The light curve of the ZZ Ceti star G226-29

Details The light curve of the ZZ Ceti star G226-29 The light curve of the ZZ Ceti star G226-29

Aug 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...271..744k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 271, Aug. 15, 1983, p. 744-753.

Astronomy and Astrophysics

Astrophysics

38

Light Curve, Stellar Oscillations, Stellar Rotation, White Dwarf Stars, Angular Velocity, Power Spectra, Stellar Motions

Scientific paper

The light curve of the ZZ Ceti star G226-29 is decomposed into its component pulsations, using data from 65 hours of observations made during 1980-1982 on the 2.1, 0.9, and 0.8-m telescopes at McDonald Observatory with a high-speed two-channel photometer without filters. The amplitude and phase data of the 109-sec pulsation are presented in a table. It is determined that the variation of the star is a closely spaced triplet of pulsations with periods of 109.08648, 109.27929, and 109.47242 sec and fractional semiamplitudes of 0.0031, 0.0011, and 0.0031. It is proposed that these are g-mode pulsations, characterized by identical k and l pulsation indices but different values of m, caused by a rotational velocity of the star in the 1-2-km/sec range. It is pointed out that k, l, m, and the rotational velocity can at present only be estimated from theoretical models, since the mass and pulsation-axis inclination of G226-29 are not known.

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