KEPLER-14b: A MASSIVE HOT JUPITER TRANSITING AN F STAR IN A CLOSE VISUAL BINARY

Journal Article · Tue Nov 01 00:00:00 EDT 2011 · Astrophysical Journal, Supplement Series

DOI:https://doi.org/10.1088/0067-0049/197/1/3· OSTI ID:21560323

Buchhave, Lars A ^[1]; Latham, David W; Carter, Joshua A; Desert, Jean-Michel; Torres, Guillermo; Adams, Elisabeth R; Charbonneau, David B; Dupree, Andrea K; Fressin, Francois ^[2]; Bryson, Stephen T; Howell, Steve B ^[3]; Ciardi, David R ^[4]; Kulesa, Craig ^[5]; Fischer, Debra A ^[6]; Gautier, Thomas N ^[7]; Gilliland, Ronald L ^[8]; Isaacson, Howard; Marcy, Geoffrey W ^[9]; Jenkins, Jon M ^[10]; McCarthy, Donald W ^[11]

---

1. Niels Bohr Institute, University of Copenhagen, DK-2100 Copenhagen (Denmark)
2. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138 (United States)
3. NASA Ames Research Center, Moffett Field, CA 94035 (United States)
4. NASA Exoplanet Science Institute/California Institute of Technology, Pasadena, CA 91109 (United States)
5. Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721 (United States)
6. Department of Astronomy, Yale University, New Haven, CT 06511 (United States)
7. Jet Propulsion Laboratory/California Institute of Technology, Pasadena, CA 91109 (United States)
8. Space Telescope Science Institute, Baltimore, MD 21218 (United States)
9. Department of Astronomy, University of California, Berkeley, CA 94720 (United States)
10. SETI Institute/NASA Ames Research Center, Moffett Field, CA 94035 (United States)
11. Steward Observatory, University of Arizona, Tucson, AZ 85721 (United States)

We present the discovery of a hot Jupiter transiting an F star in a close visual (0.''3 sky projected angular separation) binary system. The dilution of the host star's light by the nearly equal magnitude stellar companion ({approx}0.5 mag fainter) significantly affects the derived planetary parameters, and if left uncorrected, leads to an underestimate of the radius and mass of the planet by 10% and 60%, respectively. Other published exoplanets, which have not been observed with high-resolution imaging, could similarly have unresolved stellar companions and thus have incorrectly derived planetary parameters. Kepler-14b (KOI-98) has a period of P = 6.790 days and, correcting for the dilution, has a mass of M{sub p} = 8.40{sup +0.35}{sub -0.34} M{sub J} and a radius of R{sub p} = 1.136{sup +0.073}{sub -0.054} R{sub J}, yielding a mean density of {rho}{sub p} = 7.1 {+-} 1.1 g cm{sup -3}.

• OSTI ID: 21560323
• Journal Information: Astrophysical Journal, Supplement Series, Vol. 197, Issue 1; Other Information: DOI: 10.1088/0067-0049/197/1/3; ISSN 0067-0049
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
JUPITER PLANET
PHOTOMETRY
STARS
PLANETS