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- W1632323193 abstract "Supernovae occur in highly evolved, massive stars and typically release 10 51 to 10 52 erg. Their light curves show that the stellar radius is about one A.U. at the time of the explosion. The typical energy density in the star is about 10 11 or 10 12 erg cm -3 when the blast reaches the stellar surface. Much of the energy is present in thermal form. Since the density of the material is high, thermal equilibrium is attained rapidiy between the radiation field and the thermal motions. The temperature in the interior of the star becomes about 10 6 K, and most of the energy is present in the form of radiation. At this time the star has a large optical depth, of order 10 7 . Therefore the effective diffusion speed for radiation is very low, about 3000 cm s -1 . But the effective sound speed is large, of order 10 9 cm s -1 , and the large input of energy has destroyed the gravitational equilibrium. So the star begins violently to expand, and the pressure of the stored radiation field does work in producing mass motion of the material. Only a small fraction of the radiant energy is released from the exploded star. The photosphere, in this phase, lies in the region where the gas changes from being ionized to non-ionized, so that the photo-spheric temperature remains low, of order 10 4 K. There is little chance of observing any high-temperature phenomena at this stage in the evolution of a supernova." @default.
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- W1632323193 date "1980-01-01" @default.
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- W1632323193 title "Hot Plasmas in Supernova Remnants" @default.
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- W1632323193 doi "https://doi.org/10.1017/s1539299600004111" @default.
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