Metal-Poor Spectroscopic Binary Studies

Details Metal-Poor Spectroscopic Binary Studies Metal-Poor Spectroscopic Binary Studies

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aas...198.6313b&link_type=abstract

American Astronomical Society, 198th AAS Meeting, #63.13; Bulletin of the American Astronomical Society, Vol. 33, p.882

Astronomy and Astrophysics

Astronomy

2

Scientific paper

For the past two years we have been observing a small sample of mildly metal-poor dwarf spectroscopic binaries using long-baseline interferometry with PTI, and high-resolution radial velocity studies with the Harvard-CfA Oakridge Observatory. Herein we present our first preliminary results on two systems: HD 195987 (G 209-25), a 57d period G-dwarf system with an [Fe/H] of -0.49, and HD 9939 (G 34-39), a 25d period K0 IV system with an [Fe/H] of -0.51. We place our mass and absolute magnitude determinations of the components in these binary systems on evolutionary models for metal-poor stars. HD 195987 is composed of a G9 V primary and a probable K5 V secondary. Because of the significant color difference, the Hipparcos mission was able to detect photocentric motion and estimate a photocentric orbit in this system. Based on our joint interferometric visibility/radial velocity physical orbit solution we find masses of 0.825 +/- 0.014 and 0.655 +/- 0.009 M&sun; for the primary and secondary component masses respectively. HD 9939 has a slightly evolved K0 IV primary component along with a probable G6 V secondary component. Our physical orbit solution yields mass determinations in this system of 1.080 +/- 0.029 and 0.842 +/- 0.020 M&sun; for the primary and secondary components respectively.

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