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dc.contributor.authorBonomo, A.S.
dc.contributor.authorSozzetti, A.
dc.contributor.authorLovis, C.
dc.contributor.authorMalavolta, L.
dc.contributor.authorRice, K.
dc.contributor.authorBuchhave, L.A.
dc.contributor.authorSasselov, D.
dc.contributor.authorCameron, A.C.
dc.contributor.authorLatham, D.W.
dc.contributor.authorMolinari, E.
dc.contributor.authorPepe, F.
dc.contributor.authorUdry, S.
dc.contributor.authorAffer, L.
dc.contributor.authorCharbonneau, D.
dc.contributor.authorCosentino, R.
dc.contributor.authorDressing, C.D.
dc.contributor.authorDumusque, X.
dc.contributor.authorFigueira, P.
dc.contributor.authorFiorenzano, A.F.M.
dc.contributor.authorGettel, S.
dc.contributor.authorHarutyunyan, A.
dc.contributor.authorHaywood, R.D.
dc.contributor.authorHorne, K.
dc.contributor.authorLopez-Morales, M.
dc.contributor.authorMayor, M.
dc.contributor.authorMicela, G.
dc.contributor.authorMotalebi, F.
dc.contributor.authorNascimbeni, V.
dc.contributor.authorPhillips, D.F.
dc.contributor.authorPiotto, G.
dc.contributor.authorPollacco, D.
dc.contributor.authorQueloz, D.
dc.contributor.authorSégransan, D.
dc.contributor.authorSzentgyorgyi, A.
dc.contributor.authorWatson, C.
dc.date.accessioned2014-12-05T13:01:05Z
dc.date.available2014-12-05T13:01:05Z
dc.date.issued2014-12
dc.identifier.citationBonomo , A S , Sozzetti , A , Lovis , C , Malavolta , L , Rice , K , Buchhave , L A , Sasselov , D , Cameron , A C , Latham , D W , Molinari , E , Pepe , F , Udry , S , Affer , L , Charbonneau , D , Cosentino , R , Dressing , C D , Dumusque , X , Figueira , P , Fiorenzano , A F M , Gettel , S , Harutyunyan , A , Haywood , R D , Horne , K , Lopez-Morales , M , Mayor , M , Micela , G , Motalebi , F , Nascimbeni , V , Phillips , D F , Piotto , G , Pollacco , D , Queloz , D , Ségransan , D , Szentgyorgyi , A & Watson , C 2014 , ' Characterization of the planetary system Kepler-101 with HARPS-N : A hot super-Neptune with an Earth-sized low-mass companion ' , Astronomy & Astrophysics , vol. 572 , A2 . https://doi.org/10.1051/0004-6361/201424617en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 159056941
dc.identifier.otherPURE UUID: 1a5493ae-551d-440c-9942-786fe8354de5
dc.identifier.otherScopus: 84911388487
dc.identifier.otherWOS: 000346101700034
dc.identifier.otherORCID: /0000-0002-8863-7828/work/58531434
dc.identifier.urihttp://hdl.handle.net/10023/5880
dc.descriptionThe research leading to these results has received funding from the European Union Seventh Framework Programme (FP7/2007-2013) under Grant Agreement No. 313014 (ETAEARTH). R.D. Haywood acknowledges support from an STFC postgraduate research studentshipen
dc.description.abstractWe characterize the planetary system Kepler-101 by performing a combined differential evolution Markov chain Monte Carlo analysis of Kepler data and forty radial velocities obtained with the HARPS-N spectrograph. This system was previously validated and is composed of a hot super-Neptune, Kepler-101b, and an Earth-sized planet, Kepler-101c. These two planets orbit the slightly evolved and metal-rich G-type star in 3.49 and 6.03 days, respectively. With mass Mp = 51.1-4.7+ 5.1 M⊕, radius Rp = 5.77-0.79+ 0.85 R⊕, and density ρp = 1.45-0.48+ 0.83 g cm-3, Kepler-101b is the first fully characterized super-Neptune, and its density suggests that heavy elements make up a significant fraction of its interior; more than 60% of its total mass. Kepler-101c has a radius of 1.25-0.17+ 0.19 R⊕, which implies the absence of any H/He envelope, but its mass could not be determined because of the relative faintness of the parent star for highly precise radial-velocity measurements (Kp = 13.8) and the limited number of radial velocities. The 1σ upper limit, Mp< 3.8 M⊕, excludes a pure iron composition with a probability of 68.3%. The architecture of the planetary system Kepler-101 − containing a close-in giant planet and an outer Earth-sized planet with a period ratio slightly larger than the 3:2 resonance − is certainly of interest for scenarios of planet formation and evolution. This system does not follow the previously reported trend that the larger planet has the longer period in the majority of Kepler systems of planet pairs with at least one Neptune-sized or larger planet.
dc.format.extent7
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rightsReproduced with permission from Astronomy & Astrophysics, © ESOen
dc.subjectPlanetary systemsen
dc.subjectStars: fundamental parametersen
dc.subjectTechniques: photometricen
dc.subjectTechniques: radial velocitiesen
dc.subjectTechniques: spectroscopicen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleCharacterization of the planetary system Kepler-101 with HARPS-N : A hot super-Neptune with an Earth-sized low-mass companionen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorEuropean Commissionen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorPPARC - Now STFCen
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/10.1051/0004-6361/201424617
dc.description.statusPeer revieweden
dc.identifier.grantnumberST/J001651/1en
dc.identifier.grantnumberen
dc.identifier.grantnumberST/I000666/1en
dc.identifier.grantnumberPP/D000890/1en
dc.identifier.grantnumberST/G001006/1en
dc.identifier.grantnumberPP/F000065/1en


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