V471 Tauri - A three-body orbit

Details V471 Tauri - A three-body orbit V471 Tauri - A three-body orbit

Jan 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...300..785b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 300, Jan. 15, 1986, p. 785-787.

Astronomy and Astrophysics

Astrophysics

15

Eclipsing Binary Stars, Stellar Orbits, Three Body Problem, White Dwarf Stars, Orbital Elements, Stellar Models

Scientific paper

A model is proposed for V471 Tauri to explain the apparent period changes currently assigned to this K2 V + white dwarf eclipsing system. It is shown that the light-time effects of a model in which the eclipsing pair orbits with an as yet undetected third body can fit the observed eclipse timings. The model features a constant period P1 = 0.52118334 days for the eclipsing pair, with the third-body orbit of period P0 = 24.6 yr, eccentricity e = 0.36, and probably of low inclination. Present observations imply an upper limit to the third-body mass of about 0.8 solar mass. Possibilities of detecting this component by IR observations, visual inspection, or speckle interferometry are discussed.

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