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yider
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ja88
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ÂÂ 2015-07-13, 11:29 PM #23
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polar168
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ÂÂ 2015-07-13, 11:35 PM #24
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msnow
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ÂÂ 2015-07-14, 12:49 PM #28
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Energy transfer

According to current models, random scattering from free electrons in the solar radiative zone (the zone within 75% of the solar radius, where heat transfer is by radiation) sets the photon diffusion time scale (or "photon travel time") from the core to the outer edge of the radiative zone at about 170,000 years.

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Photons and neutrinos

High-energy gamma-ray photons initially released with fusion reactions in the core are almost immediately absorbed by the solar plasma of the radiative zone, usually after traveling only a few millimeters. Re-emission happens in a random direction and usually at a slightly lower energy. With this sequence of emissions and absorptions, it takes a long time for radiation to reach the Sun's surface. Estimates of the photon travel time range between 10,000 and 170,000 years

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Lewis, Richard. The Illustrated Encyclopedia of the Universe. Harmony Books, New York. 1983: 65.

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Because energy transport in the Sun is a process that involves photons in thermodynamic equilibrium with matter, the time scale of energy transport in the Sun is longer, on the order of 30,000,000 years. This is the time it would take the Sun to return to a stable state, if the rate of energy generation in its core were suddenly changed.[90]

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On the time scale of energy transport in the sun

Abstract

It is pointed out that the time scale of energy transport in the Sun is the Kelvin¡VHelmholtz time scale, of order 3¡Ñ10^7 years, roughly 100 times longer than the photon-diffusion time estimated by Mitalas and Sills (1992). The difference corresponds to a factor U gas/U rad, the ratio of thermal energy density to radiation energy density. Thus the heat transport, even when mediated by photons, is slowed down by the large heat capacity of the star. A numerical example calculation is presented.

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ÂÂ 2015-07-14, 04:13 PM #29
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asdfgz
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