How many years does it take for heat generated in the Sun's core to reach its outler layer, the photosphere
966288
I remember this from college as being quite a long time, but I can't remember it exactly. This is from Wikipedia:\n\n"The high-energy photons (gamma and X-rays) released in fusion reactions take a long time to reach the Sun's surface, slowed down by the indirect path taken, as well as by constant absorption and reemission at lower energies in the solar mantle. Estimates of the "photon travel time" range from as much as 50 million years to as little as 17,000 years."
663516
150000000 kilometres from the sun\n\nSo, that comes to 166666.67 hours\n\nThat is 6944.44 days\n\nwhich is 19 years, so f.
80131
According to answers.com, the sun will last another 6 billion years, so you don't need to worry about it. It also says that it will turn into a white dwarf. Yet, the other source says that it will last around 5 billion years until it turns into a white dwarf. Then, it will cool down, taking billions of years, then turn into a black dwarf.\nhttp://www.enchantedlearning.com/subjects/astronomy/stars/lifecycle/\nhas a diagram to show the cycles of stars like the sun.
1076419
The sun is only about 4.5 billion years old.  The cloud of gas and dust that it formed out of was probably huge, though.
235735
Depending on its position in the oval orbit it has around the sun, the earth gets sunlight 8.317 minutes after it is emitted from the sun.
75347
This question can't be adaquately addressed in this forum.  There are a couple websites you can refer to for these answers.\n\nhttp://solarsystem.nasa.gov\nhttp://www.nineplanets.org
84417
The Sun is currently about 5 billion years old, "burning" hydrogen by fusing hydrogen into helium. The fusion only works in the core, where the temperature and pressure is high enough.\n\nWhen the hydrogen is used up the Sun will begin to contract. Eventually the core will become hot enough that helium will start to fuse. During this time the outer layers of the Sun will expand. This is the Red Giant phase.\n\nFairly soon after this (astronomically speaking) the Sun will run out of helium. Again the sun will contract, but this time not enough to heat the core for helium to burn (helium burning happens in massive stars). \n\nAt this stage the Sun will continually contract, glowing fainter and fainter with energy derived from the collapse and not fusion, until the remnant Sun is compressed so much that it is about the size of the Moon. At the begining of this collapse more gas is lost from the outer layers of the Sun, forming what is known as a "Planetary Nebulae," a shell of gas that has nothing to do with planets.\n\nThe white dwarf stage is very, very long. The Sun will slowly fade until it is barely radiating and is a cold, bare "black dwarf."  The Sun will NOT turn into a black hole.\n\n\nSo the answer is:\n--The Sun is about 5 billion years old.\n--The Red Giant phase will occur in about 5 billion years\n--Sun as a White dwarf - starting about 5 billion from now, and ending about 10 or 15 billion years from now.\n--Sun as a cold, black dwarf - as long as the Sun doesn't crash into anything, this stage may last for hundreds of billions of years
1029085
The Sun does not have enough mass to explode as a supernova, and its mass is below the Chandrasekhar limit. 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. Following the red giant phase, intense thermal pulsations will cause the Sun to throw off its outer layers, forming a planetary nebula. The Sun will then evolve into a white dwarf, slowly cooling over eons. This stellar evolution scenario is typical of low- to medium-mass stars.
686543
From the Wiki,\n\n"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."\n\nHumans will probably be long dead before then or will have moved on.  In a few billion years, the sun will get too hot for Earth to sustain life, but it'll be a while before it finally "blows up."  More accurately, it will actually implode and slowly become an inert mass.
417138
On it's axis I presume. I'm afraid it's not definitive at all:\n\n25 days at the equator\n27 days 35 degrees of latitude from the equator.\n33 days 75 degrees of latitude from the equator.\n\nThis is for the "surface" of the sun.
458339
It takes the earth 365.25 days to complete one revolution of the sun.
526984
NO, angle of the earth on it's axis limits sunlight for a few months. The days never warm up.
134819
False  - the core is the core and the photosphere is a couple of zones beyond that.\n\nI couldn't get the other posted link to load, so I decided to answer so I could post a link for you, or others who are interested.
752529
The energy in the sun's core comes from fusing hydrogen into helium.  Most of the energy emerges in the form of high-speed particles and gamma rays, neither of which can go very far in the dense, hot plasma.  This energy moves by a process of conduction through the core, until it reaches less dense regions of the sun, where a process of convection moves the energy through the material.  \n\nOnly in the upper regions of the sun's surface does the density reach a point where the energy moves by the more familiar (to us) radiation.  The time for energy to go from the core of the sun to its surface is about a quarter of a million years.  \n\nThus, almost all the energy we see is a display of the activity in the Sun's core a quarter of a million years ago.  But there IS a way to jump the queue and see what is happening in the core.\n\nEvery fusion reaction in the Sun produces neutrinos, mass-less particles that barely interact with the surrounding matter.  These fly off unimpeded by the material around them, so, like the light from the photosphere, they move at the speed of light, and reach us eight minutes later after crossing the distance between us and the sun.\n\nIt takes a lot of effort to capture a neutrino, but they tell us a lot about what is happening in the core of the sun right now, while all we see on its surface is a sign of its remote past.  Since we're not finding as many neutrinos as we think we should, we're wondering if our knowledge of physics needs improving, or if the Sun is, in fact,a more variable star than we'd like to think.
