Issue |
A&A
Volume 376, Number 3, September IV 2001
|
|
---|---|---|
Page(s) | 950 - 954 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20010949 | |
Published online | 15 September 2001 |
The formation of black hole low-mass X-ray binaries: Through case B or case C mass transfer?
Astronomical Institute "Anton Pannekoek" , Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
Corresponding author: G. Nelemans, GijsN@astro.uva.nl
Received:
17
April
2001
Accepted:
27
June
2001
The formation of low-mass X-ray binaries containing a rather
massive () black hole is problematic because in most
recent stellar evolutionary calculations the immediate progenitors
of these black holes (Wolf-Rayet stars) lose so much mass via their
stellar wind that their final masses are well below the observed
black hole masses. We discuss the recently proposed solution that
these binaries are formed through case C mass transfer (i.e. mass
transfer after core helium burning is completed), avoiding a long
Wolf-Rayet phase and thus significant mass loss. We show that only
some of the currently available models for the evolution of massive
stars allow this formation channel. We also investigate the effect
of the downward revised Wolf-Rayet mass-loss rate as is suggested by
observations, and conclude that in that case Wolf-Rayet stars end
their lives with significantly higher masses than previously found
and may be able to form a black holes.
Key words: stars: statistics / stars: binaries: close / stars: evolution
© ESO, 2001
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