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Scientific paper
Jul 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001hst..prop.9159o&link_type=abstract
HST Proposal ID #9159
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Hst Proposal Id #9159 Hot Stars
Scientific paper
We propose to test a new method for identifying the spherical harmonic index of pulsation modes in variable white dwarfs, pre-white dwarfs, and central stars of planetary nebulae. Once the mode-indices are found for such stars, the observed periods can yield accurate measurements of mass, luminosity, rotation rate, magnetic field strength, and interior structure. Unfortunately, so far only a single star, PG1159-035, shows a pulsation spectrum rich enough for unambiguous identification of both ell=1 and ell=2 modes via its observed pattern of periods alone. Theory predicts that limb darkening should cause the amplitudes of ell=1 and 2 modes to vary differently with wavelength in the UV. However, previous UV observations directed at determining mode indices in DA white dwarfs show that the models must be calibrated before this method can prove truly useful. We therefore propose to measure amplitude versus wavelength for the 20 known ell=1 and 9 known ell=2 modes in PG1159-035 using the STIS FUV- MAMA. We will thus measure the limb-darkening law for pre- white dwarfs, calibrate models for future application to other post-AGB pulsators, and truly test a new observational tool of enormous potential.
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