Analysis of selected Kepler Mission planetary light curves

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dc.contributor.authorRhodes, M. D.
dc.contributor.authorBudding, E.
dc.date.accessioned2025-01-27T20:29:38Z
dc.date.available2025-01-27T20:29:38Z
dc.date.issued2014
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractWe have modified the graphical user interfaced close binary system analysis program CurveFit to the form WinKepler and applied it to 16 representative planetary candidate light curves found in the NASA Exoplanet Archive (NEA) at the Caltech website , with an aim to compare different analytical approaches. WinKepler has parameter options for a realistic physical model, including gravity-brightening and structural parameters derived from the relevant Radau equation. We tested our best-fitting parameter-sets for formal determinacy and adequacy. A primary aim is to compare our parameters with those listed in the NEA. Although there are trends of agreement, small differences in the main parameter values are found in some cases, and there may be some relative bias towards a 90(a similar to) value for the NEA inclinations. These are assessed against realistic error estimates. Photometric variability from causes other than planetary transits affects at least 6 of the data-sets studied; with small pulsational behaviour found in 3 of those. For the false positive KOI 4.01, we found that the eclipses could be modelled by a faint background classical Algol as effectively as by a transiting exoplanet. Our empirical checks of limb-darkening, in the cases of KOI 1.01 and 12.01, revealed that the assigned stellar temperatures are probably incorrect. For KOI 13.01, our empirical mass-ratio differs by about 7 % from that of Mislis and Hodgkin (Mon. Not. R. Astron. Soc. 422:1512, 2012), who neglected structural effects and higher order terms in the tidal distortion. Such detailed parameter evaluation, additional to the usual main geometric ones, provides an additional objective for this work.
dc.description.sponsorshipRASNZ's Kingdon Tomlinson Fund
dc.description.sponsorshipM.R. and E. B. attended the Carl Sagan Summer Workshop at the California Institute of Technology, Pasadena during the week July 22-29, 2012, which was a considerable stimulation for much of the work in this paper. The meeting was organized by the NASA Exoplanet Science Institute (NExScI), who supported EB's registration and accommodation. EB appreciates also the RASNZ's Kingdon Tomlinson Fund for its partial support of his travel costs.
dc.identifier.doi10.1007/s10509-014-1822-1
dc.identifier.endpage471
dc.identifier.issn0004-640X
dc.identifier.issn1572-946X
dc.identifier.issue2
dc.identifier.startpage451
dc.identifier.urihttps://doi.org/10.1007/s10509-014-1822-1
dc.identifier.urihttps://hdl.handle.net/20.500.12428/23001
dc.identifier.volume351
dc.identifier.wosWOS:000335449300008
dc.identifier.wosqualityQ2
dc.indekslendigikaynakWeb of Science
dc.language.isoen
dc.publisherSpringer
dc.relation.ispartofAstrophysics and Space Science
dc.relation.publicationcategoryinfo:eu-repo/semantics/openAccess
dc.rightsinfo:eu-repo/semantics/closedAccess
dc.snmzKA_WoS_20250125
dc.subjectStars-close binary
dc.subjectExoplanets
dc.subjectLight curve analysis
dc.titleAnalysis of selected Kepler Mission planetary light curves
dc.typeArticle

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