HD147506b: A Super-Massive Planet in an Eccentric Orbit Transiting a Bright Star

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dc.creatorBakos, G. A.
dc.creatorKovacs, G.
dc.creatorTorres, G.
dc.creatorFischer, D. A.
dc.creatorLatham, D. W.
dc.creatorNoyes, R. W.
dc.creatorSasselov, D. D.
dc.creatorMazeh, T.
dc.creatorShporer, A.
dc.creatorButler, R. P.
dc.creatorStefanik, R. P.
dc.creatorFernandez, J. M.
dc.creatorSozzetti, A.
dc.creatorPal, A.
dc.creatorJohnson, J.
dc.creatorMarcy, G. W.
dc.creatorWinn, J.
dc.creatorSipocz, B.
dc.creatorLazar, J.
dc.creatorPapp, I.
dc.creatorSari, P.
dc.date2007-05-01
dc.date2007-07-03
dc.date.accessioned2026-07-07T11:41:04Z
dc.date.available2026-07-07T11:41:04Z
dc.descriptionWe report the discovery of a massive (Mp = 9.04+/-0.50 MJup) planet transiting the bright (V = 8.7) F8 star HD 147506, with an orbital period of 5.63341+/-0.00013 days and an eccentricity of e = 0.520+/-0.010. From the transit light curve we determine that the radius of the planet is Rp = 0.982^{+0.038}_{0.105}RJup. HD 147506b (also coined HAT-P-2b) has a mass about 9 times the average mass of previously-known transiting exoplanets, and a density of rho = 11.9 g cm-3, greater than that of rocky planets like the Earth. Its mass and radius are marginally consistent with theories of structure of massive giant planets composed of pure H and He, and may require a large (~100 Earth mass) core to account for. The high eccentricity causes a 9-fold variation of insolation of the planet between peri- and apastron. Using follow-up photometry, we find that the center of transit is Tmid = 2,454,212.8559 +/- 0.0007 (HJD), and the transit duration is 0.177 +/-0.002 d.
dc.descriptionRevised version sent to ApJ
dc.identifierhttps://arxiv.org/abs/0705.0126
dc.identifierhttp://arxiv.org/abs/0705.0126
dc.identifierAstrophys.J.670:826-832,2007
dc.identifierdoi:10.1086/521866
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/200408
dc.subjectAstrophysics
dc.titleHD147506b: A Super-Massive Planet in an Eccentric Orbit Transiting a Bright Star
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