Examining the orbital decay targets KELT-9 b, KELT-16 b, and WASP-4 b, and the transit-timing variations of HD 97658 b,

J. V. Harre; A. M.S. Smith; S. C.C. Barros; G. Boué; Sz Csizmadia; D. Ehrenreich; H. G. Florén; A. Fortier; P. F.L. Maxted; M. J. Hooton; B. Akinsanmi; L. M. Serrano; N. M. Rosário; B. O. Demory; K. Jones; J. Laskar; V. Adibekyan; Y. Alibert; R. Alonso; D. R. Anderson; G. Anglada; J. Asquier; T. Bárczy; D. Barrado Y Navascues; W. Baumjohann; M. Beck; T. Beck; W. Benz; N. Billot; F. Biondi; A. Bonfanti; X. Bonfils; A. Brandeker; C. Broeg; J. Cabrera; V. Cessa; S. Charnoz; A. Collier Cameron; M. B. Davies; M. Deleuil; L. Delrez; O. D.S. Demangeon; A. Erikson; L. Fossati; M. Fridlund; D. Gandolfi; M. Gillon; M. Güdel; C. Hellier; K. Heng; S. Hoyer; K. G. Isaak; L. L. Kiss; A. Lecavelier Des Etangs; M. Lendl; C. Lovis; A. Luntzer; D. Magrin; V. Nascimbeni; G. Olofsson; R. Ottensamer; I. Pagano; E. Pallé; C. M. Persson; G. Peter; G. Piotto; D. Pollacco; D. Queloz; R. Ragazzoni; N. Rando; H. Rauer; I. Ribas; G. R. Ricker; S. Salmon; N. C. Santos; G. Scandariato; S. Seager; D. Ségransan; A. E. Simon; S. G. Sousa; M. Steller; Gy M. Szabó; N. Thomas; S. Udry; B. Ulmer; V. Van Grootel; N. A. Walton; T. G. Wilson; J. N. Winn; B. Wohler

doi:10.1051/0004-6361/202244529

Examining the orbital decay targets KELT-9 b, KELT-16 b, and WASP-4 b, and the transit-timing variations of HD 97658 b^,

J. V. Harre, A. M.S. Smith, S. C.C. Barros, G. Boué, Sz Csizmadia, D. Ehrenreich, H. G. Florén, A. Fortier, P. F.L. Maxted, M. J. Hooton, B. Akinsanmi, L. M. Serrano, N. M. Rosário, B. O. Demory, K. Jones, J. Laskar, V. Adibekyan, Y. Alibert, R. Alonso, D. R. AndersonG. Anglada, J. Asquier, T. Bárczy, D. Barrado Y Navascues, W. Baumjohann, M. Beck, T. Beck, W. Benz, N. Billot, F. Biondi, A. Bonfanti, X. Bonfils, A. Brandeker, C. Broeg, J. Cabrera, V. Cessa, S. Charnoz, A. Collier Cameron, M. B. Davies, M. Deleuil, L. Delrez, O. D.S. Demangeon, A. Erikson, L. Fossati, M. Fridlund, D. Gandolfi, M. Gillon, M. Güdel, C. Hellier, K. Heng, S. Hoyer, K. G. Isaak, L. L. Kiss, A. Lecavelier Des Etangs, M. Lendl, C. Lovis, A. Luntzer, D. Magrin, V. Nascimbeni, G. Olofsson, R. Ottensamer, I. Pagano, E. Pallé, C. M. Persson, G. Peter, G. Piotto, D. Pollacco, D. Queloz, R. Ragazzoni, N. Rando, H. Rauer, I. Ribas, G. R. Ricker, S. Salmon, N. C. Santos, G. Scandariato, S. Seager, D. Ségransan, A. E. Simon, S. G. Sousa, M. Steller, Gy M. Szabó, N. Thomas, S. Udry, B. Ulmer, V. Van Grootel, N. A. Walton, T. G. Wilson, J. N. Winn, B. Wohler

Astrophysical Sciences

Research output: Contribution to journal › Article › peer-review

2 Scopus citations

Abstract

Context. Tidal orbital decay is suspected to occur for hot Jupiters in particular, with the only observationally confirmed case of this being WASP-12 b. 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.

