what is the sun made out of?
106776
Hydrogen and helium, mostly. \n\n\nElement Number %\n\n--------------------------------------------------------------------------------\n in percent\nHydrogen 92.0\nHelium 7.8   \nCarbon 0.02 \nNitrogen 0.008\nOxygen 0.06\nNeon 0.01 \nMagnesium 0.003\nSilicon 0.004\nSulfur 0.002\nIron 0.003
924812
The mass of the sun is 330,000 times that of the earth. It is about half again as dense as water.
313345
solar,  sun light, hydrogen
536779
The conversion of light elements into heavy elements, hydrogen into helium and on right up to iron, by atomic fusion. This is how a star shines. When the iron stage is reached the Sun has run out of fuel and the equilibrium between thermal forces and gravity is lost and gravity wins, resulting in the collapse into a white dwarf after going Nova and spreading its heavy elements into space. That's right we are all made of star stuff! JULES
170430
I think - not sure just think- the sun is much bigger?!!!!\n\nand it is made of gas, helium! \nandddd it's so hot!
224377
No. In general, the inner planets of a solar system will be made up of heavy metals, while the lighter elements will be found in the outer planets. Jupiter, for example, has a core of liquid hydrogen.
985287
THe SUN IS NOT BURNING. IT IS MADE UP OF MILLION OF STARS SO IT DOES NOT NEED TO BURN.
728755
The Sun's current age, determined using computer models of stellar evolution and nucleocosmochronology, is thought to be about 4.57 billion years.[4]\n\nThe Sun is about halfway through its main-sequence evolution, during which nuclear fusion reactions in its core fuse hydrogen into helium. Each second, more than 4 million tonnes of matter are converted into energy within the Sun's core, producing neutrinos and solar radiation. The Sun will spend a total of approximately 10 billion years as a main sequence star.\n\nThe Sun does not have enough mass to explode as a supernova. Instead, in 4-5 billion years, it will enter a red giant phase, its outer layers expanding as the hydrogen fuel in the core is consumed and the core contracts and heats up. Helium fusion will begin when the core temperature reaches about 3×108 K. While it is likely that the expansion of the outer layers of the Sun will reach the current position of Earth's orbit, recent research suggests that mass lost from the Sun earlier in its red giant phase will cause the Earth's orbit to move further out, preventing it from being engulfed. However, Earth's water and most of the atmosphere will be boiled away.\n\nFollowing the red giant phase, intense thermal pulsations will cause the Sun to throw off its outer layers, forming a planetary nebula. The only object that remains after the outer layers are ejected is the extremely hot stellar core, which will slowly cool and fade as a white dwarf over many billions of years. This stellar evolution scenario is typical of low- to medium-mass stars.[5][6]
332983
The sun.  That's what Mother Nature used, and it works pretty good.
377820
The Sun is a ball of plasma with a diameter of 1.392 million km (864,950 mi) and a mass of about 2.0×1030 kg, which is somewhat greater than that of an average star in the Milky Way galaxy. About 74% of its mass is hydrogen, with 25% helium, and the rest made up of trace quantities of heavier elements. The Sun is about 4.6 billion (109) years old and is about halfway through its main sequence evolution, during which nuclear fusion reactions in its core fuse hydrogen into helium. About 5 million tons of matter are converted into energy within the Sun's core every second, producing neutrinos and solar radiation. In about 5 billion years, the Sun will evolve into a red giant and then a white dwarf, creating a planetary nebula in the process.
231076
The sun emits most of its radiation in a wavelength band between 0.1 and 4.0 micrometers (µm). The amount of radiation emitted from a body increases exponentially with a linear rise in temperature.\n \nSee fig 6f-2 in the link below\nhttp://www.physicalgeography.net/fundamentals/6f.html
444152
Nature is all about entropy or conservation of energy.  Stars of which Our Sun is one start their life as large balls of Hydrogen gas.  Due to the friction of the untold number of molecules  moving about, heat is developed- just like rubbing Your hands together.  The inside temperature of the Sun is about 2 million degrees.  It takes more energy to maintain 4 atoms of hydrogen than it does for one Helium.  With all the heat in the star's core it is possible for the hydrogens to form a helium by the process of nuclear fusion.  6 hydrogens take part in the reaction but two are recovered so the net result is 4h>1He.  This reaction results in the saving of 0.6% energy which works its way to the surface and radiates out into space.  Within the Sun it is estimated that about 745,000 tons of H are converted every second.  This number varies a bit when one reads the literature, but whatever the actual number is it is huge.
