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Дата изменения: Tue Feb 25 19:08:23 1997 Дата индексирования: Tue Oct 2 14:12:06 2012 Кодировка: Поисковые слова: annular solar eclipse |
Next: Stellar
Winds From Normal Up: Principal
Evolutionary States of Previous: Roche
lobe overflow (stage
In the process of mass exchange, the hydrogen envelope of the star can
be almost completely lost, leaving behind a hot WD for
, or as a non-degenerate helium star
for higher masses (a WR-star in the case of a star with initial mass >
) as a remnant. The lifetime of a helium star
is determined by the helium nuclear burning duration (Iben and Tutukov,
1985[74])
If the helium (WR) star fills its RL (the relatively rare case ``BB'' of evolution; Delgado and Thomas (1981)[44]; see discussion in van den Heuvel (1994)[205]), the helium-rich envelope is lost and a CO stellar core remains with a mass