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dc.contributor.authorHarre, J.-V.
dc.contributor.authorSmith, A. M. S.
dc.contributor.authorBarros, S. C. C.
dc.contributor.authorBoué, G.
dc.contributor.authorCsizmadia, Sz.
dc.contributor.authorEhrenreich, D.
dc.contributor.authorFlorén, H.-G.
dc.contributor.authorFortier, A.
dc.contributor.authorMaxted, P. F. L.
dc.contributor.authorHooton, M. J.
dc.contributor.authorAkinsanmi, B.
dc.contributor.authorSerrano, L. M.
dc.contributor.authorRosário, N. M.
dc.contributor.authorDemory, B.-O.
dc.contributor.authorJones, K.
dc.contributor.authorLaskar, J.
dc.contributor.authorAdibekyan, V.
dc.contributor.authorAlibert, Y.
dc.contributor.authorAlonso, R.
dc.contributor.authorAnderson, D. R.
dc.contributor.authorAnglada, G.
dc.contributor.authorAsquier, J.
dc.contributor.authorBárczy, T.
dc.contributor.authorBarrado y Navascues, D.
dc.contributor.authorBaumjohann, W.
dc.contributor.authorBeck, M.
dc.contributor.authorBeck, T.
dc.contributor.authorBenz, W.
dc.contributor.authorBillot, N.
dc.contributor.authorBiondi, F.
dc.contributor.authorBonfanti, A.
dc.contributor.authorBonfils, X.
dc.contributor.authorBrandeker, A.
dc.contributor.authorBroeg, C.
dc.contributor.authorCabrera, J.
dc.contributor.authorCessa, V.
dc.contributor.authorCharnoz, S.
dc.contributor.authorCollier Cameron, A.
dc.contributor.authorDavies, M. B.
dc.contributor.authorDeleuil, M.
dc.contributor.authorDelrez, L.
dc.contributor.authorDemangeon, O. D. S.
dc.contributor.authorErikson, A.
dc.contributor.authorFossati, L.
dc.contributor.authorFridlund, M.
dc.contributor.authorGandolfi, D.
dc.contributor.authorGillon, M.
dc.contributor.authorGüdel, M.
dc.contributor.authorHellier, C.
dc.contributor.authorHeng, K.
dc.contributor.authorHoyer, S.
dc.contributor.authorIsaak, K. G.
dc.contributor.authorKiss, L. L.
dc.contributor.authorLecavelier des Etangs, A.
dc.contributor.authorLendl, M.
dc.contributor.authorLovis, C.
dc.contributor.authorLuntzer, A.
dc.contributor.authorMagrin, D.
dc.contributor.authorNascimbeni, V.
dc.contributor.authorOlofsson, G.
dc.contributor.authorOttensamer, R.
dc.contributor.authorPagano, I.
dc.contributor.authorPallé, E.
dc.contributor.authorPersson, C. M.
dc.contributor.authorPeter, G.
dc.contributor.authorPiotto, G.
dc.contributor.authorPollacco, D.
dc.contributor.authorQueloz, D.
dc.contributor.authorRagazzoni, R.
dc.contributor.authorRando, N.
dc.contributor.authorRauer, H.
dc.contributor.authorRibas, I.
dc.contributor.authorRicker, G. R.
dc.contributor.authorSalmon, S.
dc.contributor.authorSantos, N. C.
dc.contributor.authorScandariato, G.
dc.contributor.authorSeager, S.
dc.contributor.authorSégransan, D.
dc.contributor.authorSimon, A. E.
dc.contributor.authorSousa, S. G.
dc.contributor.authorSteller, M.
dc.contributor.authorSzabó, Gy. M.
dc.contributor.authorThomas, N.
dc.contributor.authorUdry, S.
dc.contributor.authorUlmer, B.
dc.contributor.authorVan Grootel, V.
dc.contributor.authorWalton, N. A.
dc.contributor.authorWilson, T. G.
dc.contributor.authorWinn, J. N.
dc.contributor.authorWohler, B.
