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dc.contributor.authorKane, Stephen R.
dc.contributor.authorWittenmyer, Robert A.
dc.contributor.authorHinkel, Natalie R.
dc.contributor.authorRoy, Arpita
dc.contributor.authorMahadevan, Suvrath
dc.contributor.authorDragomir, Diana
dc.contributor.authorMatthews, Jayme M.
dc.contributor.authorHenry, Gregory W.
dc.contributor.authorChakraborty, Abhijit
dc.contributor.authorBoyajian, Tabetha S.
dc.contributor.authorWright, Jason T.
dc.contributor.authorCiardi, David R.
dc.contributor.authorFischer, Debra A.
dc.contributor.authorButler, R. Paul
dc.contributor.authorTinney, C. G.
dc.contributor.authorCarter, Brad D.
dc.contributor.authorJones, Hugh
dc.contributor.authorBailey, Jeremy
dc.contributor.authorO'Toole, Simon J.
dc.date.accessioned2016-11-08T17:43:24Z
dc.date.available2016-11-08T17:43:24Z
dc.date.issued2016-04-11
dc.identifier.citationKane , S R , Wittenmyer , R A , Hinkel , N R , Roy , A , Mahadevan , S , Dragomir , D , Matthews , J M , Henry , G W , Chakraborty , A , Boyajian , T S , Wright , J T , Ciardi , D R , Fischer , D A , Butler , R P , Tinney , C G , Carter , B D , Jones , H , Bailey , J & O'Toole , S J 2016 , ' Evidence for Reflected Light from the Most Eccentric Exoplanet Known ' , The Astrophysical Journal , vol. 821 , pp. 65 . https://doi.org/10.3847/0004-637X/821/1/65
dc.identifier.issn0004-637X
dc.identifier.otherPURE: 10455467
dc.identifier.otherPURE UUID: 8effb85c-e376-4dd5-8e96-1739dda99e89
dc.identifier.otherScopus: 84964374549
dc.identifier.urihttp://hdl.handle.net/2299/17304
dc.descriptionThis is an author-created, un-copyedited version of an article published in The Astrophysical Journal. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at https://doi.org/10.3847/0004-637X/821/1/65.
dc.description.abstractPlanets in highly eccentric orbits form a class of objects not seen within our solar system. The most extreme case known among these objects is the planet orbiting HD20782, with an orbital period of 597days and an eccentricity of 0.96. Here we present new data and analysis for this system as part of the Transit Ephemeris Refinement and Monitoring Survey. We obtained CHIRON spectra to perform an independent estimation of the fundamental stellar parameters. New radial velocities from Anglo-Australian Telescope and PARAS observations during periastron passage greatly improve our knowledge of the eccentric nature of the orbit. The combined analysis of our Keplerian orbital and Hipparcos astrometry show that the inclination of the planetary orbit is >1.22, ruling out stellar masses for the companion. Our long-term robotic photometry show that the star is extremely stable over long timescales. Photometric monitoring of the star during predicted transit and periastron times using Microvariability and Oscillations of STars rule out a transit of the planet and reveal evidence of phase variations during periastron. These possible photometric phase variations may be caused by reflected light from the planet’s atmosphere and the dramatic change in star–planet separation surrounding the periastron passage.en
dc.format.extent12
dc.language.isoeng
dc.relation.ispartofThe Astrophysical Journal
dc.rightsEmbargoed
dc.subjectplanetary systems
dc.subjectstars: individual (HD 207820
dc.subjectphotometric
dc.subjectradial velocities
dc.titleEvidence for Reflected Light from the Most Eccentric Exoplanet Knownen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.contributor.institutionCentre for Astrophysics Research
dc.description.statusPeer reviewed
dc.identifier.urlhttp://arxiv.org/abs/1511.08679
dc.description.versiontypeFinal Accepted Version
dcterms.dateAccepted2016-04-11
rioxxterms.versionAM
rioxxterms.versionofrecordhttps://doi.org/10.3847/0004-637X/821/1/65
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue
herts.rights.accesstypeEmbargoed


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