Original language	English (US)
Article number	A124
Journal	Astronomy and Astrophysics
Volume	669
DOIs	https://doi.org/10.1051/0004-6361/202244529
State	Published - Jan 1 2023

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

planet-star interactions
planets and satellites: dynamical evolution and stability
techniques: photometric

Access to Document

10.1051/0004-6361/202244529

Cite this

Harre, 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., ... Wohler, B. (2023). Examining the orbital decay targets KELT-9 b, KELT-16 b, and WASP-4 b, and the transit-timing variations of HD 97658 b^,. Astronomy and Astrophysics, 669, Article A124. https://doi.org/10.1051/0004-6361/202244529

@article{8eebb413a11a42be9768221111aa2b58,

title = "Examining the orbital decay targets KELT-9 b, KELT-16 b, and WASP-4 b, and the transit-timing variations of HD 97658 b,",

abstract = "Context. Tidal orbital decay is suspected to occur for hot Jupiters in particular, with the only observationally confirmed case of this being WASP-12 b. 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.",

keywords = "planet-star interactions, planets and satellites: dynamical evolution and stability, techniques: photometric",

author = "Harre, {J. V.} and Smith, {A. M.S.} and Barros, {S. C.C.} and G. Bou{\'e} and Sz Csizmadia and D. Ehrenreich and Flor{\'e}n, {H. G.} and A. Fortier and Maxted, {P. F.L.} and Hooton, {M. J.} and B. Akinsanmi and Serrano, {L. M.} and Ros{\'a}rio, {N. M.} and Demory, {B. O.} and K. Jones and J. Laskar and V. Adibekyan and Y. Alibert and R. Alonso and Anderson, {D. R.} and G. Anglada and J. Asquier and T. B{\'a}rczy and {Y Navascues}, {D. Barrado} and W. Baumjohann and M. Beck and T. Beck and W. Benz and N. Billot and F. Biondi and A. Bonfanti and X. Bonfils and A. Brandeker and C. Broeg and J. Cabrera and V. Cessa and S. Charnoz and Cameron, {A. Collier} and Davies, {M. B.} and M. Deleuil and L. Delrez and Demangeon, {O. D.S.} and A. Erikson and L. Fossati and M. Fridlund and D. Gandolfi and M. Gillon and M. G{\"u}del and C. Hellier and K. Heng and S. Hoyer and Isaak, {K. G.} and Kiss, {L. L.} and {Des Etangs}, {A. Lecavelier} and M. Lendl and C. Lovis and A. Luntzer and D. Magrin and V. Nascimbeni and G. Olofsson and R. Ottensamer and I. Pagano and E. Pall{\'e} and Persson, {C. M.} and G. Peter and G. Piotto and D. Pollacco and D. Queloz and R. Ragazzoni and N. Rando and H. Rauer and I. Ribas and Ricker, {G. R.} and S. Salmon and Santos, {N. C.} and G. Scandariato and S. Seager and D. S{\'e}gransan and Simon, {A. E.} and Sousa, {S. G.} and M. Steller and Szab{\'o}, {Gy M.} and N. Thomas and S. Udry and B. Ulmer and {Van Grootel}, V. and Walton, {N. A.} and Wilson, {T. G.} and Winn, {J. N.} and B. Wohler",

