Binary Evolution Channels explaining the subdwarf B star PG1336-018
[S.l. : s.n.]
InIAU Symposium, pp. 171
Article in monograph or in proceedings
Display more detailsDisplay less details
iss. ; 240
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[o]). 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.
Upload full text
Use your RU credentials (u/z-number and password) tolog in with SURFconextto upload a file for processing by the repository team.