Mathematics – Probability
Scientific paper
Aug 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003basbr..23q..97c&link_type=abstract
Boletim da Sociedade Astronômica Brasileira (ISSN 0101-3440), vol.23, no.1, p. 97-97
Mathematics
Probability
Scientific paper
White dwarf stars are the evolutive end of almost 98% of all stars; after mass loss during their lives, they will become white dwarf stars. Our work is to study the structure of the pulsating white dwarf stars, which present multi-period light variations, with periods around minutes, defining instability strips along their cooling sequence. We determine the effective temperature, surface gravity, mass, and pulsation spherical harmonic degrees for the star DAV G185-32, by means of the study of its light curve. We report on a weighted Fourier transform of the Whole Earth Telescope (WET) data. The weights, for each chunk data, are defined as the inverse of the our estimative of the noise, which is the square root of the average power. Improving the signal-to-noise ratio, we detected 24 periodicities in the light curve. The periodicity at 141.9 s does not behave like a normal mode, not fitting any model, and at 70.9 s is the shortest period pulsation ever detected in any pulsating white dwarf. We compared the change in amplitude with wavelength of the detected periodicities to calculate effective temperature and surface gravity. We also compared these values to other independent methods of determination: optical spectra, color indices, and ultraviolet spectra with parallax, using probability densities with normal distribution. The best solution from these determinations is Teff = 11 820+/-80 K, logg = 8.02+/-0.04, and M = 0.616+/-0.025M¤.
Castanheira Barbara G.
Kepler S. O.
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