期刊
ASTROPHYSICAL JOURNAL
卷 699, 期 2, 页码 933-937出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/699/2/933
关键词
planetary systems; stars: abundances; stars: late-type
资金
- NSF [AST-0702821]
Knowledge of the metallicities of M dwarfs rests predominantly on the photometric calibration of Bonfils and collaborators, which predicts that M dwarfs in the solar neighborhood, including those with known planets, are systematically metal poor compared to their higher-mass counterparts. We test this prediction using a volume-limited sample of low-mass stars, together with a subset of M dwarfs with high-metallicity, F, G, and K wide binary companions. We find that the Bonfils et al. photometric calibration systematically underestimates the metallicities of our high-metallicity M dwarfs by an average of 0.32 dex. We derive a new photometric metallicity calibration and show that M dwarfs with planets appear to be systematically metal rich, a result that is consistent with the metallicity distribution of FGK dwarfs with planets.
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