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Mode Identification of BPM 37093 with the HST
Kepler, S. O.; Montgomery, M. H.; Winget, D. E. +3 more
Theoretical calculations indicate that the massive pulsating white dwarf BPM 37093 has a crystallized interior (Winget et al. 1997, Kanaan 1996, Montgomery 1998). Crystallization was predicted theoretically about 40 years ago (Abrisokov 1961, Kirshnitz 1960; Salpeter 1961), but in spite of its importance in astrophysics, there is no direct observa…
Mode Identification in Pulsating White Dwarfs Using the HST
Kepler, S. O.; Clemens, J. C.; Jiang, X. J. +3 more
We obtained time-resolved ultraviolet spectroscopy for the pulsating DA stars G 226-29 and G 185-32 and for the pulsating DBV star PG 1351+489 with the Hubble Space Telescope Faint Object Spectrograph, to compare the ultraviolet to the optical pulsation amplitudes. We find that for essentially all observed pulsation modes the amplitude rises to th…
MASCOT: A Multi-Wavelength All-Sky Catalogue for Observations With Ground- and Space-Based Telescopes
Pasian, F.; Dluzhnevskaya, O.; Malkov, O.
New powerful observational techniques require a careful planning of observing programs. These requirements will be met within the proposed project MASCOT, A Multi-wavelength All-Sky Catalogue for Observations with ground- and space-based Telescopes. MASCOT will be based on the world's largest digitized all-sky survey containing astrometric and pho…
An IUE Archival Study of the White Dwarf Temperature Variation in the Dwarf Nova WZ Sagittae
Sion, E. M.; Cheng, F. H.; Slevinsky, R. J. +2 more
The IUE archive offers a series of far UV spectra of ultra-short period dwarf nova WZ Sge over a long time baseline and hence the opportunity to monitor the ongoing accretion, the cooling of the white dwarf and temporal variations in the line spectra. We have carried out a quantitative analysis of these spectra including model atmosphere simulatio…
The Temperature of the Hot DB GD 190
Provencal, J. L.; Shipman, H. L.
We are currently in the midst of an investigation of hydrogen and carbon abundances in hot DB white dwarfs. Our HST UV spectra give evidence that hot DBs contain traces of carbon which can be used to determine the temperatures of these objects. We present the results of our investigation of GD 190.