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dc.contributor.authorBarros, S. C. C.
dc.contributor.authorGosselin, H.
dc.contributor.authorLillo-Box, J.
dc.contributor.authorBayliss, D.
dc.contributor.authorDelgado Mena, E.
dc.contributor.authorBrugger, B.
dc.contributor.authorSanterne, A.
dc.contributor.authorArmstrong, D. J.
dc.contributor.authorAdibekyan, V.
dc.contributor.authorArmstrong, J. D.
dc.contributor.authorBarrado, D.
dc.contributor.authorBento, J.
dc.contributor.authorBoisse, I.
dc.contributor.authorBonomo, A. S.
dc.contributor.authorBouchy, F.
dc.contributor.authorBrown, D. J. A.
dc.contributor.authorCochran, W. D.
dc.contributor.authorCollier Cameron, A.
dc.contributor.authorDeleuil, M.
dc.contributor.authorDemangeon, O.
dc.contributor.authorDíaz, R. F.
dc.contributor.authorDoyle, A.
dc.contributor.authorDumusque, X.
dc.contributor.authorEhrenreich, D.
dc.contributor.authorEspinoza, N.
dc.contributor.authorFaedi, F.
dc.contributor.authorFaria, J. P.
dc.contributor.authorFigueira, P.
dc.contributor.authorFoxell, E.
dc.contributor.authorHébrard, G.
dc.contributor.authorHojjatpanah, S.
dc.contributor.authorJackman, J.
dc.contributor.authorLendl, M.
dc.contributor.authorLigi, R.
dc.contributor.authorLovis, C.
dc.contributor.authorMelo, C.
dc.contributor.authorMousis, O.
dc.contributor.authorNeal, J. J.
dc.contributor.authorOsborn, H. P.
dc.contributor.authorPollacco, D.
dc.contributor.authorSantos, N. C.
dc.contributor.authorSefako, R.
dc.contributor.authorShporer, A.
dc.contributor.authorSousa, S. G.
dc.contributor.authorTriaud, A. H. M. J.
dc.contributor.authorUdry, S.
dc.contributor.authorVigan, A.
dc.contributor.authorWyttenbach, A.
dc.date.accessioned2017-11-14T13:30:08Z
dc.date.available2017-11-14T13:30:08Z
dc.date.issued2017-12-01
dc.identifier.citationBarros , S C C , Gosselin , H , Lillo-Box , J , Bayliss , D , Delgado Mena , E , Brugger , B , Santerne , A , Armstrong , D J , Adibekyan , V , Armstrong , J D , Barrado , D , Bento , J , Boisse , I , Bonomo , A S , Bouchy , F , Brown , D J A , Cochran , W D , Collier Cameron , A , Deleuil , M , Demangeon , O , Díaz , R F , Doyle , A , Dumusque , X , Ehrenreich , D , Espinoza , N , Faedi , F , Faria , J P , Figueira , P , Foxell , E , Hébrard , G , Hojjatpanah , S , Jackman , J , Lendl , M , Ligi , R , Lovis , C , Melo , C , Mousis , O , Neal , J J , Osborn , H P , Pollacco , D , Santos , N C , Sefako , R , Shporer , A , Sousa , S G , Triaud , A H M J , Udry , S , Vigan , A & Wyttenbach , A 2017 , ' Precise masses for the transiting planetary system HD 106315 with HARPS ' Astronomy & Astrophysics , vol. 608 , A25 . https://doi.org/10.1051/0004-6361/201731276en
dc.identifier.issn0004-6361
dc.identifier.otherPURE: 251493858
dc.identifier.otherPURE UUID: b360b62f-9d15-4617-ae4f-40a7ca6cdb4f
dc.identifier.otherBibCode: 2017arXiv170900865B
dc.identifier.otherScopus: 85037033143
dc.identifier.urihttps://arxiv.org/abs/1709.00865en
dc.identifier.urihttp://adsabs.harvard.edu/abs/2017arXiv170900865Ben
dc.descriptionFunding: UK Science and Tecnology Facilities Council STFC ST/M001296/1 (ACC)en
dc.description.abstractContext. The multi-planetary system HD 106315 was recently found in K2 data. The planets have periods of Pb ~ 9.55 and Pc ~ 21.06 days, and radii of rb = 2.44 ± 0.17 R⊕ and rc = 4.35 ± 0.23 R⊕ . The brightness of the host star (V = 9.0 mag) makes it an excellent target for transmission spectroscopy. However, to interpret transmission spectra it is crucial to measure the planetary masses. Aims. We obtained high precision radial velocities for HD 106315 to determine the mass of the two transiting planets discovered with Kepler K2. Our successful observation strategy was carefully tailored to mitigate the effect of stellar variability. Methods. We modelled the new radial velocity data together with the K2 transit photometry and a new ground-based partial transit of HD 106315c to derive system parameters. Results. We estimate the mass of HD 106315b to be 12.6 ± 3.2 M⊕ and the density to be 4.7 ± 1.7 g cm-3, while for HD 106315c we estimate a mass of 15.2 ± 3.7 M⊕ and a density of 1.01 ± 0.29 g cm-3. Hence, despite planet c having a radius almost twice as large as planet b, their masses are consistent with one another. Conclusions. We conclude that HD 106315c has a thick hydrogen-helium gaseous envelope. A detailed investigation of HD 106315b using a planetary interior model constrains the core mass fraction to be 5–29%, and the water mass fraction to be 10–50%. An alternative, not considered by our model, is that HD 106315b is composed of a large rocky core with a thick H–He envelope. Transmission spectroscopy of these planets will give insight into their atmospheric compositions and also help constrain their core compositions.
dc.format.extent14
dc.language.isoeng
dc.relation.ispartofAstronomy & Astrophysicsen
dc.rights© 2017, ESO. 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/10.1051/0004-6361/201731276en
dc.subjectPlanetary systems: detectionen
dc.subjectPlanetary systems: fundamental parametersen
dc.subjectPlanetary systems: compositionen
dc.subjectStars: individual HD 106315, EPIC 201437844en
dc.subjectTechniques: photometricen
dc.subjectTechniques: radial velocitiesen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titlePrecise masses for the transiting planetary system HD 106315 with HARPSen
dc.typeJournal articleen
dc.description.versionPostprinten
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/10.1051/0004-6361/201731276
dc.description.statusPeer revieweden


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