Composite spectra Paper 16: HR 3222, a 2.5-yr binary with a metallic-line secondary

Details Composite spectra Paper 16: HR 3222, a 2.5-yr binary with a metallic-line secondary Composite spectra Paper 16: HR 3222, a 2.5-yr binary with a metallic-line secondary

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010mnras.402.1675g&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 402, Issue 3, pp. 1675-1684.

Astronomy and Astrophysics

Astronomy

Binaries: Spectroscopic, Stars: Individual: Hr 3222

Scientific paper

HR 3222 is a late-type giant star that has long been known as a spectroscopic binary. A single-lined orbit is readily found; it has a period of 955 d and an eccentricity of 0.33. The spectrum is noticeably composite, especially at short wavelengths; radial-velocity traces show a weak secondary dip that is broadened by a rotational velocity of 18 kms-1. We employ high-dispersion spectroscopy and uncover the secondary spectrum by subtracting from the observed composite one the spectrum of the K0 giant β Gem; the residue is a metallic-line star of type kA8hF2mF4, and measurements of its wavelength displacement from the primary spectrum give a more reliable radial velocity for that component than seems achievable from radial-velocity traces. The mass ratio is 1.20 +/- 0.03. The stars can both be placed on an evolutionary track corresponding to an age of 1.4 Gyr. The fact that the secondary component is a metallic-line star cannot be attributed to the result of tidal effects in this binary system.

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