Binary Evolution Channels explaining the subdwarf B star PG1336-018

Details Binary Evolution Channels explaining the subdwarf B star PG1336-018 Binary Evolution Channels explaining the subdwarf B star PG1336-018

Aug 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007iaus..240..384h&link_type=abstract

Binary Stars as Critical Tools and Tests in Contemporary Astrophysics, International Astronomical Union. Symposium no. 240, he

Astronomy and Astrophysics

Astrophysics

Scientific paper

The formation of subdwarf B (sd B) stars poses several problems for stellar and binary evolution theory. SdB stars are core-helium burning stars (~0.5 M[]) with an extremely thin hydrogen envelope (<0.02 M[&sun;]). A large fraction of sdB stars are found in binaries. This suggests that Roche lobe overflow can be an effective way to remove almost the entire hydrogen envelope near the tip of the first giant branch. To test this and other models, a detailed investigation of the sdB interior structure is necessary. Luckily, sdB stars have been observed to pulsate in heat-driven oscillation modes in agreement with theoretical expectations. Thus, asteroseismology provides an excellent tool to test the outcome of sdB formation channels. The work we present here is a first step in this direction and concerns a dedicated study of the range of fundamental parameters of progenitors of the sdB pulsating eclipsing binary PG 1336-018 from a binary evolution code. Our results will constitute a fruitful starting point for our future seismic work on this star which will be based on high-precision VLT photometry and spectroscopy of this target star.

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