note = "Funding Information: We thank the anonymous referee for their helpful comments. The CHEOPS photometric data underlying this article is publicly accessible using the CHEOPS archive browser ( https://cheops-archive.astro.unige.ch/archive_browser/ ), at the DACE website in the CHEOPS database, or via PYCHEOPS using the file keys provided in Table 1. The TESS data used in this publication is publicly available at the MAST archive. The timing data for the various planets and the photometric CHEOPS data is available with the online version of this article and at the CDS. CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The CHEOPS Consortium would like to gratefully acknowledge the support received by all the agencies, offices, universities, and industries involved. Their flexibility and willingness to explore new approaches were essential to the success of this mission. JVH acknowledges the support of the DFG priority programme SPP 1992 “Exploring the Diversity of Extrasolar Planets (SM 4862-1)”. S.C.C.B. acknowledges support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004. This project has received funding from the European Research Council (ERC) under the European Union{\textquoteright}s Horizon 2020 research and innovation programme (project FOUR ACES. P.M. acknowledges support from STFC research grant number ST/M001040/1. L.M.S. gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 {\textquoteleft}Gaseous or rocky? Unveiling the nature of small worlds{\textquoteright}. B.-O.D. acknowledges support from the Swiss National Science Foundation (PP00P2-190080). This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements d{\textquoteright}Avenir supervised by the Agence Nationale pour la Recherche. Y.A. and M.J.H. acknowledge the support of the Swiss National Fund under grant 200020_172746. We acknowledge support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, PGC2018-098153-B-C33, PGC2018-098153-B-C31, ESP2017-87676-C5-1-R, MDM-2017-0737 Unidad de Excelencia Maria de Maeztu-Centro de Astrobiolog{\'i}a (INTA-CSIC), as well as the support of the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. X.B., S.C., D.G., M.F. and J.L. acknowledge their role as ESA-appointed CHEOPS science team members. A.Br. was supported by the SNSA. A.C.C. acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. This project was supported by the CNES. The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Programme, and by the University of Li{\`e}ge through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. L.D. is an F.R.S.-FNRS Postdoctoral Researcher. This work was supported by FCT - Funda{\c c}{\~a}o para a Ci{\^e}ncia e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalizac{\~a}o by these grants: UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020, PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113, PTDC/FIS-AST/28953/2017 & POCI-01-0145-FEDER-028953, PTDC/FIS-AST/28987/2017 & POCI-01-0145-FEDER-028987, O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. M.F. and C.M.P. gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/18). DG gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 “Gaseousor rocky? Unveiling the nature of small worlds”. M.G. is an F.R.S.-FNRS Senior Research Associate. SH gratefully acknowledges CNES funding through the grant 837319. K.G.I. is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme. She does not participate in, or contribute to, the definition of the Guaranteed Time Programme of the CHEOPS mission through which observations described in this paper have been taken, nor to any aspect of target selection for the programme. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. LBo, GBr, VNa, IPa, GPi, RRa, GSc, VSi, and TZi acknowledge support from CHEOPS ASI-INAF agreement no. 2019-29-HH.0. This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). IRI acknowledges support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grant PGC2018-098153-B-C33, as well as the support of the Generalitat de Catalunya/CERCA programme. S.G.S. acknowledge support from FCT through FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). GyMSz acknowledges the support of the Hungarian National Research, Development and Innovation Office (NKFIH) grant K-125015, a a PRODEX Experiment Agreement No. 4000137122, the Lend{\"u}let LP2018-7/2021 grant of the Hungarian Academy of Science and the support of the city of Szom-bathely. V.V.G. is an F.R.S-FNRS Research Associate. N.A.W. acknowledges UKSA grant ST/R004838/1. 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. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA{\textquoteright}s Science Mission Directorate. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Programme through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. Publisher Copyright: {\textcopyright} The Authors 2023.",

year = "2023",

month = jan,

day = "1",

doi = "10.1051/0004-6361/202244529",

language = "English (US)",

volume = "669",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Harre, JV, Smith, AMS, Barros, SCC, Boué, G, Csizmadia, S, Ehrenreich, D, Florén, HG, Fortier, A, Maxted, PFL, Hooton, MJ, Akinsanmi, B, Serrano, LM, Rosário, NM, Demory, BO, Jones, K, Laskar, J, Adibekyan, V, Alibert, Y, Alonso, R, Anderson, DR, Anglada, G, Asquier, J, Bárczy, T, Y Navascues, DB, 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, Cameron, AC, Davies, MB, Deleuil, M, Delrez, L, Demangeon, ODS, Erikson, A, Fossati, L, Fridlund, M, Gandolfi, D, Gillon, M, Güdel, M, Hellier, C, Heng, K, Hoyer, S, Isaak, KG, Kiss, LL, Des Etangs, AL, Lendl, M, Lovis, C, Luntzer, A, Magrin, D, Nascimbeni, V, Olofsson, G, Ottensamer, R, Pagano, I, Pallé, E, Persson, CM, Peter, G, Piotto, G, Pollacco, D, Queloz, D, Ragazzoni, R, Rando, N, Rauer, H, Ribas, I, Ricker, GR, Salmon, S, Santos, NC, Scandariato, G, Seager, S, Ségransan, D, Simon, AE, Sousa, SG, Steller, M, Szabó, GM, Thomas, N, Udry, S, Ulmer, B, Van Grootel, V, Walton, NA, Wilson, TG, Winn, JN & Wohler, B 2023, 'Examining the orbital decay targets KELT-9 b, KELT-16 b, and WASP-4 b, and the transit-timing variations of HD 97658 b^,', Astronomy and Astrophysics, vol. 669, A124. https://doi.org/10.1051/0004-6361/202244529

TY - JOUR

T1 - Examining the orbital decay targets KELT-9 b, KELT-16 b, and WASP-4 b, and the transit-timing variations of HD 97658 b,

AU - Harre, J. V.

