Other
Scientific paper
Mar 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...278..754k&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 278, March 15, 1984, p. 754-760.
Other
24
Stellar Oscillations, White Dwarf Stars, Astronomical Photometry, Light Curve, Power Spectra
Scientific paper
The ZZ Ceti star GD 385 has been observed with a high-speed two-channel photometer on the 2.1 and 0.9 m telescopes of McDonald Observatory. The light curve of the star was composed of three separate pulsations during the 1982 observing season, with two close pulsations of period near 256.2 s and semiamplitudes of 1.1 percent, and another pulsation of 128.1 s with a semiamplitude of 0.4 percent. The pulsations reported by Fontaine et al. (1980) and Vauclair and Bonazzola (1981) were not found during 62.5 hr of observation from 1979 to 1982. The maximum semiamplitude of the 256.2 s variation changed from 3.5 percent during 1978-1981 to 2.2 percent during 1982. The change could be caused by beating of two or more extremely close pulsation frequencies with a beat period of a few years, or by a true change of the observed pulsations originating in nonlinear effects.
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