temerature and atmosphere for the sun?
813508
The temperature of the sun varies depending on proximity to the surface.  The core temperature can be more than 13 million degrees Celcius.  The corona is only about 5 million degrees Celcius.  As a large ball of plasma fusing gases together, the sun does not have an atmosphere in the usual sense of the word.
1018347
The surface of the Sun, called the photosphere, is at a temperature of about 5800 Kelvin/ 5 526 degree Celsius/ 9 980 Fahrenheit.\n\n\nErm guys, the lithosphere is the brittle uppermost shell of the earth, not the sun.  *just to clarify out things a bit*
729148
Our atmosphere -- the gaseous envelope surrounding the Earth -- is composed of several gases, primarily nitrogen, oxygen, argon and carbon dioxide. Water vapor and minute bits of dust, salt and clay-silicate particles swirl about in the mixture.\nThe atmosphere has four vertical layers that radiate from Earth and vary by temperature and composition. Proceeding from the ground outward, they are the troposphere, stratosphere, mesosphere and thermosphere.\n\n\nAll of the “optical phenomena” – halos, sun dogs, sun pillars, coronas and rainbows – are produced at specific levels in the troposphere, which extends from the surface up to about 12 kilometers, eight miles or 42,000 feet depending on which measuring stick you pick. Here, the temperature decreases rapidly with altitude – averaging 59°F at the surface and a right chilly -69°F at 11 km. Commercial jets fly in the upper reaches of the troposphere.\n\n\nHigh-level cirrus clouds form in extremely cold air where water vapor condenses on tiny dust and salt particles to form ice \ncrystals.\nHence these are responsible for various phenomena circles aroound light emitting/reflecting bodies on the sky, and the rings are formed depending upon how the light gets scattered and the colours also depend on that.\nVR
747063
Mercury actually does have an atmosphere but the planet's small size makes it hard to retain.  It is not stable.
19701
Earth's Atmosphere\nThe Earth is surrounded by a blanket of air, which we call the atmosphere. It reaches over 560 kilometers (348 miles) from the surface of the Earth, so we are only able to see what occurs fairly close to the ground. Early attempts at studying the nature of the atmosphere used clues from the weather, the beautiful multi-colored sunsets and sunrises, and the twinkling of stars. With the use of sensitive instruments from space, we are able to get a better view of the functioning of our atmosphere.\n\nLife on Earth is supported by the atmosphere, solar energy, and our planet's magnetic fields. The atmosphere absorbs the energy from the Sun, recycles water and other chemicals, and works with the electrical and magnetic forces to provide a moderate climate. The atmosphere also protects us from high-energy radiation and the frigid vacuum of space.\n\nThe envelope of gas surrounding the Earth changes from the ground up. Four distinct layers have been identified using thermal characteristics (temperature changes), chemical composition, movement, and density\n\nComposition of the Atmosphere\nThe atmosphere is primarily composed of Nitrogen (N2, 78%), Oxygen (O2, 21%), and Argon (Ar, 1%). A myriad of other very influential components are also present which include the water (H2O, 0 - 7%), "greenhouse" gases or Ozone (O, 0 - 0.01%), Carbon Dioxide (CO2, 0.01-0.1%),\n\n\nLayers of atmosphere\n\nThe atmosphere is divided into five layers. It is thickest near the surface and thins out with height until it eventually merges with space. \n\n1) The troposphere is the first layer above the surface and contains half of the Earth's atmosphere. \nThe troposphere is where all weather takes place; it is the region of rising and falling packets of air. The air pressure at the top of the troposphere is only 10% of that at sea level (0.1 atmospheres). There is a thin buffer zone between the troposphere and the next layer called the tropopause\n\n2)The Stratosphere and Ozone Layer\nAbove the troposphere is the stratosphere, where air flow is mostly horizontal. The thin ozone layer in the upper stratosphere has a high concentration of ozone, a particularly reactive form of oxygen. This layer is primarily responsible for absorbing the ultraviolet radiation from the Sun. The formation of this layer is a delicate matter, since only when oxygen is produced in the atmosphere can an ozone layer form and prevent an intense flux of ultraviolet radiation from reaching the surface, where it is quite hazardous to the evolution of life. There is considerable recent concern that manmade flourocarbon compounds may be depleting the ozone layer, with dire future consequences for life on the Earth\nMany jet aircrafts fly in the stratosphere because it is very stable. \n\n3)Mesosphere\nThe mesosphere starts just above the stratosphere and extends to 85 kilometers (53 miles) high. In this region, the temperatures again fall as low as -93 degrees Celsius as you increase in altitude. The chemicals are in an excited state, as they absorb energy from the Sun. The mesopause separates the mesophere from the thermosphere.