The transit light curve project. V. System parameters and stellar rotation period of HD 189733

被引：141

作者：

Winn, Joshua N.

Holman, Matthew J.

Henry, Gregory W.

Roussanova, Anna

Enya, Keigo

Yoshii, Yuzuru

Shporer, Avi

Mazeh, Tsevi

Johnson, John Asher

Narita, Norio

Suto, Yasushi

机构：

[1] MIT, Dept Phys, Cambridge, MA 02139 USA

[2] MIT, Kavli Inst Astrophys & Space Res, Cambridge, MA 02139 USA

[3] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

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

[5] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan

[6] Univ Tokyo, Sch Sci, Inst Astron, Mitaka, Tokyo 1810015, Japan

[7] Univ Tokyo, Sch Sci, Res Ctr Early Universe, Bunkyo Ku, Tokyo 1130033, Japan

[8] Tel Aviv Univ, Raymond & Beverly Sackler Fac Exact Sci, Wise Observ, IL-69978 Tel Aviv, Israel

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

[10] Univ Tokyo, Dept Phys, Tokyo 1130033, Japan

来源：

ASTRONOMICAL JOURNAL | 2007年 / 133卷 / 04期

关键词：

planetary systems; planetary systems : formation; stars : individual (HD 189733); stars : rotation;

D O I：

10.1086/512159

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present photometry of HD 189733 during eight transits of its close-in giant planet, and out-of-transit photometry spanning 2 yr. Using the transit photometry, we determine the stellar and planetary radii and the photometric ephemeris. Outside of transits, there are quasi-periodic flux variations with a 13.4 day period that we attribute to stellar rotation. In combination with previous results, we derive upper limits on the orbital eccentricity and on the true angle between the stellar rotation axis and planetary orbit (as opposed to the angle between the projections of those axes on the sky).

引用

页码：1828 / 1835

页数：8

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