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Scientific paper
Jul 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6442k&link_type=abstract
HST Proposal ID #6442
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Hst Proposal Id #6442 Hot Stars
Scientific paper
The use of white dwarfs to test calculations of stellarevolution and to measure the history of star formation in thegalaxy depends on accurate knowledge of white dwarf interiors.White dwarf pulsations give the most detailed picture of theirinteriors, but the picture is correct only if the indices ofthe pulsation modes have been identified correctly. Standardmode identifications are based on matching observed pulsationperiods to periods determined from complex theoreticalcalculations. These methods are circular, prone to mis-identifications, and do not work for stars with few excitedpulsations. Other methods of mode identifications must be usedto avoid these problems. The wavelength dependence ofpulsation amplitudes at ultraviolet wavelengths gives anunambiguous and model-independent signature of the pulsationindex. We propose to measure the ultraviolet amplitudes of thepulsations in the pulsating DB white dwarf PG1351+489 withFOS. We choose this star because (1) There are no model-independent mode identifications for any DB white dwarf; (2)The observations will independently test earlier conclusionsthat some DB white dwarfs rotate differentially and have low-mass helium surface layers; (3) The observations will helpdefine the temperature scale for DB white dwarfs; (4)PG1346+489 has the simplest light curve of any pulsating DBwhite dwarf, so we avoid the serious complications caused bybeating between modes.
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