Seismology of White Dwarfs: The ZZ Ceti Stars

Details Seismology of White Dwarfs: The ZZ Ceti Stars Seismology of White Dwarfs: The ZZ Ceti Stars

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1170..616c&link_type=abstract

STELLAR PULSATION: CHALLENGES FOR THEORY AND OBSERVATION: Proceedings of the International Conference. AIP Conference Proceedin

Computer Science

Pulsations, Oscillations, And Stellar Seismology, Cepheids, Faint Blue Stars, White Dwarfs, Degenerate Stars, Nuclei Of Planetary Nebulae

Scientific paper

We calculate an extensive adiabatic model grid for pulsating white dwarfs with H dominated atmospheres, the ZZ Ceti stars. We developed a new approach for asteroseismology, using the relative observed amplitudes as weights, and compared the computed modes with the observed ones for the class of ZZ Ceti stars. We measure the H layer mass for 83 stars and found an average of MH/M* = 10-6.3, which is thinner than the predicted value of MH/M* = 10-4. Our results indicate that the stars lose more mass during their evolution than previously expected.

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