TY - JOUR
T1 - HAT-P-7b
T2 - An extremely hot massive planet transiting a bright star in the Kepler field
AU - Pál, A.
AU - Bakos, G. Á
AU - Torres, G.
AU - Noyes, R. W.
AU - Latham, D. W.
AU - Kovács, Géza
AU - Marcy, G. W.
AU - Fischer, D. A.
AU - Butler, R. P.
AU - Sasselov, D. D.
AU - Sipocz, B.
AU - Esquerdo, G. A.
AU - Kovács, Gábor
AU - Stefanik, R.
AU - Lázár, J.
AU - Papp, I.
AU - Sári, P.
PY - 2008/6/20
Y1 - 2008/6/20
N2 - We report on the latest discovery of the HATNet project: a very hot giant planet orbiting a bright (V = 10.5) star with a small semimajor axis of a = 0.0377 ±0.0005 AU. Ephemeris for the system is P = 2.2047299 ±0.0000040 days, midtransit time E = 2,453,790.2593 ±0.0010 (BJD). Based on the available spectroscopic data on the host star and photometry of the system, the planet has a mass of Mp = 1.78-0.05 +0.08 MJ and radius of Rp = 1.36 -0.09+0.020 RJ. The parent star is a slightly evolved F6 star with M*= 1.47-0.05+0.08M ⊙R*, =1.840.11+0.23 R ⊙,Teff = 6350 ±80 K, and metallicity [Fe/H] = +0.26 ±0.08. The relatively hot and large host star, combined with the close orbit of the planet, yield a very high planetary irradiance of 4.71 -0.05+1.44 × 109 erg cm-2 s-1, which places the planet near the top of the pM class of irradiated planets as defined by Fortney et al. If as predicted by Fortney et al. the planet reradiates its absorbed energy before distributing it to the night side, the day-side temperature should be about 273012 K. Because the host star is quite bright, measurement of the secondary eclipse should be feasible for ground-based telescopes, providing a good opportunity to compare the predictions of current hot Jupiter atmospheric models with the observations. Moreover, the host star falls in the field of the upcoming Kepler mission; hence extensive space-borne follow-up, including not only primary transit and secondary eclipse observations but also asteroseismology, will be possible.
AB - We report on the latest discovery of the HATNet project: a very hot giant planet orbiting a bright (V = 10.5) star with a small semimajor axis of a = 0.0377 ±0.0005 AU. Ephemeris for the system is P = 2.2047299 ±0.0000040 days, midtransit time E = 2,453,790.2593 ±0.0010 (BJD). Based on the available spectroscopic data on the host star and photometry of the system, the planet has a mass of Mp = 1.78-0.05 +0.08 MJ and radius of Rp = 1.36 -0.09+0.020 RJ. The parent star is a slightly evolved F6 star with M*= 1.47-0.05+0.08M ⊙R*, =1.840.11+0.23 R ⊙,Teff = 6350 ±80 K, and metallicity [Fe/H] = +0.26 ±0.08. The relatively hot and large host star, combined with the close orbit of the planet, yield a very high planetary irradiance of 4.71 -0.05+1.44 × 109 erg cm-2 s-1, which places the planet near the top of the pM class of irradiated planets as defined by Fortney et al. If as predicted by Fortney et al. the planet reradiates its absorbed energy before distributing it to the night side, the day-side temperature should be about 273012 K. Because the host star is quite bright, measurement of the secondary eclipse should be feasible for ground-based telescopes, providing a good opportunity to compare the predictions of current hot Jupiter atmospheric models with the observations. Moreover, the host star falls in the field of the upcoming Kepler mission; hence extensive space-borne follow-up, including not only primary transit and secondary eclipse observations but also asteroseismology, will be possible.
KW - Planetary systems
KW - Stars: individual (GSC 03547-01402, HAT-P-7)
KW - Techniques: spectroscopic
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U2 - 10.1086/588010
DO - 10.1086/588010
M3 - Article
AN - SCOPUS:46249123766
SN - 0004-637X
VL - 680
SP - 1450
EP - 1456
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
ER -