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- W10040752 abstract "Accretion is a dominant factor in the early evolution of stars. The first time an accretion regime settles in is when a dusty opaque core forms. The mass of adiabatically contracting core inside the isothermally collapsing envelope depends only on the optical properties of dust. Spherically symmetric models of dusty cores were constructed using the Henyey technique with accretion boundary conditions (Menshchikov 1986). It appears that all protostars with normal chemical composition should pass through the stage of a quasistatic dusty core. The evolution of dusty cores is similar to that of “normal” young stars with accretion. One could distinguish convective, radiative and central core contraction phases. The life-time t c of the core depends on the core mass M c and the accretion rate Ṁ (for M c = 0.01 M ⊙ and Ṁ = 1.6x10 −6 , 1.6x10 −5 M ⊙ /year t c = 1.2x10 4 , 3x10 3 yrs consequently). After dust exhaustion in the core it collapses and a central ionized quasistatic region grows in several tens of years. A flash of infrared radiation at the moment is not excluded." @default.
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- W10040752 date "1987-01-01" @default.
- W10040752 modified "2023-10-16" @default.
- W10040752 title "On Early Evolution of Accreting Stars" @default.
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- W10040752 doi "https://doi.org/10.1017/s0074180900096169" @default.
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