stream of charged particles released from the upper atmosphere of the Sun, called the corona. This plasma consists of mostly electrons, protons and alpha particles with thermal energy between 1.5 and 10 keV. Embedded within the solar-wind plasma is the interplanetary magnetic field. The solar wind varies in density, temperature and speed over time and over solar latitude and longitude. Its particles can escape the Sun's gravity because of their high energy resulting from the high temperature of the corona, which in turn is a result of the coronal magnetic field. At a distance of more than a few solar radii from the Sun, the solar wind is supersonic and reaches speeds of 250 to 750 kilometers per second.
Sun
The Sun is the star at the center of the Solar System. It is a nearly perfect sphere of hot plasma, with internal convective motion that generates a magnetic field via a dynamo process. It is by far the most important source of energy for life on Earth. Its diameter is about 1.39 million kilometers, i.e. 109 times that of Earth, and its mass is about 330,000 times that of Earth, accounting for about 99.86% of the total mass of the Solar System. About three quarters of the Sun's mass consists of hydrogen (~73%); the rest is mostly helium (~25%), with much smaller quantities of heavier elements, including oxygen, carbon, neon, and iron.
1_Apprentice
When do you think it will burn out? I'm scared!
0_Wizard
At 300,000 times the size of Earth there is a lot of energy there.  Certainly it will last long beyond our lifetimes.
109 times that of Earth, and its mass is about 330,000 times that of Earth, accounting for about 99.86% of the total mass of the Solar System.
self_Sun_3
Sun
self_6_Sun
Sun
The Sun is the star at the center of the Solar System. It is a nearly perfect sphere of hot plasma, with internal convective motion that generates a magnetic field via a dynamo process. It is by far the most important source of energy for life on Earth. Its diameter is about 1.39 million kilometers, i.e. 109 times that of Earth, and its mass is about 330,000 times that of Earth, accounting for about 99.86% of the total mass of the Solar System. About three quarters of the Sun's mass consists of hydrogen (~73%); the rest is mostly helium (~25%), with much smaller quantities of heavier elements, including oxygen, carbon, neon, and iron.
Radiation effects from the Fukushima Daiichi nuclear disaster
The radiation effects from the Fukushima Daiichi nuclear disaster are the observed and predicted effects resulting from the release of radioactive isotopes from the Fukushima Daiichi Nuclear Power Plant after the 2011 Tōhoku earthquake and tsunami. Radioactive isotopes were released from reactor containment vessels as a result of venting to reduce gaseous pressure, and the discharge of coolant water into the sea. This resulted in Japanese authorities implementing a 20 km exclusion zone around the power plant, and the continued displacement of approximately 156,000 people as of early 2013. Trace quantities of radioactive particles from the incident, including iodine-131 and caesium-134/137, have since been detected around the world.
Star
A star is type of astronomical object consisting of a luminous spheroid of plasma held together by its own gravity. The nearest star to Earth is the Sun. Many other stars are visible to the naked eye from Earth during the night, appearing as a multitude of fixed luminous points in the sky due to their immense distance from Earth. Historically, the most prominent stars were grouped into constellations and asterisms, the brightest of which gained proper names. Astronomers have assembled star catalogues that identify the known stars and provide standardized stellar designations. However, most of the stars in the Universe, including all stars outside our galaxy, the Milky Way, are invisible to the naked eye from Earth.
Supercapacitor
A supercapacitor (SC) (also electric double-layer capacitor (EDLC), also called supercap, ultracapacitor or Goldcap) is a high-capacity capacitor with capacitance values much higher than other capacitors (but lower voltage limits) that bridge the gap between electrolytic capacitors and rechargeable batteries. They typically store 10 to 100 times more energy per unit volume or mass than electrolytic capacitors, can accept and deliver charge much faster than batteries, and tolerate many more charge and discharge cycles than rechargeable batteries. Supercapacitors are used in applications requiring many rapid charge/discharge cycles rather than long term compact energy storage: within cars, buses, trains, cranes and elevators, where they are used for regenerative braking, short-term energy storage or burst-mode power delivery.
Product lifetime
Product lifetimes represent an important area of enquiry with regards to product design, the circular economy and sustainable development. This is because products, with the materials involved in their design, production, distribution, use and disposal (across their life cycle), embody carbon due to the energy involved in these processes. Therefore, if product lifetimes can be extended, the use of energy, embodied in carbon, can be reduced and progress can be made towards reducing greenhouse gas emissions: Bocken et al. term this ""Slowing resource loops"" (309, "their emphasis"). In addition, excessive waste generation has been attributed to short-lived goods and a throwaway society.
Energy storage
Energy storage is the capture of energy produced at one time for use at a later time. A device that stores energy is sometimes called an accumulator or battery. Energy comes in multiple forms including radiation, chemical, gravitational potential, electrical potential, electricity, elevated temperature, latent heat and kinetic. Energy storage involves converting energy from forms that are difficult to store to more conveniently or economically storable forms. Bulk energy storage is currently dominated by hydroelectric dams, both conventional as well as pumped. Some technologies provide short-term energy storage, while others can endure for much longer.
List of Lorien Legacies characters
This is a list of characters appearing in the "Lorien Legacies" series of young adult science fiction books, written under the pseudonym Pittacus Lore. The Elders were 10 Loric Garde that acted as the protectors and/or politicians of Lorien who had discovered the Phoenix stones, they rewarded Lorien with legacies and chimæra. Originally there were ten Lorien Elders, but due to the Secret Wars; the conflict between the Loric and the Mogadorians, the tenth Elder had supposedly died during this time. There was a prophecy which said that an unknown evil that will destroy and take Lorien by surprise.
1_Apprentice
Oh thank goodness!