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dc.contributor.authorEnoch, B.
dc.contributor.authorCollier Cameron, A.
dc.contributor.authorParley, N.~R.
dc.contributor.authorHebb, L.
dc.date.accessioned2014-01-16T11:31:00Z
dc.date.available2014-01-16T11:31:00Z
dc.date.issued2010-06
dc.identifier.citationEnoch , B , Collier Cameron , A , Parley , N R & Hebb , L 2010 , ' An improved method for estimating the masses of stars with transiting planets ' , Astronomy & Astrophysics , vol. 516 , A33 . https://doi.org/10.1051/0004-6361/201014326en
dc.identifier.issn1432-0746
dc.identifier.otherPURE: 5849705
dc.identifier.otherPURE UUID: 4a9639ed-1149-48e2-a9ad-0c498adad25c
dc.identifier.otherBibtex: urn:18175f0ddc8e7b7c23e85c37fe1ddb8f
dc.identifier.otherScopus: 77957827731
dc.identifier.otherORCID: /0000-0002-8863-7828/work/58531425
dc.identifier.urihttps://hdl.handle.net/10023/4377
dc.description.abstractContext. To determine the physical parameters of a transiting planet and its host star from photometric and spectroscopic analysis, it is essential to independently measure the stellar mass. This is often achieved by the use of evolutionary tracks and isochrones, but the mass result is only as reliable as the models used. Aims. The recent paper by Torres et al. (2010, A&ARv, 18, 67) showed that accurate values for stellar masses and radii could be obtained from a calibration using Teff, log g and [Fe/H]. We investigate whether a similarly good calibration can be obtained by substituting log ρ – the fundamental parameter measured for the host star of a transiting planet – for log g, and apply this to star-exoplanet systems.Methods. We perform a polynomial fit to stellar binary data provided in Torres et al. (2010) to obtain the stellar mass and radius as functions of Teff, log ρ and [Fe/H], with uncertainties on the fit produced from a Monte Carlo analysis. We apply the resulting equations to measurements for seventeen SuperWASP host stars, and also demonstrate the application of the calibration in a Markov Chain Monte Carlo analysis to obtain accurate system parameters where spectroscopic estimates of effective stellar temperature and metallicity are available. Results. We show that the calibration using log ρ produces accurate values for the stellar masses and radii; we obtain masses and radii of the SuperWASP stars in good agreement with isochrone analysis results. We ascertain that the mass calibration is robust against uncertainties resulting from poor photometry, although a good estimate of stellar radius requires good-quality transit light curve to determine the duration of ingress and egress.
dc.format.extent5
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© 2010, ESO. A&A 516, A33 (2010). Reproduced with permission from the publishers.en
dc.subjectPlanetary systemsen
dc.subjectPhotometric analysisen
dc.subjectSpectroscopic analysisen
dc.subjectStellar massen
dc.subjectQB Astronomyen
dc.subject.lccQBen
dc.titleAn improved method for estimating the masses of stars with transiting planetsen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1051/0004-6361/201014326
dc.description.statusPeer revieweden
dc.identifier.grantnumberST G001987 1en
dc.identifier.grantnumberPP/F000065/1en


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