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dc.contributor.authorSozzetti, Alessandro
dc.contributor.authorTorres, Guillermo
dc.contributor.authorCharbonneau, David
dc.contributor.authorLatham, David W.
dc.contributor.authorHolman, Matthew J.
dc.contributor.authorWinn, Joshua N.
dc.contributor.authorLaird, John B.
dc.contributor.authorO’Donovan, Francis T.
dc.date.accessioned2019-09-24T17:24:54Z
dc.date.issued2007
dc.identifier.citationSozzetti, Alessandro, Guillermo Torres, David Charbonneau, David W. Latham, Matthew J. Holman, Joshua N. Winn, John B. Laird, and Francis T. O’Donovan. 2007. “Improving Stellar and Planetary Parameters of Transiting Planet Systems: The Case of TrES‐2.” The Astrophysical Journal 664 (2): 1190–98. https://doi.org/10.1086/519214.
dc.identifier.issn0004-637X
dc.identifier.issn1538-4357
dc.identifier.urihttp://nrs.harvard.edu/urn-3:HUL.InstRepos:41397384*
dc.description.abstractWe report on a spectroscopic determination of the atmospheric parameters and chemical abundance of the parent star of the recently discovered transiting planet TrES-2. A detailed LTE analysis of a set of Fe (I) and Fe (II) lines from our Keck spectra yields T-eff = 5850 +/- 50 K, log g = 4.4 +/- 0: 1, and [Fe/H]= -0.15 +/- 0.10. Several independent checks (e.g., additional spectroscopy, line-depth ratios) confirm the reliability of our spectroscopic T-eff estimate. The mass and radius of the star, needed to determine the properties of the planet, are traditionally inferred by comparison with stellar evolution models using T-eff and some measure of the stellar luminosity, such as the spectroscopic surface gravity. We apply here a new method in which we use instead of log g the normalized separation a/R-* ( related to the stellar density), directly measurabele from the light curves of transiting planets with much greater precision. With the a/R-* value from the light-curve analysis of Holman and coworkers and our T-eff estimate, we obtain M-* = 0.980 +/- 0.062 M-circle dot and R-* = 1.000(-0.033) (+0.036) R-circle dot, and an evolutionary age of 5.1(-2.3)(+2.7) Gyr, in good agreement with other constraints ( Ca (II) H and K line cores, lithium abundance, and rotation). The new stellar parameters yield improved values for the planetary mass and radius of M-p = 1.198 +/- 0: 053 M-J and Rp = 1.220(- 0.042)(+0.045) R-J, confirming that TrES-2 is the most massive among the currently known nearby (d less than or similar to 300 pc) transiting hot Jupiters. The surface gravity of the planet, log g(p) = 3.299 +/- 0.016, can be derived independently of the knowledge of the stellar parameters (i.e., directly from observations), and with a very high precision rivaling that of the best known double-lined eclipsing binaries.
dc.language.isoen_US
dc.publisherAmerican Astronomical Society
dash.licenseLAA
dc.titleImproving Stellar and Planetary Parameters of Transiting Planet Systems: The Case of TrES‐2
dc.typeJournal Article
dc.description.versionVersion of Record
dc.relation.journalThe Astrophysical Journal
dash.depositing.authorCharbonneau, David::a0e3ca75d3fb8511f2f554ed69428108::600
dc.date.available2019-09-24T17:24:54Z
dash.workflow.comments1Science Serial ID 97580
dc.identifier.doi10.1086/519214
dash.source.volume664;2
dash.source.page1190-1198


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