Observations and Orbital Analysis of the Giant White Dwarf Binary System HR 5692

Details Observations and Orbital Analysis of the Giant White Dwarf Binary System HR 5692 Observations and Orbital Analysis of the Giant White Dwarf Binary System HR 5692

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aj....141..144s&link_type=abstract

The Astronomical Journal, Volume 141, Issue 5, article id. 144 (2011).

Astronomy and Astrophysics

Astronomy

Binaries: General, Methods: Data Analysis, Stars: Individual: Hr 5692, Techniques: Spectroscopic, White Dwarfs

Scientific paper

We report spectroscopic observations of the red giant star HR 5692, previously known to be a binary system both from other spectroscopic work and from deviations in the astrometric motion detected by the Hipparcos satellite. Earlier International Ultraviolet Explorer (IUE) observations had shown the presence of a hot white dwarf companion to the giant primary. We have combined our radial velocity observations with other existing measurements and with the Hipparcos intermediate astrometric data to determine a complete astrometric-spectroscopic orbital solution, providing the inclination angle for the first time. We also determine an improved parallax for the system of 10.12 ± 0.67 mas. We derive the physical properties of the primary, and with an estimate of its mass from stellar evolution models (1.84 ± 0.40 M sun), we infer the mass of the white dwarf companion to be M WD = 0.59 ± 0.12 M sun. An analysis of an IUE white dwarf spectrum, using our parallax, yields T eff = 30, 400 ± 780 K, log g = 8.25 ± 0.15, and a mass M WD = 0.79 ± 0.09 M sun, in marginal agreement with the dynamical mass.

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