A COMPARISON OF OBSERVATIONALLY DETERMINED RADII WITH THEORETICAL RADIUS PREDICTIONS FOR SH.pdfVIP

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A COMPARISON OF OBSERVATIONALLY DETERMINED RADII WITH THEORETICAL RADIUS PREDICTIONS FOR SH.pdf

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A COMPARISON OF OBSERVATIONALLY DETERMINED RADII WITH THEORETICAL RADIUS PREDICTIONS FOR SH

A COMPARISON OF OBSERVATIONALLY DETERMINED RADII WITH THEORETICAL RADIUS PREDICTIONS FOR SHORT-PERIOD TRANSITING EXTRASOLAR PLANETS Gregory Laughlin, 1 Aaron Wolf, 1 Tonny Vanmunster, 2 Peter Bodenheimer, 1 Debra Fischer, 3 Geoff Marcy, 4 Paul Butler, 5 and Steve Vogt 1 Receivved 2004 October 27; accepted 2004 November 17 ABSTRACT Two extrasolar planets, HD 209458b and TrES-1, are currently known to transit bright parent stars for which physical properties can be accurately determined. The two transiting planets have very similar masses and periods and hence invite detailed comparisons between their observed and theoretically predicted properties. In this paper, we carry out these comparisons. We first report photometric and spectroscopic follow-up observations of TrES-1, and we use these observations to obtain improved estimates for the planetary radius, Rpl ? (1:08 0:05)RJ, and the planetary mass, Mpl ? (0:729 0:036)MJ. We also confirm that the inclination estimate of the planetary orbit as i ? 88N2. These values agree with those obtained by Alonso et al. in their discovery paper, but the uncertainty in the planet radius has been improved as a result of both high-cadence photometry of two full transits and from independent radius determinations for the V ? 11:8 K0 V parent star. We derive estimates for the TrES-1 stellar parameters of R=R ? 0:83 0:03 (by combining independent estimates from stellar models, high-resolution spectra, and transit light curve fitting)M=M ? 0:87 0:05 (via fitting to evolutionary tracks), TeA ? 5214 23 K, ?Me=H ? 0:001 0:04, rotational velocity V sin (i) ? 1:08 0:3 km s1, log g ? 4:52 0:05 dex, log L=L ? 0:32, d ? 157 6 pc, and an age of ? 4 2 Gyr. These estimates of the physical properties of the system allow us to compute evolutionary models for the planet that result in a predicted radius of Rpl ? 1:05RJ for a model that contains an incompressible 20 M core and a radius Rpl ? 1:09RJ for a model without a