What is the temperature of the inner core of the sun ?
493064
The core temperature of the sun is:\n15,600,000 K.\n\n[Just for information: Surface temperature is: 5800 K]
106448
The sun moves between 23.5 degrees N and S latitude.  In one year, (starting with spring equinox), it will move from the equator N 23.5 to the tropic of Cancer, south 47 deg. to the Tropic of Capricorn, then back north to the equator, another 23.5 deg. for a total of 94 degrees.\n\nDividing 94 degrees by 365 gives about 0.258 degrees per day or 1.806 degrees per week.
883595
The inner core has a radius of about 1,220 km (about 800 miles) and is located from 5,100 to 6,300 km (3,200 to 4,000 miles) below earth's surface. Recent discoveries suggest that the solid inner core itself is composed of layers, separated by a transition zone about 250 to 400 km thick.
19060
Inner Core: 1,221 km (759 miles)\nOuter Core: 2,259 km (1404 miles)\nLower Mantle: 2,171 km  (1345 miles)\nUpper Mantle: 720 km  (447 miles)\n\nThe page linked as a source below will give you a great introduction to the internal structre of the Earth.
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*
58963
"Solar 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."\n\n"The Sun's outer visible layer is called the photosphere and has a temperature of 6,000°C (11,000°F). "\n\n"Sunspots are dark depressions on the photosphere with a typical temperature of 4,000°C (7,000°F)."
682677
About 74% of the Sun's mass is hydrogen, 25% is helium, and the rest is 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. Approximately 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.
164903
Gravitational contraction makes things hot, just like your bicycle air pump gets hot from compressing air.  In the sun, this means TREMENDOUSLY HOT.\n\nHot enough and with enough pressure to start nuclear reactions, also facilitated by carbon atoms--the hydrogen-carbon-helium reaction:\n\nMatter is so pressed in the sun that actual space inside atoms is reduced.  Hydrogen is forced into the carbon nucleus, but it can hold only four such protons.  When this saturation state is achieved, it begins to emit helium as fast as new protons arrive.  Thus the hydrogen is changed into helium with the production of energy. Carbon, the catalyst, remains unchanged.\n\nThere is a loss of mass -- check out atomic weights and you will see a difference between two hydrogens and one helium.  The difference is mass that was converted to energy.\n\nThere are other processes going on in the sun.  Check out THE URANTIA BOOK in the 400+ pages range for more copious info on this subject in easy to understand English without jargon and pretension.\n\nThe brutally dangerous energies are attenuated by the "Compton effect" (look it up) as they percolate towards the surface transferred from one strata of elements to another.  This journey takes 500,000 years from the center!\n\nThe sun consists of many layers like an onion.  The last layer is calcium rich and 6000 miles thick.  That is because calcium is propelled to the surface, even though it is heavier.\n\nThis miraculous provision of the creators makes life possible on the earth as harmful X-rays are attenuated.\n\nCalcium is a photokinetic material under certain circumstances, where it loses one electron.  The PHOTOKINETIC FORCE propels much of this type out into the solar system annually, in spite of the massive solar gravity.\n\nYou also see shells of exploding material coming off of supernovae, much like the shell being blown off an egg.\n\nThe surface temperature of the sun is about 6000 degrees F, 3333 degrees C.\n\nHowever, in the center it is 35 million degrees Fahrenheit, about 19.4 million degrees C.\n\nThe suface is boiling.  All elements are in gaseous state, even calcium.  Much of this is boiling calcium.\n\nThere is a great battle between the forces of heat and gravity, expansion and contraction.  These have achieved a state of dynamic equilibirium on a massive scale.  At an earlier age the sun actually pulsed like those stars called Cepheid variables.\n\nI see other people have relevant details that I will not repeat.  Temperatures going out from surface are different...\n\nMy information is often left out.
53664
The heat and light in the sun is due to the vast amounts of energy produced at the core. At the core hdrogen atoms combine together to form Helium atoms due to the pressure (billions of atmospheres.) and temperature (15 million degrees C). This reaction is called fusion. \n\n  However the mass of the helium atoms produced is slightly less than the combining hydrogen atoms. This difference in the mass is coverted into energy according to einsteins equation E= mc2 (c is squared).\n  This energy is in the formed of gamma rays which reaches the earth. However what we look at is only the surface of the sun called the "photosphere" which is very much cooled than the core (just 6000 degrees).\n\nThe sun wont always be bright. Eventually as the hydrongen gets used up, the reaction will slow down and the sun will become a red giant and on further reduction will become a white dwarf and at the end it will be a black dwarf.
102507
Saturn's interior is similar to Jupiter's, having a rocky core at the center, a liquid metallic hydrogen layer above that, and a molecular hydrogen layer above that. Traces of various ices are also present. Saturn has a very hot interior, reaching 12000 K at the core, and it radiates more energy into space than it receives from the Sun. Most of the extra energy is generated by the Kelvin-Helmholtz mechanism (slow gravitational compression), but this alone may not be sufficient to explain Saturn's heat production. An additional proposed mechanism by which Saturn may generate some of its heat is the "raining out" of droplets of helium deep in Saturn's interior, the droplets of helium releasing heat by friction as they fall down through the lighter hydrogen.
