Two-phase ultraviolet spectrophotometry of the pulsating white dwarf ZZ PISCIUM

Details Two-phase ultraviolet spectrophotometry of the pulsating white dwarf ZZ PISCIUM Two-phase ultraviolet spectrophotometry of the pulsating white dwarf ZZ PISCIUM

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...289..774h&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 289, Feb. 15, 1985, p. 774-781.

Astronomy and Astrophysics

Astrophysics

14

Iue, Stellar Oscillations, Stellar Spectrophotometry, Ultraviolet Spectra, White Dwarf Stars, Real Time Operation, Satellite-Borne Instruments, Stellar Atmospheres, Stellar Temperature

Scientific paper

Spectra of the pulsating white dwarf ZZ Psc (= G29-38) were obtained using the International Ultraviolet Explorer. By using a multiple-exposure technique in conjunction with simultaneous ground-based exposure-metering photometry, it was possible to obtain mean on-pulse and off-pulse spectra in the 1950-1310 A wavelength range. The ratio of the time-averaged on-pulse to off-pulse spectra is best fitted by a temperature variation that is in phase with the optical light variation. This result is consistent with the hypothesis that the observed variation is due to a high-order nonradial pulsation. Conventional ultraviolet spectra of ZZ Psc showed broad absorption features at 1390 and 1600 A. These features are also found in the spectra of the cool DA-type white dwarfs G226-29 and G67-23, and appear to increase in strength with decreasing temperature. A possible explanation for the 1600 A feature is absorption by the satellite band of resonance-broadened hydrogen Ly-alpha. Such absorption would also help explain a discrepancy between the observed pulsation amplitude shortward of 1650 A and the predicted amplitudes based on model atmospheres.

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