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dc.contributor.authorMalavolta, Luca
dc.contributor.authorMayo, Andrew W.
dc.contributor.authorLouden, Tom
dc.contributor.authorRajpaul, Vinesh M.
dc.contributor.authorBonomo, Aldo S.
dc.contributor.authorBuchhave, Lars A.
dc.contributor.authorKreidberg, Laura
dc.contributor.authorKristiansen, Martti H.
dc.contributor.authorLopez-Morales, Mercedes
dc.contributor.authorMortier, Annelies
dc.contributor.authorVanderburg, Andrew
dc.contributor.authorCoffinet, Adrien
dc.contributor.authorEhrenreich, David
dc.contributor.authorLovis, Christophe
dc.contributor.authorBouchy, Francois
dc.contributor.authorCharbonneau, David
dc.contributor.authorCiardi, David R.
dc.contributor.authorCollier Cameron, Andrew
dc.contributor.authorCosentino, Rosario
dc.contributor.authorCrossfield, Ian J. M.
dc.contributor.authorDamasso, Mario
dc.contributor.authorDressing, Courtney D.
dc.contributor.authorDumusque, Xavier
dc.contributor.authorEverett, Mark E.
dc.contributor.authorFigueira, Pedro
dc.contributor.authorFiorenzano, Aldo F. M.
dc.contributor.authorGonzales, Erica J.
dc.contributor.authorHaywood, Raphaëlle D.
dc.contributor.authorHarutyunyan, Avet
dc.contributor.authorHirsch, Lea
dc.contributor.authorHowell, Steve B.
dc.contributor.authorJohnson, John Asher
dc.contributor.authorLatham, David W.
dc.contributor.authorLopez, Eric
dc.contributor.authorMayor, Michel
dc.contributor.authorMicela, Giusi
dc.contributor.authorMolinari, Emilio
dc.contributor.authorNascimbeni, Valerio
dc.contributor.authorPepe, Francesco
dc.contributor.authorPhillips, David F.
dc.contributor.authorPiotto, Giampaolo
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.identifier.citationMalavolta , L , Mayo , A W , Louden , T , Rajpaul , V M , Bonomo , A S , Buchhave , L A , Kreidberg , L , Kristiansen , M H , Lopez-Morales , M , Mortier , A , Vanderburg , A , Coffinet , A , Ehrenreich , D , Lovis , C , Bouchy , F , Charbonneau , D , Ciardi , D R , Collier Cameron , A , Cosentino , R , Crossfield , I J M , Damasso , M , Dressing , C D , Dumusque , X , Everett , M E , Figueira , P , Fiorenzano , A F M , Gonzales , E J , Haywood , R D , Harutyunyan , A , Hirsch , L , Howell , S B , Johnson , J A , Latham , D W , Lopez , E , Mayor , M , Micela , G , Molinari , E , Nascimbeni , V , Pepe , F , Phillips , D F , Piotto , G , Rice , K , Sasselov , D , Ségransan , D , Sozzetti , A , Udry , S & Watson , C 2018 , ' An ultra-short period rocky super-Earth with a secondary eclipse and a Neptune-like companion around K2-141 ' , Astronomical Journal , vol. 155 , no. 3 , 107 .
dc.identifier.otherBibCode: 2018arXiv180103502M
dc.identifier.otherORCID: /0000-0002-8863-7828/work/58531376
dc.description.abstractUltra-short period (USP) planets are a class of low mass planets with periods shorter than one day. Their origin is still unknown, with photo-evaporation of mini-Neptunes and in-situ formation being the most credited hypotheses. Formation scenarios differ radically in the predicted composition of USP planets, it is therefore extremely important to increase the still limited sample of USP planets with precise and accurate mass and density measurements. We report here the characterization of an USP planet with a period of 0.28 days around K2-141 (EPIC 246393474), and the validation of an outer planet with a period of 7.7 days in a grazing transit configuration. We derived the radii of the planets from the K2 light curve and used high-precision radial velocities gathered with the HARPS-N spectrograph for mass measurements. For K2-141b we thus inferred a radius of 1.51 ± 0.05 R⊕ and a mass of 5.08 ± 0.41 M⊕, consistent with a rocky composition and lack of a thick atmosphere. K2-141c is likely a Neptune-like planet, although due to the grazing transits and the non-detection in the RV dataset, we were not able to put a strong constraint on its density. We also report the detection of secondary eclipses and phase curve variations for K2-141b. The phase variation can be modeled either by a planet with a geometric albedo of 0.30 ± 0.06 in the Kepler bandpass, or by thermal emission from the surface of the planet at ∼3000K. Only follow-up observations at longer wavelengths will allow us to distinguish between these two scenarios.
dc.relation.ispartofAstronomical Journalen
dc.subjectPlanetary systemsen
dc.subjectPlanets and satellites: compositionen
dc.subjectPlanets and satellites: individual (K2-141b, K2-141c)en
dc.subjectPlanets and satellites: interiorsen
dc.subjectStars: individual (K2-141)en
dc.subjectTechniques: photometricen
dc.subjectTechniques: radial velocitiesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleAn ultra-short period rocky super-Earth with a secondary eclipse and a Neptune-like companion around K2-141en
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorEuropean Commissionen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews. St Andrews Centre for Exoplanet Scienceen
dc.description.statusPeer revieweden

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