What happens at that temperature?  Is that like the temperature of the sun or something?
207516
The surface of the Earth turns to molten lava.
316309
No its not necessarily closer to the sun(visit usgs.org) and even if its closer, it may be closer by 0.000001%.What big difference does that make.Its the difference in air pressure that makes the peaks colder.The higher you go up in the earth's atmosphere,the pressure decreases.And even an object 90% closer to the sun may not be that hot.
205604
The sun heats the ground. \nThe warm ground in turn heats the air above. (In the above diagram, the warm ground and air are shaded in red.) \nThe warm air at the ground is lighter and less dense than the surrounding air above, so it begins to rise. \nThe rising air takes on the shape of a round "parcel." \nSeveral things happen as the parcel rises up through the atmosphere:\nThe higher up into the atmosphere you go, the lower the pressure. As the parcel of air rises, it experiences this drop in pressure. As the pressure on the air parcel drops, the parcel expands and increases in size. (In the diagram I drew the rising parcel getting bigger as it rises.) \nAnytime air expands due to a drop in pressure, it also gets cooler. So, as the parcel rises and expands, it also cools. (In the diagram, the green and blue colors indicate the parcel getting cooler.) The parcel cools at a rate of approximately 10 degrees C per 1000 meters of rise (or 5.5 degrees F per 1000 feet of rise.) This is called the dry adiabatic lapse rate. \nWarm air is able to hold larger amounts of water vapor (water in gas form) than cool air. The cooling parcel is no longer able to hold all of the water vapor it was able to hold when it was warm. The excess water vapor begins to condense out of the air parcel in the form of liquid cloud droplets. When water vapor begins to condense into liquid droplets (moisture), this means the air parcel is saturated and has reached its dewpoint temperature. The higher the parcel rises, the more it expands, the cooler it gets, and the greater the amount of moisture that condenses out of it. \nThe rising, expanding, cooling air parcel finally rises so high that the surrounding atmospheric air is the same temperature as the cooled parcel. This is called equilibrium temperature. When equilibrium is reached, the parcel loses momentum and stops rising. \nBy the time the air parcel has reached equilibrium temperature, enough moisture has condensed out of it to form a visible cloud! \nCloud heights and shapes vary according to the atmospheric conditions. On a hot day, clouds will tend to form higher, because the rising air parcels must rise higher in order to cool enough to reach dewpoint. When air parcels continue to rise after dewpoint has been reached and condensation has occurred, the cloud becomes very tall. This is how cumulus congestus and cumulonimbus clouds form. If air parcels only rise a short distance over a large geographical area after reaching dewpoint, layer clouds (such as stratus) will form.
4261
It's a long winded explanation - see link below.\n\n(snip)\nthe sun's heat acts almost the same as the sun's light — it passes through the air almost as though the air wasn't there.\n\nThis means that almost all of the sun's heat goes into warming up the oceans and the land it hits. As the oceans and ground warm up, they warm the air next to them, and this air warms the air a little higher up and so on. But, as you go higher, there's less and less heat available to go up, and the air gets colder.\n(snip)
103029
It evaporates.  Remember your body temperature is very warm (98.6 deg).  Your skin is an organ that is designed to protect your body by keeping things out.  You may get a little absorption on the outer most layer, but even it will eventually evaporate.
488149
Well, we know that the white star must be hotter...for stars, the bluer it is, the hotter.  Similarly, the redder it is, the colder it is.\n\nIn general, white stars have a surface temperature around 10,000 Kelvin, while red stars are around 3000 Kelvin.  For simplicity's sake, let's say the white star is 3 times hotter.\n\nBy The "Stefan-Boltzmann" law, hot things emit more light...a whole lot more, in fact: the amount of light emitted goes as the temperature to the fourth power.  A chunk of white star material that's 3 times hotter than a chunk of red star material will emit 3 raised to the fourth power, or 81 times as much light.\n\nSo, if they're the same brightness and distance, there must be a whole lot more "cool chunks" in the red star to appear just as bright as the "hot chunks" of the white star...it's the same way that two 50-watt light bulbs will be just as bright as a 100-watt light bulb.\n\nTherefore, the red star is much larger.
247429
A good approximation to the distribution of electromagnetic radiation emitted by the sun is given by the equation for a blackbody with a temperature of 5780 Kelvin:\n\nPower (Watts/meter^2 surface are/meter wavelength) = \n  2*pi*h*c^2/L^5*(exp(h*c/L*k*T)-1)\n\nwhere\n\nh = Planck's constant (6.626 x 10^-34 Joule*sec)\nc = speed of light (2.998 x 10^8 meters/sec)\nL = wavelength (meters)\nk = Boltzmann's constant (1.38 x 10^-23 Joule/Kelvin)\nT = temperature (Kelvin)\n\nThe sun's power output peaks in the visible portion (around a wavelength of 500nm) of the electromagnetic spectrum, but it emits over the entire range of possible wavelengths.\n\nIn reality, the solar spectrum is much more complicated than a simple blackbody curve because of the absorption of specific frequencies by the atoms making up the sun, as well as temperature inhomogeneities and effects due to the sun's magnetic field.