324411
Mean distance from\nEarth 149.6×106 km\n(92.95×106 mi)\n(8.31 minutes at the speed of light) \n\n--\nThe Sun is the spectral type G2V yellow star at the center of Earth's solar system. The Earth and other matter (including other planets, asteroids, meteoroids, comets and dust) orbit the Sun. Different latitudes of the Sun rotate at different rates; a point on the equator takes 25 days to complete a rotation, while a point at a pole takes 36 days. The resultant torsion creates the Sun's very strong magnetic field, which in turn drives the 11-year cycle of solar activity. The Sun accounts for more than 99% of the solar system's mass. Energy from the Sun has supported almost all life on Earth through photosynthesis since the appearance of the first organisms. Humans use sunlight for eyesight, warmth, growing crops, and powering solar cells.\n\nThe Sun is a ball of plasma with a diameter of 1.392 million km (864,950 mi) and a mass of about 2.0×1030 kg, which is somewhat greater than that of an average star in the Milky Way galaxy. About 74% of its mass is hydrogen, with 25% helium, and the rest made up of trace quantities of heavier elements. The Sun is about 4.6 billion (109) years old and is about halfway through its main sequence evolution, during which nuclear fusion reactions in its core fuse hydrogen into helium. About 5 million tons of matter are converted into energy within the Sun's core every second, producing neutrinos and solar radiation. In about 5 billion years, the Sun will evolve into a red giant and then a white dwarf, creating a planetary nebula in the process.
300263
Our sun began forming within an immense interstellar cloud of drifting gas and dust. Inside this cloud (called a 'nebula') were regions of relatively high density where gravity began drawing together bits and pieces of the gas and dust. Over several million years, this spherical region became denser and denser which caused its central temperature to rise. Finally, some 4.5-billion years ago, the temperature was hot enough to start nuclear fusion. Our sun was born.\n\nGod should be spelled B-I-G B-A-N-G\nPBrax@netscape.com
12842
Our Sun is a star and is thus made of the same materials (in general) that the rest of the stars are.\n\nBut because of different ages and environments, there are probably no two stars that are exactly alike.
1166564
CO2+H20+sunlight=\nO2+C6H12O6(SUGAR)\nraw material
527742
The sun is a star.  All stars eventually burn out.  See facts below:\n\nThe Sun will last about 5 billion years as it is now, a so called Main Sequence Star, and burns 700 billion tonnes a second. This may look like a lot but the Sun actually burns Hydrogen, a gas, and it turns it into Helium, another gas. This happens in the central part of the Sun, its Core, through a process called nuclear fusion. A side effect of fusion is that light and heat are created. So only a small amount of this Hydrogen, only a few Billion tonnes a second, is actually burned off to create light. I would not worry that so much Hydrogen is burnt every second as the sun has a mass of 1.989 times 1030Kg. That is 1,989,000,000,000,000,000,000,000,000,000,000 Kg, or one million nine thousand, eight hundred and nine billion, billion, billion Kg. So the odd few Billion tonnes will not be missed. \n\nWhat is really interesting is what happens after the Hydrogen has been used up in the Suns core. At this point in our Sun's life the central part of the Sun, its core, shrinks and heats up and its atmosphere will expand to cover the Earth, and possibly Mars. The Sun is now called a Red Giant Star. If you can find the constellation Orion, the bright red star in the upper left hand corner is a Red Giant called Betelgeuse. After only a few million years the core will shrink again and the our Suns atmosphere will be blown off into space to become Planetary Nebulae. What will be left is a type of Star called a White Dwarf. This will last for many tens of billions of years, slowly cooling and getting dimmer. So, our star, the Sun, will last for 5 Billion years as it is, a few million years as a Red Giant, and finally tens of Billions of Years as a White Dwarf.