Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6727w&link_type=abstract
HST Proposal ID #6727
Astronomy and Astrophysics
Astronomy
Hst Proposal Id #6727 Hot Stars
Scientific paper
An improved understanding of the white dwarf stars has a greatpotential in both physics and astronomy. Determination of thebasic physical parameters of the white dwarf stars will helpus realize that potential; asteroseismology is the key. We canuse asteroseismology to constrain the stellar structure andevolution, including the stellar mass and even the stellardistance if we can determine the pulsation indices (k,ell,m)of the non-radial g-mode light variations observed in compactpulsators. We made tentative identifications for GD 358 usinga method based on the frequency distribution of consecutiveradial overtone g-modes. A comparison of the amplitude of thepulsation between the optical and the UV proves to be anotherindependent method to identify the pulsation indices. Ourproject is to apply both methods to GD358. For the HSTobservations we will use the FOS blue digicon with the G160Lgrating in RAPID readout mode to obtain time-resolvedspectrophotometry to measure the ultraviolet amplitudes. Wewill measure the optical amplitude with time seriesphotometry. By observing the DBV star GD 358 with the HST, wehave a unique opportunity to cross-calibrate the two methods --- essential if we are to have confidence in the conclusionsdrawn from either method. The future of asteroseismology ofwhite dwarf stars hinges on these observations; they will notbe possible after Feb 97, with the replacement of FOS.
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