Analysis of the exoplanet containing system Kepler-91

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dc.authoridPuskullu, Caglar/0000-0001-9213-0969
dc.contributor.authorBudding, E.
dc.contributor.authorPuskullu, C.
dc.contributor.authorRhodes, M. D.
dc.contributor.authorDemircan, O.
dc.contributor.authorErdem, A.
dc.date.accessioned2025-01-27T20:51:56Z
dc.date.available2025-01-27T20:51:56Z
dc.date.issued2016
dc.departmentÇanakkale Onsekiz Mart Üniversitesi
dc.description.abstractWe have applied the graphical user interfaced close binary system analysis program WINFITTER to an intensive study of Kepler-91 using all the available photometry from the NASA Exoplanet Archive (NEA) at the Caltech website: http://exoplanetarchive.ipac.caltech.edu. Our fitting function for the tidal distortion derives from the relevant Radau equation and includes terms up to the fifth power of the fractional radius. This results in a systematic improvement in the mass ratio estimation over that of Lillo-Box et al. (Astron. Astrophys. 562:A109, 2014a) and our derived value for the mass ratio is in close agreement with that inferred from recent high-resolution spectroscopic data. It is clear that the data analysis in terms of simply an eclipsing binary system is compromised by the presence of significant other causes of light variation, in particular non-radial pulsations. We apply a low-frequency filtering procedure to separate out some of this additional light variation. Whilst the derived eccentricity appears then reduced, an eccentric effect remains in the light curve. We consider how this may be maintained in spite of likely frictional effects operating over a long time. There are also indications that could be associated with Trojan or other period-resonant mass concentrations. Suggestions of a possible secular period variation are briefly discussed.
dc.description.sponsorshipTUBITAK (Scientific and Technological Research Council of Turkey) [113F353]
dc.description.sponsorshipThis research has been supported by TUBITAK (Scientific and Technological Research Council of Turkey) under Grant No. 113F353. The help of colleagues in the Physics Dept., COMU, including Dr. M. Tuysuz, is acknowledged.
dc.identifier.doi10.1007/s10509-015-2564-4
dc.identifier.issn0004-640X
dc.identifier.issn1572-946X
dc.identifier.issue1
dc.identifier.urihttps://doi.org/10.1007/s10509-015-2564-4
dc.identifier.urihttps://hdl.handle.net/20.500.12428/25592
dc.identifier.volume361
dc.identifier.wosWOS:000367516500017
dc.identifier.wosqualityQ3
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.subjectStellar dynamics
dc.subjectExoplanets
dc.subjectLight curve analysis
dc.titleAnalysis of the exoplanet containing system Kepler-91
dc.typeArticle

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