136548
You do not possibly have enough information to answer this question properly, you need to know, where it is at, how far from the sun, like the others said, is there a planet or any obstacle between it and the sun, what is it's current temp, so on and so on....here is something about tempature in space though\n\nEmpty space itself cannot have a temperature, unless you mean some abstruse question about quantum vacuums.\n\nHowever, if you put a physical object into space, it will reach a temperature that depends on how efficiently it absorbs and emits radiation and on what heating sources are nearby.  For example, an object that both absorbs and emits perfectly, put at the Earth's distance from the Sun, will reach a temperature of about 280 K or 7 C. If it is shielded from the Sun but exposed to interplanetary and interstellar radiation, it reaches about 5 K.  If it were far from all stars and galaxies, it would come into librium with the microwave background at about 2.7 K. Spacecraft (and spacewalking astronauts) often run a bit hotter than 280 K because they generate internal energy.
329738
If you are talking about the sun's surface, then the earth's core is hotter than it, because the earth's core is 15,000 C while the sun's surface is 5,000 C only. But if you compare the earth's core with the sun's core, then the sun's core temperature is estimated to be 14,000,000 C - 15,000,000 C.
7954
The Sun's outer visible layer is called the photosphere and has a temperature of 6,000°C (11,000°F). This layer has a mottled appearance due to the turbulent eruptions of energy at the surface. \n\nSolar energy is created deep within the core of the Sun. It is here that the temperature (15,000,000° C; 27,000,000° F) and pressure (340 billion times Earth's air pressure at sea level) is so intense that nuclear reactions take place.
56081
Temperature is the degree of heat and heat is the transfer of energy from one body to another as a result of a difference in temperature or a change in phase.
352415
The others set the problem up, but don't answer the question!? \n\nThe surface temperature answer for a star emitting twice the energy flux of the sun(Sol) is 6900 degrees K.
513583
All energy eventually ends up as heat.  It's a consequence of the second law of thermodynamics
499758
It is absorbed as heat.
176603
The answer is: the sun doesn't burn.  What you are thinking of is combustion, the process of combining oxygen with something to release energy (fire).  What is happening in the sun is nuclear fusion.  Two hydrogen atoms smack into each other with such force that they join together to make a helium atom.  During this process, some of the mass is turned into energy, which is heat and light.  It has nothing to do with oxygen.
148054
i remember a couple years ago we had a hot spell.  we actually keep track of the hotest and coldest of every day of the year. so it will be like, hey did you hear?  no what?  yesterday was the hotest april 19th since 1932!  yea?! awesome.  \nok. so its kinda cheesey...back to the question, somewhere around 105-110f and as low as mebe 20f.  not  quite exactly sure
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Extrapolate the formula, using the surface temoerature, and instead of the earth distance, substitute the distance you want to caluclate the temperature at.  \n\n\nMeasuring the Sun's Temperature\nOne method, called Wien's law, uses the wavelength of the peak emission, wavelengthpeak, in the Sun's continuous spectrum. The temperature in Kelvin = 2.9 × 106 nanometers/wavelengthpeak.\n\nAnother method uses the flux of energy reaching the Earth and the inverse square law. Recall from the Stellar Properties chapter that the flux is the amount of energy passing through a unit area (e.g., 1 meter2) every second. From the Inverse Square Law of Light Brightness, you find that the solar flux at the Earth's distance = the Sun's surface flux × (Sun's radius/Earth's distance)2 = 1380 Watts/meter2. Since the Sun's photosphere is approximately a thermal radiator, the flux of energy at its surface = sigma × (the Sun's surface temperature)4, where sigma is the Stefan-Boltzmann constant. Rearranging the equation, the photosphere's temperature = [(solar flux at Earth)/sigma) × (Earth distance/Sun's radius)2]1/4.\n\nThese two methods give a rough temperature for the Sun of about 5800 K. The upper layers of the photosphere are cooler and less dense than the deeper layters, so you see absorption lines in the solar spectrum. Which element absorption lines are present and their strength depends sensitively on the temperature. You can use the absorption line strengths as an accurate temperature probe to measure a temperature of about 5840 K. \n\nRead the link, you'll have to scroll down to come up to the stuff I have cut and paste above.\nst\nHope you find this useful.