XO-3b: A massive planet in an eccentric orbit transiting an F5V star

被引：115
|
作者：
Johns-Krull, Christopher M. [1 ]
McCullough, Peter R. [2 ]
Burke, Christopher J. [2 ]
Valenti, Jeff A. [2 ]
Janes, K. A. [3 ]
Heasley, J. N. [4 ]
Prato, L. [5 ]
Bissinger, R. [6 ]
Fleenor, M. [7 ]
Foote, C. N. [8 ]
Garcia-Melendo, E. [9 ]
Gary, B. L. [10 ]
Howell, P. J. [3 ]
Mallia, F. [11 ]
Masi, G. [12 ]
Vanmunster, T. [13 ]
机构：
[1] Rice Univ, Dept Phys & Astron, Houston, TX 77005 USA
[2] Space Telescope Sci Inst, Baltimore, MD 21218 USA
[3] Boston Univ, Dept Astron, Boston, MA 02215 USA
[4] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA
[5] Lowell Observ, Flagstaff, AZ 86001 USA
[6] Racoon Run Observ, Pleasanton, CA 94566 USA
[7] Volunteer Observ, Knoxville, TN 37932 USA
[8] Vermillon Cliffs Observ, Kanab, UT 84741 USA
[9] Esteve Duran Observ, Barcelona 08553, Spain
[10] Hereford Arizona Observ, Hereford, AZ 85615 USA
[11] Campo Catino Astron Observ, Guarcino, FR, Italy
[12] Bellatrix Observ, I-03023 Ceccano, FR, Italy
[13] CBA Belgium Observ, B-3401 Landen, Belgium
来源：
ASTROPHYSICAL JOURNAL | 2008年 / 677卷 / 01期
关键词：
binaries : eclipsing; planetary systems; stars : individual (GSC 03727-01064); techniques : photometric; techniques : radial velocities;
D O I：
10.1086/528950
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We report the discovery of a massive planet (M-p sin i 13.02 +/- 0.64 M-J; total mass = 13.25 +/- 0.64 M-J), large (1.95 +/- 0.16 R-J) planet in a transiting, eccentric orbit (e = 0.260 +/- 0.017) around a 10th magnitude F5 V star in the constellation Camelopardalis. We designate the planet XO-3b and the star XO-3, also known as GSC 03727-01064. The orbital period of XO-3b is 3.1915426 +/- 0.00014 days. XO-3 lacks a trigonometric parallax; we estimate its distance to be 260 +/- 23 pc. The radius of XO-3 is 2.13 +/- 0.21 R-circle dot, its mass is 1.41 +/- 0.08 M-circle dot, its v sin i = 18.54 +/- 0.17 km s(-1), and its metallicity is Fe/H = -0.177 +/- 0.027. This system is unusual for a number of reasons. XO-3b is one of the most massive planets discovered around any star for which the orbital period is less than 10 days. The mass is near the deuterium-burning limit of 13 M-J, which is a proposed boundary between planets and brown dwarfs. Although Burrows et al. propose that formation in a disk or formation in the interstellar medium in a manner similar to stars is a more logical way to differentiate planets and brown dwarfs, our current observations are not adequate to address this distinction. XO-3b is also unusual in that its eccentricity is large given its relatively short orbital period. Both the planetary radius and the inclination are functions of the spectroscopically determined stellar radius. Analysis of the transit light curve of XO-3b suggests that the spectroscopically derived parameters may be overestimated. Though relatively noisy, the light curves favor a smaller radius in order to better match the steepness of the ingress and egress. The light curve fits imply a planetary radius of 1.25 +/- 0.15 R-J, which would correspond to a mass of 12.03 +/- 0.46 M-J. A precise trigonometric parallax measurement or a very accurate light curve is needed to resolve the uncertainty in the planetary mass and radius.
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收藏
页码：657 / 670
页数：14
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