TESTING THE PLANET-METALLICITY CORRELATION IN M-DWARFS WITH GEMINI GNIRS SPECTRA

被引：0

作者：

Hobson, M. J. ^{[1
,3
]}

Jofre, E. ^{[1
,2
,3
]}

Garcia, L. ^{[1
,3
]}

Petrucci, R. ^{[1
,2
,3
]}

Gomez, M. ^{[1
,2
,3
]}

机构：

[1] Observ Astron, Cordoba, Argentina

[2] Consejo Nacl Invest Cient & Tecn, Buenos Aires, DF, Argentina

[3] Observ Astronm Crdoba, Laprida 854, Crdoba, Argentina

来源：

REVISTA MEXICANA DE ASTRONOMIA Y ASTROFISICA | 2018年 / 54卷 / 01期

关键词：

methods: observational; planets and satellites: general; stars: abundances; techniques: spectroscopic; EXTRA-SOLAR PLANETS; M-CIRCLE-PLUS; CARNEGIE EXOPLANET SURVEY; SATURN-MASS PLANET; HARPS SEARCH; STELLAR PARAMETERS; GIANT PLANET; STARS; I; ACCRETION;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

While the planet-metallicity correlation for FGK main-sequence stars hosting giant planets is well established, it is less clear for NI-dwarf stars. We determine stellar parameters and metallicities for 16 M-dwarf stars, 11 of which host planets, with near-infrared spectra from the Gemini Near-Infrared Spectrograph (GNIRS). We find that M-dwark with planets are preferentially metal rich compared to those without planets. This result is supported by the analysis of a larger catalogue of 18 M stars with planets and 213 M stars without known planets (Terrier et al. 2015), and demonstrates the utility of GNIRS spectra to obtain reliable stellar parameters of NI stars. We also find that NI dwarfs with giant planets are preferentially more metallic than those with low-mass planets, in agreement with previous results for solar-type stars. These results favor the core accretion model of planetary formation.

引用

页码：65 / 84

页数：20

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