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Title:
The Transit Light Curve Project. V. System Parameters and Stellar Rotation Period of HD 189733
Authors:
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
Affiliation:
AA(Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA ), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA ), AC(Center of Excellence in Information Systems, Tennessee State University, Nashville, TN 37209, USA ), AD(Department of Physics, and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA 02139, USA ), AE(Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa 229-8510, Japan ), AF(Institute of Astronomy, School of Science, University of Tokyo, Mitaka, Tokyo 181-0015, Japan ; Research Center for the Early Universe, School of Science, University of Tokyo, Bunkyo-ku, Tokyo 113-0033, Japan ), AG(Raymond and Beverly Sackler Faculty of Exact Sciences, Wise Observatory, Tel Aviv University, Tel Aviv 69978, Israel ), AH(Raymond and Beverly Sackler Faculty of Exact Sciences, Wise Observatory, Tel Aviv University, Tel Aviv 69978, Israel ), AI(Department of Astronomy, University of California, Berkeley, CA 94720, USA ), AJ(Department of Physics, University of Tokyo, Tokyo 113-0033, Japan), AK(Department of Physics, University of Tokyo, Tokyo 113-0033, Japan)
Publication:
The Astronomical Journal, Volume 133, Issue 4, pp. 1828-1835 (2007). (AJ Homepage)
Publication Date:
04/2007
Origin:
IOP
DOI:
10.1086/512159
Bibliographic Code:
2007AJ....133.1828W

Abstract

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).

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