Observational limits on companions to G29-38

Details Observational limits on companions to G29-38 Observational limits on companions to G29-38

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...436..875k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 436, no. 2, p. 875-884

Mathematics

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21

Astronomical Photometry, Binary Stars, Brown Dwarf Stars, Power Spectra, Stellar Oscillations, Stellar Spectra, White Dwarf Stars, Photometers, Radial Velocity

Scientific paper

Recent interset in the variable (DAV) white dwarf G29-38 has been stirred by a tentative report of a radial velocity variation that may be due to an unseen companion. Earlier evidence for a brown dwarf in the system has come from an observed infrared excess in the star's spectrum. For asteroseismological reasons, we have accumulated more than five seasons of high-speed photometric data on the star. By measuring the phase of an isolated, stable frequency in the power spectrum, we show the measured variation is not due (at least in its entirety) to an orbital companion. Because any orbital radial velocity variation must result in a systematic phase variation, the data we present can be used to place stringent limits on the types of companions the system may contain.

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