Observational white dwarf seismology

Details Observational white dwarf seismology Observational white dwarf seismology

Jun 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007coast.150..221k&link_type=abstract

Communications in Astroseismology, Vol. 150, p.221

Physics

4

Scientific paper

After the Sun, the stars with the most detected pulsation modes are the white dwarfs. From the hot PG 1159 stars, through the pulsating DBs near 25000 K, to the more numerous DAVs around 12000 K, we now know of around 150 pulsating white dwarf stars, but they are still all in the nearby thin disk of our Galaxy. As the white dwarf models are simple and the details of the initial conditions are washed out when the stars reach the DBV and the DAV instability strips, seismology does give structural information with detail and precision, and even allows us to measure evolutionary timescales. Taking into account that around 97% of all stars evolve to white dwarfs, we measure the records of Galactic history, which is a powerful tool to study physics at high energies.

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