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dc.contributor.authorDressing, Courtney D.
dc.contributor.authorCharbonneau, David
dc.contributor.authorDumusque, Xavier
dc.contributor.authorGettel, Sara
dc.contributor.authorPepe, Francesco
dc.contributor.authorCameron, Andrew Collier
dc.contributor.authorLatham, David W.
dc.contributor.authorMolinari, Emilio
dc.contributor.authorUdry, Stephane
dc.contributor.authorAffer, Laura
dc.contributor.authorBonomo, Aldo S.
dc.contributor.authorBuchhave, Lars A.
dc.contributor.authorCosentino, Rosario
dc.contributor.authorFigueira, Pedro
dc.contributor.authorFiorenzano, Aldo F. M.
dc.contributor.authorHarutyunyan, Avet
dc.contributor.authorHaywood, Raphaelle D.
dc.contributor.authorJohnson, John Asher
dc.contributor.authorLopez-Morales, Mercedes
dc.contributor.authorLovis, Christophe
dc.contributor.authorMalavolta, Luca
dc.contributor.authorMayor, Michel
dc.contributor.authorMicela, Giusi
dc.contributor.authorMotalebi, Fatemeh
dc.contributor.authorNascimbeni, Valerio
dc.contributor.authorPhillips, David F.
dc.contributor.authorPiotto, Giampaolo
dc.contributor.authorPollacco, Don
dc.contributor.authorQueloz, Didier
dc.contributor.authorRice, Ken
dc.contributor.authorSasselov, Dimitar
dc.contributor.authorSegransan, Damien
dc.contributor.authorSozzetti, Alessandro
dc.contributor.authorSzentgyorgyi, Andrew
dc.contributor.authorWatson, Chris
dc.date.accessioned2015-03-24T17:01:04Z
dc.date.available2015-03-24T17:01:04Z
dc.date.issued2015-02-20
dc.identifier176497413
dc.identifierdb827179-b287-4e37-9efd-af6663f54110
dc.identifier000349782500058
dc.identifier84924273193
dc.identifier000349782500058
dc.identifier.citationDressing , C D , Charbonneau , D , Dumusque , X , Gettel , S , Pepe , F , Cameron , A C , Latham , D W , Molinari , E , Udry , S , Affer , L , Bonomo , A S , Buchhave , L A , Cosentino , R , Figueira , P , Fiorenzano , A F M , Harutyunyan , A , Haywood , R D , Johnson , J A , Lopez-Morales , M , Lovis , C , Malavolta , L , Mayor , M , Micela , G , Motalebi , F , Nascimbeni , V , Phillips , D F , Piotto , G , Pollacco , D , Queloz , D , Rice , K , Sasselov , D , Segransan , D , Sozzetti , A , Szentgyorgyi , A & Watson , C 2015 , ' The mass of Kepler-93b and the composition of terrestrial planets ' , Astrophysical Journal , vol. 800 , no. 2 , 135 . https://doi.org/10.1088/0004-637X/800/2/135en
dc.identifier.issn0004-637X
dc.identifier.otherORCID: /0000-0002-8863-7828/work/58531485
dc.identifier.urihttps://hdl.handle.net/10023/6308
dc.description.abstractKepler-93b is a 1.478 ± 0.019 R ⊕ planet with a 4.7 day period around a bright (V = 10.2), astroseismically characterized host star with a mass of 0.911 ± 0.033 M ☉ and a radius of 0.919 ± 0.011 R ☉. Based on 86 radial velocity observations obtained with the HARPS-N  spectrograph on the Telescopio Nazionale Galileo and 32 archival Keck/HIRES observations, we present a precise mass estimate of 4.02 ± 0.68 M ⊕. The corresponding high density of 6.88 ± 1.18 g cm–3 is consistent with a rocky composition of primarily iron and magnesium silicate. We compare Kepler-93b to other dense planets with well-constrained parameters and find that between 1 and 6 M ⊕, all dense planets including the Earth and Venus are well-described by the same fixed ratio of iron to magnesium silicate. There are as of yet no examples of such planets with masses >6 M ⊕. All known planets in this mass regime have lower densities requiring significant fractions of volatiles or H/He gas. We also constrain the mass and period of the outer companion in the Kepler-93 system from the long-term radial velocity trend and archival adaptive optics images. As the sample of dense planets with well-constrained masses and radii continues to grow, we will be able to test whether the fixed compositional model found for the seven dense planets considered in this paper extends to the full population of 1-6 M ⊕ planets.
dc.format.extent7
dc.format.extent505605
dc.language.isoeng
dc.relation.ispartofAstrophysical Journalen
dc.subjectPlanetary systemsen
dc.subjectPlanets and satellites: compositionen
dc.subjectStars: individual (Kepler-93=KOI 69=KIC 3544595)en
dc.subjectTechniques: radial velocitiesen
dc.subject100 Earth massesen
dc.subjectSuper-Earthsen
dc.subjectRadius relationshipsen
dc.subjectExtrasolar planetsen
dc.subjectSolar-systemsen
dc.subjectStarsen
dc.subjectAbundancesen
dc.subjectTransitsen
dc.subjectCatalogen
dc.subjectOrbitsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectNDASen
dc.subjectBDCen
dc.subjectR2Cen
dc.subject~DC~en
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleThe mass of Kepler-93b and the composition of terrestrial planetsen
dc.typeJournal articleen
dc.contributor.sponsorEuropean Commissionen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorPPARC - Now STFCen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.identifier.doi10.1088/0004-637X/800/2/135
dc.description.statusPeer revieweden
dc.identifier.grantnumberen
dc.identifier.grantnumberST/M001296/1en
dc.identifier.grantnumberST/I000666/1en
dc.identifier.grantnumberPP/D000890/1en
dc.identifier.grantnumberST/J001651/1en
dc.identifier.grantnumberST/G001006/1en
dc.identifier.grantnumberPP/F000065/1en


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