Poster abstract details

Hot subdwarf B stars (sdBs) burn helium in their cores and have only a thin hydrogen layer left at their surfaces. It is currently not well understood how these stars lost most of their hydrogen envelopes. The most promising mechanism proposed up to now is binary interaction of the subdwarf's progenitor with a companion star. We want to test this hypothesis by asteroseismic studies of pulsating subdwarfs. We compute comprehensive grids of sdB models which will be confronted with Kepler data and multicolour ground based data. This will allow us to get a detailed determination of the core and envelope masses, as well as the ages of the stars, which we will compare with the values predicted by the binary evolution theory.