Philipp Podsiadlowski

Abstract:

Binary evolution produces a large number of formation channels for hydrogen-deficient stars. Here I review the main binary interactions, stable and unstable mass transfer, binary mergers, and apply them to a variety of objects. including hot subdwarfs, He-rich sdO stars, AM CVn stars, Type Ia supernova progenitors, ultracool white dwarfs and Type Ic and gamma-ray burst progenitors.

Abstract:

Context. The nature of the companion stars in type Ia Supernova (SNe) progenitor systems remains unclear. One possible way to discriminate between different scenarios is the presence (or absence) of circumstellar material, the left overs from the progenitor evolution that may be revealed by their interaction with the SN. Aims. A new method to probe the circumstellar environment has been exploited for the normal type Ia SN 2006X, leading for the first time to the direct detection of material which escaped the progenitor system. In this paper we apply the same analysis to the peculiar type Ia SN 2000cx, with the aim of constraining the properties of its progenitor system. Methods. Using multi-epoch, high-resolution spectroscopy we have studied the spectral region where narrow, time-variable Na ID absorption features are expected in case circumstellar material is present along the line of sight. Results. No Na ID absorption is detected in the rest-frame of the host galaxy to a level of a few mÂ, setting a stringent upper limit to the column density of the absorbing material (N(NaI) < 2 × 1010 cm -2). Conclusions. In this respect the peculiar type Ia SN 2000cx is different from the normal Ia SN 2006X. Whether this is to be attributed to a different progenitor system, to viewing-angle effects or to a low metallicity remains to be clarified. © ESO 2007.