Hot subdwarfs

Details Hot subdwarfs Hot subdwarfs

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aspc..318..387m&link_type=abstract

In Spectroscopically and Spatially Resolving the Components of the Close Binary Stars, Proceedings of the Workshop held 20-24 Oc

Astronomy and Astrophysics

Astronomy

3

Scientific paper

Hot subdwarfs can be divided broadly into subdwarf O-stars (sdO) and subdwarf-B stars (sdB). The majority of sdB stars are extreme horizontal branch (EHB) stars, i.e., core-helium burning stars with a mass close to 0.5 Msun and with a very thin, inert hydrogen envelope. It has recently been discovered that most sdB stars are spectroscopic binaries with orbital periods of hours or days. I review the observed properties of these binaries and discuss the constraints these observations impose on models for the formation of the EHB stars. The sdO stars are a heterogeneous group. I highlight some recent results for binary sdO stars.

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