The pulsating central star of the planetary nebula Kohoutek 1-16

Details The pulsating central star of the planetary nebula Kohoutek 1-16 The pulsating central star of the planetary nebula Kohoutek 1-16

Feb 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...277..211g&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 277, Feb. 1, 1984, p. 211-215. Research supported by the Donaghey Foundatio

Astronomy and Astrophysics

Astrophysics

71

Nonstabilized Oscillation, Planetary Nebulae, Stellar Oscillations, Variable Stars, White Dwarf Stars, Astronomical Photometry, Light Curve, Stellar Evolution, Stellar Spectrophotometry, Ubv Spectra

Scientific paper

High-speed photometry of the central star of the planetary nebula Kohoutek 1-16 shows it to be a low-amplitude pulsating variable. The dominant period is 28.3 minutes, with a semiamplitude that is usually about 0.01 mag. However, several additional periods sometimes appear in power spectra computed from light curves, and on two occasions a rapid drop into, or emergence from, a state in which no detectable variations were present was observed. Such 'mode switching' is typical of some of the ZZ Ceti-type white dwarf nonradial pulsators, but, at effective temperatures higher than 80,000 K, K1-16 is much too hot to be a ZZ Ceti variable. Spectroscopically and photometrically, the central star of K1-16 closely resembles the previously known hot pulsator PG 1159-035; these two objects represent a new pulsational instability mechanism for extremely hot degenerate or predegenerate stars. It is predicted that the evolutionary contraction of K1-16 will lead to a period decrease so rapid that it should be detectable over an interval of about 2 yr.

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