289825
Our sun does not have enough mass or density to go nova.\n\n"The Sun is about 4.5 billion years old. it has used up about half of its nuclear fuel (hydrogen). In about 5 billion years from now, the sun will begin to die.\n\nAs the Sun grows old, it will expand. As the core runs out of hydrogen and then helium, the core will contact and the outer layers will expand, cool, and become less bright. It will become a red giant star.\n\nAfter this phase, the outer layers of the Sun will continue to expand. As this happens, the core will contract; the helium atoms in the core will fuse together, forming carbon atoms and releasing energy. The core will then be stable since the carbon atoms are not further compressible.\n\nThen the outer layers of the Sun drift off into space, forming a planetary nebula (a planetary nebula has nothing to do with planets), exposing the core.\n\nMost of its mass will go to the nebula. The remaining Sun will cool and shrink; it will eventually be only a few thousand miles in diameter!\n\nThe star is now a white dwarf, a stable star with no nuclear fuel. It radiates its left-over heat for billions of years. When its heat is all dispersed, it will be a cold, dark black dwarf - essentially a dead star (perhaps replete with diamonds, highly compressed carbon)."\n\n---and---\n\n"Our star, the sun, was born in the heavens about 4.5 billion years ago. Our sun is about 1/3 of the way through its expected life. Scientists are now predicting the following events during the remaining life of our star:\n\n    * In the next 1.1 billion years, its brightness will increase by 10%. This will super-heat our planet as a result of a severe greenhouse effect. All of the oceans on earth will boil away and all life will be destroyed.\n\n    * In about 6.5 billion years, our sun will double in brightness and use up all of its supply of hydrogen fuel in its core. This will cause the sun to begin swelling as it uses hydrogen from the layers surrounding the core.\n\n    * In about 8 billion years the sun will swell to 166 times its present size. This giant star will swallow up Mercury, Venus, and maybe even our Earth. Our sun will then be what scientists call a Red Giant because it will be very large and red in color.\n\n    * After all hydrogen fuel is used, the sun will begin to use helium as its fuel. This fuel will burn very quickly and only last about 100 million years.\n\n    * In about 12 billion years, the sun will eject much of its outer layers and become a smoldering, collapsed core that scientists would call a White Dwarf."
584790
There is no one single uniform temperature in the sun. It depends which layer we are talking about ...\n\nThe Core\nThe innermost layer of the sun is the core. With a temperature of 15 million kelvins (27 million degrees Fahrenheit) \n\nSolar Envelope\nOutside of the core is the radiative envelope, which is surrounded by the convective envelope. The temperature is 4 million kelvins (7 million degrees F). The core contains 40 percent of the sun's mass in 10 percent of the volume, while the solar envelope has 60 percent of the mass in 90 percent of the volume.\n\nPhotosphere\nThe photosphere is the zone from which the sunlight we see is emitted. The photosphere is a comparatively thin layer of low pressure gasses surrounding the envelope. It is only a few hundred kilometers thick, with a temperature of 6000 K. \n\nChromosphere\nIn an eclipse, a red circle around the outside of the sun can sometimes can be seen. This is the chromosphere. Its red coloring is caused by the abundance of hydrogen.\n\nFrom the center of the sun to the chromosphere, the temperature decreases proportionally as the distance from the core increases. The chromosphere's temperature, however, is 7000 K, hotter than that of the photosphere. Temperatures continue to increase through the corona.\n\nSunspots\nSunspots are dark spots on the photosphere, typically with the same diameter as the Earth. They have cooler temperatures than the photosphere. The center of a spot, the umbra, looks dark gray if heavily filtered and is only 4500 K (as compared to the photosphere at 6000K). \n\nThe sun has enormous organized magnetic fields that reach from pole to pole. Loops of the magnetic field oppose convection in the convective envelope and stop the flow of energy to the surface. This results in cool spots at the surface which produce less light than the warmer areas. These cool, dark spots are the sunspots.\n\nCorona\nThe outermost layer of the sun is the corona. Only visible during eclipses, it is a low density cloud of plasma with higher transparency than the inner layers. The white corona is a million times less bright than the inner layers of the sun, but is many times larger.\n\nThe corona is hotter than some of the inner layers. Its average temperature is 1 million K (2 million degrees F) but in some places it can reach 3 million K (5 million degrees F).\n\nTemperatures steadily decrease as we move farther away from the core, but after the photosphere they begin to rise again. There are several theories that explain this, but none have been proven.\n\nSolar Flares\nIn the corona, above sunspots and areas of complex magnetic field patterns, are solar flares. These sparks of energy sometimes reach the size of the Earth and can last for up to several hours. Their temperature has been recorded at 11 million K (20 million degrees F). The extreme heat produces x rays that create light when they hit the gases of the corona.
1112253
Photons are produced by the sun in it´s core, because it is only there that fusion takes place. But the plasma of the sun is dense \nand the photon is continuously absorbed and re-emitted during its rise to the surface. Hence the photon will take about a million year to make the trip.\n\nAnd 8 minutes 20 seconds more to travel from the surface to the earth.