Describe the structure of the sun and its major processes.?
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In essence, the sun is a gargantuan nuclear fusion reactor. It uses hydrogen as its fuel, the fusion process creates helium, which is lighter than hydrogen. Witin the sun, hydrogen is 'falling' toward the core, as helium is rising to the surface, causing convection currents. This is what gives the sun its mottled appearance. Sunspots occasionally occur, these oddities are associated with geomagnetic storms which send tons of radiation hurtling into space as a solar flare, or a larger coronal mass ejection. When this radiation interacts with our magnetosphere here on earth, spectacular light shows ensue around the poles...the Aurorae. These bursts of electromagnetic energy also play havoc on radio reception. The sun is a complex engine of massive power and energy, but it's still in essence a fusion reactor.
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solar,  sun light, hydrogen
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check out this site for general information\nwww.nineplanets.org/sol.html \n\nhttp://sohowww.nascom.nasa.gov/\n\nhttp://www.spaceweather.com/\n\n\nthese are just some sites. is there anything in particular that you would like to know about the sun??
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How hot is concentrated light, what is the temp of the sun?\n\nWELL WE HAVE A ENERGY SHORTAGE, ONLY AT SUNSET.\n\n I read about Solar collection in power plants like Solar One.  In these plants the where they make molten salt, for heat transfer for running steam generator. At the reciever of Solar One plant or concentrated light point temperature reachest approximately 1,050 Fahrenheit.\n    \n      THIS LINK IS ABOUT YOUR SUN AND THE TEMPS ARE HOT.\n         SO HOW MUCH LIGHT CAN WE CONDENTRATE MORE  \n           DEVELOPMENT IN SOLAR SAILS\n\nhttp://hyperphysics.phy-astr.gsu.edu/hbase/hframe.html \n\n Earth's Sun is a medium-sized star which lies on the main sequence with 90% of the known stars. It has a effective surface temperature is 5780 K, putting it in spectral class G2. Its mass is 1.989 x 1030 kg and its mean radius is 6.96 x 108 meters. The mass of the sun is over 99.8% of the mass of the entire known solar system, leading de Pater and Lissauer to refer lightly to the solar system as "the Sun plus some debris". \n\nThe sun radiates energy at the rate of 3.85 x1026 watts. Just outside the earth's atmosphere solar energy is received, assuming normal incidence, at the rate of 1340 watts per square meter. \n \n\nThe orbit of Earth ranges from 1.47 to 1.52 x 1011 meters from the Sun. The average light travel time to the earth is 8.3 minutes. \n\nThe radius of the sun at 696,000 km is 109 times the Earth's radius. Its surface gravity is 274 m/s2 or 28.0 times that of the Earth. Its mean density is 1410 kg/m3 or 0.255 times the mean density of Earth. \n\nThe composition of the sun is 71% hydrogen, 27.1% helium and less than 2% of all other elements. \n\nThe center temperature is modeled to be 15.5 million K. The Sun is fueled by the proton cycle of nuclear fusion.\n\nEscape velocity = 618 km/s\n\nSO
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First you start with a nebula of gas and dust. Under its own gravity, the nebula begins to spiral and clump together. As the gas gets closer together, it starts to heat up. Once the mass of the center object(proto-star) contains enough matter(mass), the object starts to fuse hydrogen into helium. This creates a massive amount of energy which we see emitted from stars. High mass stars like blue giants will burn through their hydrogen much faster than smaller stars like our sun. I hope this isn't too complex for 2nd grade.
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Your teacher.\n\nThe sun is the center of our solar system (thus the terminology), and all of the planets circle around the sun.\n\nJust to clarify on one point...The sun is not the center of the universe.  It is the center of our solar system.  There are thousands of solar systems in our universe, and our sun is not at the center of these.
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Astronomy:The life of Stars. You can get some awesome pictures for that and there is plenty to write about, like (i am not completely sure about this number)did u know that light takes almost 250,000 years to travel from the center of our sun to the surface.\n\nhttp://en.wikipedia.org/wiki/Star
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try these sites. They will answer any questions you might have.\n\nwww.msnbc.com/news/251727.asp\n\ncsep10.phys.utk.edu/astr161/lect/time/seasons.html\n\ncurious.astro.cornell.edu/question.php?number=196\n\nscience.howstuffworks.com/question165.htm
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The energy from the sun comes from nuclear fussion: the combining of 2 Hydrogen atoms to make Helium and energy.\nWhen the sun will lose it's fuel (in about 5 Billion years), it will turn into a red giant star.
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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.
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Intro with main idea of topic\n2-3 supporting detail paragraphs\n1 short conclustion
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It's going to be difficult to tell you more than I know, but I'll give it my best shot.\n\nThe sun is big and bright and hot.  It is a giant fusion reactor creating energy by fusing atoms of matter together.  The energy is transmitted out into space as photons of light.\n\nIt is a medium sized yellow star which began making energy about 4 billion years ago and is estimated to have about 5 billion years left before its fuel begins to run out.