\n\nThe regions of the stratosphere and the mesosphere, along with the stratopause and mesopause, are called the middle atmosphere by scientists. This area has been closely studied on the ATLAS Spacelab mission series. Meteors or rock fragments burn up in the mesosphere.\n\n4)Thermosphere\nThe thermosphere starts just above the mesosphere and extends to 600 kilometers (372 miles) high. The temperatures go up as you increase in altitude due to the Sun's energy. Temperatures in this region can go as high as 1,727 degrees Celsius. Chemical reactions occur much faster here than on the surface of the Earth. This layer is known as the upper atmosphere.\n\nThe upper and lower layers of the thermosphere will be studied more closely during the Tethered Satellite Mission (TSS-1R).\n\n\n5) exosphere\nThe exosphere starts at the t
1002235
The planet's temp. depends on their distance frm the sun. Otherwise it's all vaccum and thus can't have temp.
310415
the atmosphere is made mostly of hydrogen and helium but contains trace amounts of methane, water vapor, and ammonia. For futher information go here: http://en.wikipedia.org/wiki/Jupiter_(planet)#Atmosphere
188714
Yes. The first atmospheres were composed of hydrogen and helium. \n\nWhen the protosun began nuclear fusion in its core it soon started blasting the planets with radiation. The atmospheres heated up and since heat is kinetic energy in between atoms and molecules it now became possible for atmospheric elements to reach escape velocity and leave their respective planet. \n\nMercurys atmosphere was doomed from the beginning being so close to the sun and having so little mass. Although there are some gasses left, like sodium, those gasses are also being blasted off into space. Mercurys atmosphere is so thin it is a more perfect vacuum than we can reproduce here on earth.\n\nVenus lost most of its hydrogen and helium. The water vapour was split into hydrogen and oxygen by ultraviolet radiation with the hydrogen quickly escaping. Heavier gasses like CO2 and nitrogen remains. Venus has about as much nitrogen, per mass, in its atmosphere as earth does and about as much CO2 that earth had in the beginning.\n\nFor earth every atom lighter than 3 U can reach escape velocity. That is why there is no He3 left while there is still some He4. Earths atmosphere was alot denser in the beginning. After the lighter elements had been blasted off there was enormous amounts of CO2 in the atmosphere. Unlike Venus earth became cold enough to condensate the water vapour. The CO2 began dissolving into the primordial oceans where chemical reactions began turning the H2CO3 into solid carbonates that settled on the bottom. This thinning was later accelerated by life. Finally life began producing oxygen that also got trapped by biochemical reactions as ironoxides that settled onto the bottom of the oceans. It took billions of years for the oceans to run out of iron until eventually oxygen began building up in the atmosphere. The atmopshere earth has now is earths third.\n\nMars was also too small to keep a significant atmosphere but it was able to survive for much longer than on Mercury because it is farther from the sun. Still only a little CO2 remains while even the nitrogen, which had to have been there, has escaped. Most of the water has suffered the same fate as the water on Venus. Interesting that mars has about the same amount of CO2, by mass, in its atmosphere while Venus has about the same amount of nitrogen. Percentage wise Venus atmosphere is almost identical to Mars only about 10000 times as dense.\n\nFurther out the gas giants have been able to hold on to their primordial atmospheres despite relentless solar radiation.
867403
The sun is made of hydrogen.
1179944
it is strongest between 10am and 2pm.  this is because as the sun rises from the horision the light (and other radiations) are being filtered through more atmosphere. as the sun climbs higher it is comming more directly at you, peeking at noon(ish). Finally as the sun sets it reverses the process and again becomes filtered through more atmosphere.