744404
The Sun is the most prominent feature in our solar system. It is the largest object and contains approximately 98% of the total solar system mass. One hundred and nine Earths would be required to fit across the Sun's disk, and its interior could hold over 1.3 million Earths. 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. \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. This reaction causes four protons or hydrogen nuclei to fuse together to form one alpha particle or helium nucleus. The alpha particle is about .7 percent less massive than the four protons. The difference in mass is expelled as energy and is carried to the surface of the Sun, through a process known as convection, where it is released as light and heat. Energy generated in the Sun's core takes a million years to reach its surface. Every second 700 million tons of hydrogen are converted into helium ashes. In the process 5 million tons of pure energy is released; therefore, as time goes on the Sun is becoming lighter. \n\n \n\nThe chromosphere is above the photosphere. Solar energy passes through this region on its way out from the center of the Sun. Faculae and flares arise in the chromosphere. Faculae are bright luminous hydrogen clouds which form above regions where sunspots are about to form. Flares are bright filaments of hot gas emerging from sunspot regions. Sunspots are dark depressions on the photosphere with a typical temperature of 4,000°C (7,000°F). \n\nThe corona is the outer part of the Sun's atmosphere. It is in this region that prominences appears. Prominences are immense clouds of glowing gas that erupt from the upper chromosphere. The outer region of the corona stretches far into space and consists of particles traveling slowly away from the Sun. The corona can only be seen during total solar eclipses. (See Solar Eclipse Image). \n\nThe Sun appears to have been active for 4.6 billion years and has enough fuel to go on for another five billion years or so. At the end of its life, the Sun will start to fuse helium into heavier elements and begin to swell up, ultimately growing so large that it will swallow the Earth. After a billion years as a red giant, it will suddenly collapse into a white dwarf -- the final end product of a star like ours. It may take a trillion years to cool off completely.
828693
During most of the lifetime of a star, it neither expands nor contracts.  The gravitational attraction is balanced by internal pressure.  The internal pressure in our Sun comes from the density and temperature of the particles (atomic nuclei and electrons) in the plasma.\n\nThe temperature is maintained by the energy released by nuclear fusion in the core.  If this fusion stopped, the interior of the Sun would cool over a period of about a million years, and it would begin to contract.  (Once it contracted enough, it would begin to fuse helium instead of hydrogen and it would re-expand.)
380436
Our Sun is a normal main-sequence G2 star, one of more than 100 billion stars in our galaxy.\n\ndiameter: 1,390,000 km.\nmass: 1.989e30 kg\ntemperature: 5800 K (surface)\n15,600,000 K (core)
578437
The Sun is the most prominent feature in our solar system. It is the largest object and contains approximately 98% of the total solar system mass. One hundred and nine Earths would be required to fit across the Sun's disk, and its interior could hold over 1.3 million Earths. 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. \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. This reaction causes four protons or hydrogen nuclei to fuse together to form one alpha particle or helium nucleus. The alpha particle is about .7 percent less massive than the four protons. The difference in mass is expelled as energy and is carried to the surface of the Sun, through a process known as convection, where it is released as light and heat. Energy generated in the Sun's core takes a million years to reach its surface. Every second 700 million tons of hydrogen are converted into helium ashes. In the process 5 million tons of pure energy is released; therefore, as time goes on the Sun is becoming lighter. \n\n\n\nThe chromosphere is above the photosphere. Solar energy passes through this region on its way out from the center of the Sun. Faculae and flares arise in the chromosphere. Faculae are bright luminous hydrogen clouds which form above regions where sunspots are about to form. Flares are bright filaments of hot gas emerging from sunspot regions. Sunspots are dark depressions on the photosphere with a typical temperature of 4,000°C (7,000°F). \n\nThe corona is the outer part of the Sun's atmosphere. It is in this region that prominences appears. Prominences are immense clouds of glowing gas that erupt from the upper chromosphere. The outer region of the corona stretches far into space and consists of particles traveling slowly away from the Sun. The corona can only be seen during total solar eclipses. (See Solar Eclipse Image). \n\nThe Sun appears to have been active for 4.6 billion years and has enough fuel to go on for another five billion years or so. At the end of its life, the Sun will start to fuse helium into heavier elements and begin to swell up, ultimately growing so large that it will swallow the Earth. After a billion years as a red giant, it will suddenly collapse into a white dwarf -- the final end product of a star like ours. It may take a trillion years to cool off completely. \nhope this works, go to the web site, too, just to see for yourself. good luck
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
425682
The Core: The Sun's core has a tremendously high temperature and pressure. The temperature is roughly 15 million °C. At this temperature, nuclear fusion occurs, turning four hydrogen nuclei into a single helium nucleus plus a LOT of energy. This "hydrogen burning" releases gamma rays (high-energy photons) and neutrinos (particles with no charge and almost no mass). \n\nThe Radiative Zone (or radiation zone): The next layer out from the core is this zone which emits radiation. This radiation diffuses outwards. The temperature ranges from 15 million °C to one million °C. It may take photons of radiation millions of years to pass through the radiative zone, as they gradually make their way outwards. \n\nThe Convective Zone: In this next layer, photons continue to make their way outwards via convection (towards lower temperature and pressure). The temperature ranges from one million °C to 6,000 °C. \n\nThe Photosphere: This is the lower atmosphere of the Sun and the part that we see (since it emits light at visible wavelengths). This layer is about 300 miles (500km) thick. The temperature is about 5,500 °C. \n\nThe Chromosphere: This reddish layer is an area of rising temperatures. The temperature ranges from 6,000 °C (at lower altitudes) to 50,000 °C (at higher altitudes). This layer is a few thousand miles (or kilometers) thick. It appears red because hydrogen atoms are in an excite state and emit radiation near the red part of the visible spectrum. \n\nThe Chromosphere is visible during solar eclipses (when the moon blocks the Photosphere). \n\nThe Corona: This is the outer layer of the Sun's atmosphere. The corona extends for millions of miles and the temperatures are tremendous, reaching one million °C. \n\nHoles in the corona occur where the Sun's magnetic field loops out into space. These coronal holes may be the source of the solar wind, a stream of energetic particles that permeate the Solar System.
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