The orbital period distribution of subdwarf B binaries

Details The orbital period distribution of subdwarf B binaries The orbital period distribution of subdwarf B binaries

2003-09-03

arxiv.org/abs/astro-ph/0309088v2

Astronomy and Astrophysics

Astrophysics

8 pages, 6 figures. To appear in "Extreme Horizontal Branch Stars and Related Objects", Astrophysics and Space Science, Kluver

Scientific paper

10.1023/B:ASTR.0000044336.18366.

We present the results of a 3.5 year long campaign to measure orbital periods of subdwarf B (sdB) star binaries. We directly compare our observed orbital period distribution with that predicted by using binary population synthesis. Up to now, most of our systems seem to have been formed through two of the formation channels discussed by Han et al.(2003), i.e. the first and the second common envelope ejection (CE) channels. At this point, thanks to the long baseline of our observations, we are starting to detect also very long orbital period systems. These have probably come from a complete different formation path, the first stable Roche Lobe overflow (RLOF) channel in which the first mass transfer phase is stable. This channel is expected to lead to the formation of very wide binaries with orbital periods ranging between 0.5 to 2000 days.

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