55579
The sun is a giant ball of plasma constantly fusing hydrogen into helium.  It is not 'on fire', so to speak, so the lack of oxygen and the coldness of space don't effect it like a match or something.
855359
Try the following links\n\n1. comp and temp: http://en.wikipedia.org/wiki/Earth%27s_atmosphere\n\n2. ozone layer: http://en.wikipedia.org/wiki/Ozone_layer\n\n3. ionosphere: http://en.wikipedia.org/wiki/Ionosphere
1136056
Because of its proximity to the earth, and because it is such a typical star, the sun is a unique resource for the study of stellar phenomena. No other star can be studied in such detail. The star closest to the sun is 4.3 light-years (4 × 1013 km/2.5 × 1013 mi) away. To observe features on its surface comparable to those that can be seen routinely on the sun would require a telescope almost 30 km (18.6 mi) in diameter. Such a telescope, moreover, would have to be put into space to avoid distortions caused by the earth's atmosphere.\n\n    The Sun is an ordinary G2 star, one of more than 100 billion stars in our galaxy.\n\n \n\n        diameter:    1,390,000 km.\n        mass:        1.989e30 kg\n        temperature: 5800 K (surface)\n                     15,600,000 K (core)\n   The Sun is by far the largest object in the solar system. It contains more than 99.8% of the total mass of the Solar System (Jupiter contains most of the rest). \n   The Sun is personified in many mythologies: the Greeks called it Helios and the Romans called it Sol. \n\n   The Sun is, at present, about 75% hydrogen and 25% helium by mass (92.1% hydrogen and 7.8% helium by number of atoms); everything else ("metals") amounts to only 0.1%. This changes slowly over time as the Sun converts hydrogen to helium in its core. \n\n \n\n   The outer layers of the Sun exhibit differential rotation: at the equator the surface rotates once every 25.4 days; near the poles it's as much as 36 days. This odd behaviour is due to the fact that the Sun is not a solid body like the Earth. Similar effects are seen in the gas planets. The differential rotation extends considerably down into the interior of the Sun but core of the Sun rotates as a solid body. \n\n   Conditions at the Sun's core (approximately the inner 25% of its radius) are extreme. The temperature is 15.6 million Kelvin and the pressure is 250 billion atmospheres. At the centre of the core the Sun's density is more than 150 times that of water. \n\n   The Sun's energy output (3.86e33 ergs/second or 386 billion billion megawatts) is produced by nuclear fusion reactions. Each second about 700,000,000 tons of hydrogen are converted to about 695,000,000 tons of helium and 5,000,000 tons (=3.86e33 ergs) of energy in the form of gamma rays. As it travels out toward the surface, the energy is continuously absorbed and re-emitted at lower and lower temperatures so that by the time it reaches the surface, it is primarily visible light. For the last 20% of the way to the surface the energy is carried more by convection than by radiation. \n\n    The surface of the Sun, called the photosphere, is at a temperature of about 5800 K. Sunspots are "cool" regions, only 3800 K (they look dark only by comparison with the surrounding regions). Sunspots can be very large, as much as 50,000 km in diameter. Sunspots are caused by complicated and not very well understood interactions with the Sun's magnetic field. \n\n   A small region known as the chromosphere lies above the photosphere. \n\n    The highly rarefied region above the chromosphere, called the corona, extends millions of kilometers into space but is visible only during eclipses (left). Temperatures in the corona are over 1,000,000 K. \n\n   The Sun's magnetic field is very strong (by terrestrial standards) and very complicated. Its magnetosphere (also known as the heliosphere) extends well beyond Pluto. \n\n    In addition to heat and light, the Sun also emits a low density stream of charged particles (mostly electrons and protons) known as the solar wind which propagates throughout the solar system at about 450 km/sec. The solar wind and the much higher energy particles ejected by solar flares can have dramatic effects on the Earth ranging from power line surges to radio interference to the beautiful aurora borealis.  \n\n   The solar wind has large effects on the tails of comets and even has measurable effects on t
985280
The modern atmosphere is sometimes referred to as Earth's "third atmosphere", in order to distinguish the current chemical composition from two notably different previous compositions. The original atmosphere was primarily helium and hydrogen. Heat from the still-molten crust, and the sun, plus a probably enhanced solar wind, dissipated this atmosphere.\n\nAbout 4.4 billion years ago, the surface had cooled enough to form a crust, still heavily populated with volcanoes which released steam, carbon dioxide, and ammonia. This led to the early "second atmosphere", which was primarily carbon dioxide and water vapor, with some nitrogen but virtually no oxygen. This second atmosphere had approximately 100 times as much gas as the current atmosphere, but as it cooled much of the carbon dioxide was dissolved in the seas and precipitated out as carbonates. The later "second atmosphere" contained nitrogen, carbon dioxide, and very recent simulations run at the University of Waterloo and University of Colorado in 2005 suggest that it may have had up to 40% hydrogen[3]. It is generally believed that the greenhouse effect, caused by high levels of carbon dioxide and methane, kept the Earth from freezing. In fact temperatures were probably very high, over 70 degrees C, until some 2.7 billion years ago.
