Show simple item record

Files in this item

Thumbnail

Item metadata

dc.contributor.authorVanderburg, Andrew
dc.contributor.authorBecker, Juliette C.
dc.contributor.authorBuchhave, Lars A.
dc.contributor.authorMortier, Annelies
dc.contributor.authorLopez, Eric
dc.contributor.authorMalavolta, Luca
dc.contributor.authorHaywood, Raphaëlle D.
dc.contributor.authorLatham, David W.
dc.contributor.authorCharbonneau, David
dc.contributor.authorLópez-Morales, Mercedes
dc.contributor.authorAdams, Fred C.
dc.contributor.authorBonomo, Aldo Stefano
dc.contributor.authorBouchy, François
dc.contributor.authorCollier Cameron, Andrew
dc.contributor.authorCosentino, Rosario
dc.contributor.authorDi Fabrizio, Luca
dc.contributor.authorDumusque, Xavier
dc.contributor.authorFiorenzano, Aldo
dc.contributor.authorHarutyunyan, Avet
dc.contributor.authorJohnson, John Asher
dc.contributor.authorLorenzi, Vania
dc.contributor.authorLovis, Christophe
dc.contributor.authorMayor, Michel
dc.contributor.authorMicela, Giusi
dc.contributor.authorMolinari, Emilio
dc.contributor.authorPedani, Marco
dc.contributor.authorPepe, Francesco
dc.contributor.authorPiotto, Giampaolo
dc.contributor.authorPhillips, David
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.accessioned2017-11-23T15:30:07Z
dc.date.available2017-11-23T15:30:07Z
dc.date.issued2017-11-17
dc.identifier.citationVanderburg , A , Becker , J C , Buchhave , L A , Mortier , A , Lopez , E , Malavolta , L , Haywood , R D , Latham , D W , Charbonneau , D , López-Morales , M , Adams , F C , Bonomo , A S , Bouchy , F , Collier Cameron , A , Cosentino , R , Di Fabrizio , L , Dumusque , X , Fiorenzano , A , Harutyunyan , A , Johnson , J A , Lorenzi , V , Lovis , C , Mayor , M , Micela , G , Molinari , E , Pedani , M , Pepe , F , Piotto , G , Phillips , D , Rice , K , Sasselov , D , Ségransan , D , Sozzetti , A , Udry , S & Watson , C 2017 , ' Precise masses in the WASP-47 system ' , Astronomical Journal , vol. 154 , no. 6 , 237 . https://doi.org/10.3847/1538-3881/aa918ben
dc.identifier.issn0004-6256
dc.identifier.otherPURE: 251425137
dc.identifier.otherPURE UUID: 8f1a15b9-fa03-438d-875a-780582731137
dc.identifier.otherBibCode: 2017arXiv171000026V
dc.identifier.otherScopus: 85038240451
dc.identifier.otherORCID: /0000-0002-8863-7828/work/58531353
dc.identifier.otherWOS: 000415867300005
dc.identifier.urihttp://hdl.handle.net/10023/12159
dc.descriptionFunding: European Union Seventh Framework Programme (FP7/2007-2013) under Grant Agreement n.313014 (ETAEARTH). Parts of this work have been supported by NASA under grants No. NNX15AC90G and NNX17AB59G issued through the Exoplanets Research Program. This publication was made possible through the support of a grant from the John Templeton Foundation.en
dc.description.abstractWe present precise radial velocity observations of WASP-47, a star known to host a hot Jupiter, a distant Jovian companion, and, uniquely, two additional transiting planets in short-period orbits: a super-Earth in a ≈19 hr orbit, and a Neptune in a ≈ 9 day orbit. We analyze our observations from the HARPS-N spectrograph along with previously published data to measure the most precise planet masses yet for this system. When combined with new stellar parameters and reanalyzed transitphotometry, our mass measurements place strong constraints on the compositions of the two small planets. We find unlike most other ultra-short-period planets, the inner planet, WASP-47 e, has a mass (6.83 ± 0.66 M⊕) and radius (1.810 ± 0.027 R⊕) inconsistent with an Earth-like composition. Instead, WASP-47 e likely has a volatile-rich envelope surrounding an Earth-like core and mantle. We also perform a dynamical analysis to constrain the orbital inclination of WASP-47 c, the outer Jovian planet. This planet likely orbits close to the plane of the inner three planets, suggesting a quiet dynamical history for the system. Our dynamical constraints also imply that WASP-47 c is much more likely to transit than a geometric calculation would suggest. We calculate a transit probability for WASP-47 c of about 10%, more than an order of magnitude larger than the geometric transit probability of 0.6%.
dc.format.extent14
dc.language.isoeng
dc.relation.ispartofAstronomical Journalen
dc.rights© 2017 The 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 https://doi.org/10.3847/1538-3881/aa918ben
dc.subjectPlanets and satellites: compositionen
dc.subjectPlanets and satellites: detectionen
dc.subjectPlanets and satellites: dynamical evolution and stabilityen
dc.subjectPlanets and satellites: fundamental parametersen
dc.subjectPlanetes and satellites: gaseous planetsen
dc.subjectPlanets and satellites: interiorsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titlePrecise masses in the WASP-47 systemen
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/aa918b
dc.description.statusPeer revieweden
dc.identifier.urlhttp://adsabs.harvard.edu/abs/2017arXiv171000026Ven


This item appears in the following Collection(s)

Show simple item record