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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.
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Nasa - The Solar Wind\nhttp://www-istp.gsfc.nasa.gov/Education/wsolwind.html\n\nSolar wind is a constant flow of gases from the sun.  It results from the expansion of gases in the corona.  Billions and billions of particles are produced by the sun each second it burns, giving off heat and light.  A vast majority of these particles have an electric charge (a plus or minus), and in turn these particles are affected by the sun’s magnetic field.  These small particles are then blasted into the upper part of the sun’s atmosphere by intense radiation from the sun’s core.  The upper region of the sun’s atmosphere that these particles are blasted into is known as the corona.  When electrons are caught in the corona they become heated to temperatures exceeding four million degrees F.  This causes the particles to move very rapidly, and they collide into each other and lose their electrons and become electrically charged particles.  These particles are known as ions and they make up the solar wind.\n\nhttp://www.kelso.wednet.edu/coweeman/contents/Mars_Project/solar_winds.htm
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The sun operates like all other stars in it uses fusion to create its energy.  The sun is made of hydrogen and when a hydrogen molecule is combined with an oxygen molecule at a highspeed it becomes helium and the excess energy from the two molecules combining gives the sun its heat.  Gravity is working to crush the star and its fusion energy is working to inflate it.  This is what gives the star its spherical shape.
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sun = constant \nconstant = sun\n\nthe only piece of information you didn't define.
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General Characteristics of the Sun\n\nThe sun is actually a star of about medium size; it appears larger than the other stars because of its relative nearness to the earth. The earth's distance from the sun varies from 91,377,000 mi (147,053,000 km) at perihelion to 94,537,000 mi (152,138,000 km) at aphelion (see apsis). The mean distance is c.92,960,000 mi (149,591,000 km); this is taken as the astronomical unit (AU) of distance used for measuring distances within the solar system. The sun is approximately 865,400 mi (1,392,000 km) in diameter, and its volume is about 1,300,000 times that of the earth. Its mass is almost 700 times the total mass of all the bodies in the solar system and 332,000 times that of the earth. The sun's surface gravity is almost 28 times that of the earth; i.e., a body on the surface of the sun would weigh about 28 times its weight on earth. The density of the material composing the sun is about one fourth that of the earth; compared with water, the sun's average density is 1.41. At its center, the sun has a density of over 100 times that of water, a temperature of 10 to 20 million degrees Celsius, and a pressure of over 1 billion atmospheres.\n\nObservations of sunspots and studies of the solar spectrum indicate that the sun rotates on its axis from east to west; because of its gaseous nature its rate of rotation varies somewhat with latitude, the speed being greatest (a period of almost 25 days) in the equatorial region and least at the poles (a period of about 35 days). The axis of the sun is inclined at an angle of about 7° to the plane of the ecliptic.\n\nThe bright surface of the sun is called the photosphere. Its temperature is about 6,000°C. The photosphere appears darker near the edge (limb) of the sun's disk because of greater absorption of light by the sun's atmosphere in this area; this phenomenon is called limb darkening. During an eclipse of the sun the chromosphere and the corona (the outer layers of the sun's atmosphere) are observed. Also of interest is the high-speed, tenuous extension of the corona known as the solar wind.\n\nProduction of Solar Energy\n\nThe vast and continual production of solar energy cannot be attributed merely to combustion, to the gradual cooling of a hot body, to the fall of meteorites into the sun, or to gradual shrinkage with transformation of potential energy into heat (a theory proposed by Helmholtz). The theory of relativity with its implication of the equivalence of mass and energy led to the assumption that energy stored in the atoms constituting the sun's gases is constantly being released by conversion of some of the masses of the atom's nuclei during nuclear transmutations (see nuclear energy). H. A. Bethe proposed a cycle of nuclear reactions known as the carbon cycle, or CNO bi-cycle, to account for the nuclear changes. In this cycle carbon acts much as a catalyst, while hydrogen is transformed by a series of reactions into helium and large amounts of high-energy gamma radiation are released. It is now thought that the so-called proton-proton process is a more important energy source; this process begins with the collision of two protons and ends with the production of helium, while gamma radiation is released throughout.\n\nSee nucleosynthesis; stellar evolution.\n\nThe Study of the Sun\n\nBy means of the spectroscope much has been learned about the composition of the sun. There are numerous dark lines of varying widths in the solar spectrum. These were first intensively studied by Joseph Fraunhofer and are commonly known by his name. From a study of the lines the chemical composition of the sun is determined on the basis of the discovery by Kirchhoff that the dark lines correspond in position to the bright lines characteristic of the spectra produced by elements in the laboratory. The darkness of the lines in the sun's spectrum is attributed to the presence of a slightly cooler layer of gases above the phot