dc.identifier.citationHarre , J-V , Smith , A M S , Barros , S C C , Boué , G , Csizmadia , S , Ehrenreich , D , Florén , H-G , Fortier , A , Maxted , P F L , Hooton , M J , Akinsanmi , B , Serrano , L M , Rosário , N M , Demory , B-O , Jones , K , Laskar , J , Adibekyan , V , Alibert , Y , Alonso , R , Anderson , D R , Anglada , G , Asquier , J , Bárczy , T , Barrado y Navascues , D , Baumjohann , W , Beck , M , Beck , T , Benz , W , Billot , N , Biondi , F , Bonfanti , A , Bonfils , X , Brandeker , A , Broeg , C , Cabrera , J , Cessa , V , Charnoz , S , Collier Cameron , A , Davies , M B , Deleuil , M , Delrez , L , Demangeon , O D S , Erikson , A , Fossati , L , Fridlund , M , Gandolfi , D , Gillon , M , Güdel , M , Hellier , C , Heng , K , Hoyer , S , Isaak , K G , Kiss , L L , Lecavelier des Etangs , A , Lendl , M , Lovis , C , Luntzer , A , Magrin , D , Nascimbeni , V , Olofsson , G , Ottensamer , R , Pagano , I , Pallé , E , Persson , C M , Peter , G , Piotto , G , Pollacco , D , Queloz , D , Ragazzoni , R , Rando , N , Rauer , H , Ribas , I , Ricker , G R , Salmon , S , Santos , N C , Scandariato , G , Seager , S , Ségransan , D , Simon , A E , Sousa , S G , Steller , M , Szabó , G M , Thomas , N , Udry , S , Ulmer , B , Van Grootel , V , Walton , N A , Wilson , T G , Winn , J N & Wohler , B 2023 , ' Examining the orbital decay targets KELT-9 b, KELT-16 b, and WASP-4b, and the transit-timing variations of HD 97658 b ' , Astronomy and Astrophysics , vol. 669 , A124 .
dc.identifier.otherPURE: 283836956
dc.identifier.otherPURE UUID: 6db13ec1-c425-4711-99e3-3af4608e2c2c
dc.identifier.othercrossref: 10.1051/0004-6361/202244529
dc.identifier.otherScopus: 85147138880
dc.identifier.otherORCID: /0000-0002-8863-7828/work/131588502
dc.identifier.otherORCID: /0000-0001-8749-1962/work/131588576
dc.descriptionFunding: A.C.C. and T.W. acknowledge support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1.en
dc.description.abstractContext Tidal orbital decay is suspected to occur for hot Jupiters in particular, with the only observationally confirmed case of this being WASP-12b. By examining this effect, information on the properties of the host star can be obtained using the so-called stellar modified tidal quality factor Q*′, which describes the efficiency with which the kinetic energy of the planet is dissipated within the star. This can provide information about the interior of the star. Aims In this study, we aim to improve constraints on the tidal decay of the KELT-9, KELT-16, and WASP-4 systems in order to find evidence for or against the presence of tidal orbital decay. With this, we want to constrain the Q*′ value for each star. In addition, we aim to test the existence of the transit timing variations (TTVs) in the HD 97658 system, which previously favoured a quadratic trend with increasing orbital period. Methods Making use of newly acquired photometric observations from CHEOPS (CHaracterising ExOplanet Satellite) and TESS (Transiting Exoplanet Survey Satellite), combined with archival transit and occultation data, we use Markov chain Monte Carlo (MCMC) algorithms to fit three models to the data, namely a constant-period model, an orbital-decay model, and an apsidal-precession model. Results We find that the KELT-9 system is best described by an apsidal-precession model for now, with an orbital decay trend at over 2 σ being a possible solution as well. A Keplerian orbit model with a constant orbital period provides the best fit to the transit timings of KELT-16 b because of the scatter and scale of their error bars. The WASP-4 system is best represented by an orbital decay model at a 5 σ significance, although apsidal precession cannot be ruled out with the present data. For HD 97658 b, using recently acquired transit observations, we find no conclusive evidence for a previously suspected strong quadratic trend in the data.
dc.relation.ispartofAstronomy and Astrophysicsen
dc.rightsCopyright © The Authors 2023. Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.en
dc.subjectPlanets and satellites: dynamical evolution and stabilityen
dc.subjectPlanet-star interactionsen
dc.subjectTechniques: photometricen
dc.subjectQB Astronomyen
dc.titleExamining the orbital decay targets KELT-9 b, KELT-16 b, and WASP-4b, and the transit-timing variations of HD 97658 ben
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.description.versionPublisher PDFen
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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