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dc.contributor.authorMalavolta, Luca
dc.contributor.authorBorsato, Luca
dc.contributor.authorGranata, Valentina
dc.contributor.authorPiotto, Giampaolo
dc.contributor.authorLopez, Eric
dc.contributor.authorVanderburg, Andrew
dc.contributor.authorFigueira, Pedro
dc.contributor.authorMortier, Annelies
dc.contributor.authorNascimbeni, Valerio
dc.contributor.authorAffer, Laura
dc.contributor.authorBonomo, Aldo S.
dc.contributor.authorBouchy, Francois
dc.contributor.authorBuchhave, Lars A.
dc.contributor.authorCharbonneau, David
dc.contributor.authorCollier Cameron, Andrew
dc.contributor.authorCosentino, Rosario
dc.contributor.authorDressing, Courtney D.
dc.contributor.authorDumusque, Xavier
dc.contributor.authorFiorenzano, Aldo F. M.
dc.contributor.authorHarutyunyan, Avet
dc.contributor.authorHaywood, Raphaëlle D.
dc.contributor.authorJohnson, John Asher
dc.contributor.authorLatham, David W.
dc.contributor.authorLopez-Morales, Mercedes
dc.contributor.authorLovis, Christophe
dc.contributor.authorMayor, Michel
dc.contributor.authorMicela, Giusi
dc.contributor.authorMolinari, Emilio
dc.contributor.authorMotalebi, Fatemeh
dc.contributor.authorPepe, Francesco
dc.contributor.authorPhillips, David F.
dc.contributor.authorPollacco, Don
dc.contributor.authorQueloz, Didier
dc.contributor.authorRice, Ken
dc.contributor.authorSasselov, Dimitar
dc.contributor.authorSégransan, Damien
dc.contributor.authorSozzetti, Alessandro
dc.contributor.authorUdry, Stéphane
dc.contributor.authorWatson, Chris
dc.date.accessioned2017-03-31T16:30:10Z
dc.date.available2017-03-31T16:30:10Z
dc.date.issued2017-04-24
dc.identifier.citationMalavolta , L , Borsato , L , Granata , V , Piotto , G , Lopez , E , Vanderburg , A , Figueira , P , Mortier , A , Nascimbeni , V , Affer , L , Bonomo , A S , Bouchy , F , Buchhave , L A , Charbonneau , D , Collier Cameron , A , Cosentino , R , Dressing , C D , Dumusque , X , Fiorenzano , A F M , Harutyunyan , A , Haywood , R D , Johnson , J A , Latham , D W , Lopez-Morales , M , Lovis , C , Mayor , M , Micela , G , Molinari , E , Motalebi , F , Pepe , F , Phillips , D F , Pollacco , D , Queloz , D , Rice , K , Sasselov , D , Ségransan , D , Sozzetti , A , Udry , S & Watson , C 2017 , ' The Kepler-19 system : a thick-envelope super-Earth with two Neptune-mass companions characterized using radial velocities and transit timing variations ' , Astronomical Journal , vol. 153 , no. 5 , 224 . https://doi.org/10.3847/1538-3881/aa6897en
dc.identifier.issn0004-6256
dc.identifier.otherPURE: 249447666
dc.identifier.otherPURE UUID: 6e3248d1-5e22-4411-b771-4e6f16403194
dc.identifier.otherBibCode: 2017arXiv170306885M
dc.identifier.otherScopus: 85019047549
dc.identifier.otherORCID: /0000-0002-8863-7828/work/58531342
dc.identifier.otherWOS: 000399888800003
dc.identifier.urihttp://hdl.handle.net/10023/10566
dc.description.abstractWe report a detailed characterization of the Kepler-19 system. This star was previously known to host a transiting planet with a period of 9.29 days, a radius of 2.2 R⊕ and an upper limit on the mass of 20 M⊕. The presence of a second, non-transiting planet was inferred from the transit time variations (TTVs) of Kepler-19b, over 8 quarters of Kepler photometry, although neither mass nor period could be determined. By combining new TTVs measurements from all the Kepler quarters and 91 high-precision radial velocities obtained with the HARPS-N spectrograph, we measured through dynamical simulations a mass of 8.4±1.6 M⊕ for Kepler-19b. From the same data, assuming system coplanarity, we determined an orbital period of 28.7 days and a mass of 13.1±2.7 M⊕ for Kepler-19c and discovered a Neptune-like planet with a mass of 20.3±3.4 M⊕ on a 63 days orbit. By comparing dynamical simulations with non-interacting Keplerian orbits, we concluded that neglecting interactions between planets may lead to systematic errors that could hamper the precision in the orbital parameters when the dataset spans several years. With a density of 4.32±0.87 g cm−3 (0.78±0.16 ρ⊕) Kepler-19b belongs to the group of planets with a rocky core and a significant fraction of volatiles, in opposition to low-density planets characterized by transit-time variations only and the increasing number of rocky planets with Earth-like density. Kepler-19 joins the small number of systems that reconcile transit timing variation and radial velocity measurements.
dc.language.isoeng
dc.relation.ispartofAstronomical Journalen
dc.rights© 2017, American Astronomical Society. This work has been made available online in accordance with the publisher’s policies. This is the author created, accepted version manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at iopscience.iop.org /en
dc.subjectPlanetary systemsen
dc.subjectPlanets and satellites: compositionen
dc.subjectPlanets and satellites: dynamical evolution and stabilityen
dc.subjectStars: individual (Kepler-19)en
dc.subjectTechniques: radial velocitiesen
dc.subjectTechniques: photometricen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe Kepler-19 system : a thick-envelope super-Earth with two Neptune-mass companions characterized using radial velocities and transit timing variationsen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews.St Andrews Centre for Exoplanet Scienceen
dc.identifier.doihttps://doi.org/10.3847/1538-3881/aa6897
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2017arXiv170306885Men


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