High-Resolution Spectroscopy of the Planetary Host HD 13189: Highly-Evolved and Metal-Poor

Details High-Resolution Spectroscopy of the Planetary Host HD 13189: Highly-Evolved and Metal-Poor High-Resolution Spectroscopy of the Planetary Host HD 13189: Highly-Evolved and Metal-Poor

2005-09-10

arxiv.org/abs/astro-ph/0509270v1

Astrophys.J.632:L131-L134,2005

Astronomy and Astrophysics

Astrophysics

14 pages, 2 figures; Accepted for publication in ApJ Letters

Scientific paper

10.1086/497988

We report on the abundances of 13 elements in the planetary host HD 13189, a massive giant star. Abundances are found to be sub-solar, with [Fe/H] = -0.58 +/- 0.04$; HD 13189 is one of the most metal-poor planetary hosts yet discovered. Abundance ratios relative to Fe show no peculiarities with respect to random field stars. A census of metallicities of the seven currently known planet-harboring giants results in a distribution that is more metal-poor than the well-known metal-rich distribution of main sequence (MS) planetary hosts. This finding is discussed in terms of accretion of H-depleted material, one of the possible mechanisms responsible for the high-metallicity distribution of MS stars with planets. We estimate the mass of the HD 13189 progenitor to be 3.5 M_sun but cannot constrain this value to better than 2-6 M_sun. A stellar mass of 3.5 M_sun implies a planetary mass of m sin i = 14.0 +/- 0.8 M_J, placing the companion at the planet/brown dwarf boundary. Given its physical characteristics, the HD 13189 system is potentially unique among planetary systems, and its continued investigation should provide invaluable data to extrasolar planetary research.

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