Diffusion in Stellar Envelopes
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In an attempt to make the present summary comprehensible yet sufficiently concise I will risk some over-simplification: further details are given in Seaton (1997, 1998 — Papers I and II).In a star let Fv dv be the outward flux of radiant and let an atom of element k present an effective area of σv(k) for absorption of radiation. Then the momentum absorbed per atom and per-unit area and unit time is G(k) = (1/c) ∫ Fvσv(k) dv which is just the force acting on the atom. The radiative acceleration is grad(k) = G(k)/M(k) where M(k) is the atom’s mass.
1976 ◽
Vol 32
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pp. 109-116
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1970 ◽
Vol 28
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pp. 260-261
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1973 ◽
Vol 31
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pp. 268-269
1984 ◽
Vol 42
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pp. 234-235
1985 ◽
Vol 43
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pp. 426-429
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1997 ◽
Vol 40
(2)
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pp. 400-404
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2020 ◽
Vol 75
(5)
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pp. 514-522