Physics
Scientific paper
Sep 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...308..706m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 308, Sept. 15, 1986, p. 706-720.
Physics
58
Main Sequence Stars, Stellar Evolution, Stellar Mass, White Dwarf Stars, Galactic Evolution, Hydrogen, Stellar Composition, Stellar Cores, Stellar Envelopes
Scientific paper
The authors followed the complete evolution of a Population I 3 M_sun; initial mass star from the main sequence to the white dwarf (WD) final cooling, by adopting the most reasonably updated input physics for all evolutionary phases. It is found that the mass of a WD remnant of the evolution of an initial 3 M_sun; star can hardly be smaller than ≡0.7 M_sun;. The chemical composition of the WD is stratified: a carbon-rich mantle is superposed on an oxygen-rich core. The WD has a remnant helium envelope of 0.01 - 0.02 M_sun;. The hydrogen envelope remnant at the end of the superwind phase largely depends on the residual luminosity of the helium shell. The evolutionary times of WDs down to invisibility seem to be definitely shorter than the age of the galactic disk, ranging from 6 to 8×109 yr, depending on the surface composition.
Dantona F.
Mazzitelli Irene
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