Physics
Scientific paper
Jan 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004esasp.538..141s&link_type=abstract
In: Second Eddington Workshop: Stellar structure and habitable planet finding, 9 - 11 April 2003, Palermo, Italy. Edited by F. F
Physics
2
Stars: White Dwarfs, B Subdwarfs, Stars: Pulsation, Stars: Structure, Stars: Evolution
Scientific paper
The technical characteristics of the Eddington mission allow to obtain crucial results in the field of white dwarf (WD) and subdwarf B (sdB) seismology. The huge improvement of the Eddington data, with respect to present ground-based multi-site campaigns, relies on many factors: longer runs (from 2-3 weeks to months/years), much cleaner spectral windows (coverage of 90% or more), higher photometric accuracy, better homogeneity of the data set. For all these reasons we can expect that Eddington observations on WD/sdB pulsators would have an important impact on many of the following topics: pulsational models (better adiabatic and nonadiabatic models and more accurate/robust seismic results), WD/sdB structure (e.g. stellar mass, WD transition zones, C/O ratio in WD cores and 12C(α γ)16O reaction rate), WD/sdB evolution (e.g. previous evolution of the sdB stars, still unclear; P. and evolutionary time scales for the instability strips), WD cooling (ratio of crystallized matter in the core) and WD luminosity function.
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