168316
The Atmosphere\n\nHow is the atmosphere structured?\nThe atmosphere consists of four distinct layers, which are seperated by a boundaries that end in the suffix "pause". There is a lot of information in the Earth Science Reference Tables page 14. \nTroposphere-This layer of the atmosphere is closest to the earth and 99% of all weather takes place here because most of the water vapor is located here. \nStratosphere-This layer is above the troposphere and contains ozone, which is an important gas, because it absorbs cancer-causing ultra violet rays from the Sun. \nMesosphere-This layer is above the stratosphere. \nThermosphere-This is the uppermost layer of the atmosphere. \nEarth Science Reference Table page 14: \nHow do we describe the present condition of the atmosphere?\nThe present condition of the atmosphere is called WEATHER and it is described using observations of temperature, air pressure, humidity, wind, cloudiness and precipitation. \nWhat is temperature?\nTemperature is a measure of the average kinetic energy of the particles of a substance. In other words, the more molecules vibrate within a substance, the higher the temperature. \nMeasurement - There are three scales that measure temperature: CELSIUS, FAHRENHEIT AND KELVIN scales. There is a conversion scale on page 13 of your ESRT. \nMaps - Meteorologists find it useful to map temperatures and they use lines to connect equal temperatures called Isotherms. \nWhat is air pressure and how is it used to predict the weather?\nAir Pressure - Air pressure is also called barometric or atmospheric pressure. By definition, it is the weight of the atmosphere pushing down on the earth. \nBarometer - A barometer is the instrument that measures air pressure and it uses units of millibars (mb) or inches of mercury (inches). \nFactors that affect air pressure:\nTemperature - As the temperature of the air increases, the air pressure decreases, which is an indirect relationship. \nHumidity - As the humidity of the air increases, the air pressure decreases, which is an indirect relationship.\nYou might ask "WHY?": Humid air is lighter than dry air. When water vapor enters dry air, it does not squeeze in between the molecules of air. Instead, the water vapor pushes out many of the air's heaviest molecules like Nitrogen and Oxygen. In other words, lighter molecules of water vapor replace heavier molecules and the result is the air weighs less and therefore has less air pressure. \n\nHigh air pressure - means that the atmosphere is heavy at that location and from our notes above, you can conclude that the air is probably cool and dry (if you are not sure, see notes above). So, if the barometer indicates high pressure or rising air pressure, you can conclude that the weather will be cool and dry. \nLow air pressure - means that the atmosphere is not heavy at that location and from our notes above, you can conclude that the air is probably warm and humid (if you are not sure, see notes above). So, if the barometer indicates low pressure or falling air pressure, you can conclude that the weather will be warmer and humid. \nMaps - Meteorologists find it useful to map air pressure and they use lines to connect equal equal air pressures called Isobars
1035134
The Atmosphere is hot(~~)
663547
By that logic, outer space should be a regular tropical paradise.  It has to do with the heat capacity of air.  The atmosphere is thinner the farther you get from the Earth's core, and less air can hold less total heat.  Also, I think the first post about the Earth's radiant heat is probably another factor.