HAT-P-14b: A 2.2 M_J Exoplanet Transiting a Bright F Star
| Autor: | Dimitar Sasselov, Brigitta Sipocz, G. W. Marcy, Debra A. Fischer, Mark E. Everett, Robert W. Noyes, Guillermo Torres, Géza Kovács, I. Papp, Gáspár Á. Bakos, John Asher Johnson, Pál Sári, Joel D. Hartman, David W. Latham, J. Lazar, G. A. Esquerdo, Andrew W. Howard, David M. Kipping, Robert P. Stefanik |
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| Jazyk: | angličtina |
| Rok vydání: | 2010 |
| Předmět: |
Physics
Orbital elements 010504 meteorology & atmospheric sciences Epoch (astronomy) Astronomy and Astrophysics Astrophysics Radius Effective temperature 01 natural sciences Exoplanet 13. Climate action Space and Planetary Science Planet 0103 physical sciences Transit (astronomy) 10. No inequality 010303 astronomy & astrophysics Jupiter mass 0105 earth and related environmental sciences |
| Popis: | We report the discovery of HAT-P-14b, a fairly massive transiting extrasolar planet orbiting the moderately bright star GSC 3086-00152 (V = 9.98), with a period of P = 4.627669 +/- 0.000005 days. The transit is close to grazing (impact parameter 0.891 +0.007/-0.008) and has a duration of 0.0912 +/- 0.0017 days, with a reference epoch of mid transit of Tc = 2454875.28938 +/- 0.00047 (BJD). The orbit is slightly eccentric (e = 0.107 +/- 0.013), and the orientation is such that occultations are unlikely to occur. The host star is a slightly evolved mid-F dwarf with a mass of 1.386 +/- 0.045 M(Sun), a radius of 1.468 +/- 0.054 R(Sun) effective temperature 6600 +/- 90 K, and a slightly metal-rich composition corresponding to [Fe/H] = +0.11 +/- 0.08. The planet has a mass of 2.232 +/- 0.059 M(Jup) and a radius of 1.150 +/- 0.052 R(Jup), implying a mean density of 1.82 +/- 0.24 g/cm3. Its radius is well reproduced by theoretical models for the 1.3 Gyr age of the system if the planet has a heavy-element fraction of about 50 M(Earth) (7% of its total mass). The brightness, near-grazing orientation, and other properties of HAT-P-14 make it a favorable transiting system to look for changes in the orbital elements or transit timing variations induced by a possible second planet, and also to place meaningful constraints on the presence of sub-Earth mass or Earth mass exomoons, by monitoring it for transit duration variations. |
| Databáze: | OpenAIRE |
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