The California Planet Survey. II. A Saturn-Mass Planet Orbiting the M Dwarf Gl 649

被引：0

作者：

Johnson, John Asher ^{[1
]}

Howard, Andrew W. ^{[2
]}

Marcy, Geoffrey W. ^{[2
]}

Bowler, Brendan P. ^{[3
]}

Henry, Gregory W. ^{[4
]}

Fischer, Debra A. ^{[5
]}

Apps, Kevin ^{[6
]}

Isaacson, Howard ^{[2
]}

Wright, Jason T. ^{[7
]}

机构：

[1] CALTECH, Dept Astrophys, Pasadena, CA 91125 USA

[2] Univ Calif Berkeley, Dept Astron, Berkeley, CA 94720 USA

[3] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA

[4] Tennessee State Univ, Ctr Excellence Informat Syst, Nashville, TN 37209 USA

[5] Yale Univ, Dept Astron, New Haven, CT 06520 USA

[6] Cheyne Walk Observ, Horley RH6 7LR, Surrey, England

[7] Penn State Univ, University Pk, PA 16802 USA

来源：

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF THE PACIFIC | 2010年 / 122卷 / 888期

关键词：

CHROMOSPHERICALLY ACTIVE STARS; SHORT-PERIOD PLANETS; EXTRA-SOLAR PLANETS; SUN-LIKE STARS; RADIAL-VELOCITY; DETERMINISTIC MODEL; HARPS SEARCH; NEARBY STAR; NEPTUNE; DETECTABILITY;

D O I：

暂无

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We report precise Doppler measurements of the nearby (d = 10.34 pc) M dwarf Gl 649 that reveal the presence of a planet with a minimum mass M(P) sin i = 0.328 M(Jup) in an eccentric (e = 0.30), 598.3 day orbit. Our photometric monitoring reveals Gl 649 to be a new variable star with brightness changes on both rotational and decadal timescales. However, neither of these timescales are consistent with the 600 day Doppler signal and so provide strong support for planetary reflex motion as the best interpretation of the observed radial velocity variations. Gl 649b is only the seventh Doppler-detected giant planet around an M dwarf. The properties of the planet and host-star therefore contribute significant information to our knowledge of planet formation around low-mass stars. We revise and refine the occurrence rate of giant planets around M dwarfs based on the California Planet Survey sample of low-mass stars (M(star) < 0.6 M(circle dot)). We find that f = 3.4(-0.9)(+2.2)% of stars with M(star) < 0.6 M(circle dot) harbor planets with M(P) sin i > 0.3 M(Jup) and a < 2.5 AU. When we restrict our analysis to metal-rich stars with [Fe/H] > +0.2, we find that the occurrence rate is 10.7(-4.2)(+5.9)%.

引用

页码：149 / 155

页数：7

共 28 条

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