AU - Smith, A. M.S.

AU - Barros, S. C.C.

AU - Boué, G.

AU - Csizmadia, Sz

AU - Ehrenreich, D.

AU - Florén, H. G.

AU - Fortier, A.

AU - Maxted, P. F.L.

AU - Hooton, M. J.

AU - Akinsanmi, B.

AU - Serrano, L. M.

AU - Rosário, N. M.

AU - Demory, B. O.

AU - Jones, K.

AU - Laskar, J.

AU - Adibekyan, V.

AU - Alibert, Y.

AU - Alonso, R.

AU - Anderson, D. R.

AU - Anglada, G.

AU - Asquier, J.

AU - Bárczy, T.

AU - Y Navascues, D. Barrado

AU - Baumjohann, W.

AU - Beck, M.

AU - Beck, T.

AU - Benz, W.

AU - Billot, N.

AU - Biondi, F.

AU - Bonfanti, A.

AU - Bonfils, X.

AU - Brandeker, A.

AU - Broeg, C.

AU - Cabrera, J.

AU - Cessa, V.

AU - Charnoz, S.

AU - Cameron, A. Collier

AU - Davies, M. B.

AU - Deleuil, M.

AU - Delrez, L.

AU - Demangeon, O. D.S.

AU - Erikson, A.

AU - Fossati, L.

AU - Fridlund, M.

AU - Gandolfi, D.

AU - Gillon, M.

AU - Güdel, M.

AU - Hellier, C.

AU - Heng, K.

AU - Hoyer, S.

AU - Isaak, K. G.

AU - Kiss, L. L.

AU - Des Etangs, A. Lecavelier

AU - Lendl, M.

AU - Lovis, C.

AU - Luntzer, A.

AU - Magrin, D.

AU - Nascimbeni, V.

AU - Olofsson, G.

AU - Ottensamer, R.

AU - Pagano, I.

AU - Pallé, E.

AU - Persson, C. M.

AU - Peter, G.

AU - Piotto, G.

AU - Pollacco, D.

AU - Queloz, D.

AU - Ragazzoni, R.

AU - Rando, N.

AU - Rauer, H.

AU - Ribas, I.

AU - Ricker, G. R.

AU - Salmon, S.

AU - Santos, N. C.

AU - Scandariato, G.

AU - Seager, S.

AU - Ségransan, D.

AU - Simon, A. E.

AU - Sousa, S. G.

AU - Steller, M.

AU - Szabó, Gy M.

AU - Thomas, N.

AU - Udry, S.

AU - Ulmer, B.

AU - Van Grootel, V.

AU - Walton, N. A.

AU - Wilson, T. G.

AU - Winn, J. N.

AU - Wohler, B.

N1 - Funding Information: We thank the anonymous referee for their helpful comments. The CHEOPS photometric data underlying this article is publicly accessible using the CHEOPS archive browser ( https://cheops-archive.astro.unige.ch/archive_browser/ ), at the DACE website in the CHEOPS database, or via PYCHEOPS using the file keys provided in Table 1. The TESS data used in this publication is publicly available at the MAST archive. The timing data for the various planets and the photometric CHEOPS data is available with the online version of this article and at the CDS. CHEOPS is an ESA mission in partnership with Switzerland with important contributions to the payload and the ground segment from Austria, Belgium, France, Germany, Hungary, Italy, Portugal, Spain, Sweden, and the United Kingdom. The CHEOPS Consortium would like to gratefully acknowledge the support received by all the agencies, offices, universities, and industries involved. Their flexibility and willingness to explore new approaches were essential to the success of this mission. JVH acknowledges the support of the DFG priority programme SPP 1992 “Exploring the Diversity of Extrasolar Planets (SM 4862-1)”. S.C.C.B. acknowledges support from FCT through FCT contracts nr. IF/01312/2014/CP1215/CT0004. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project FOUR ACES. P.M. acknowledges support from STFC research grant number ST/M001040/1. L.M.S. gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 ‘Gaseous or rocky? Unveiling the nature of small worlds’. B.-O.D. acknowledges support from the Swiss National Science Foundation (PP00P2-190080). This work was granted access to the HPC resources of MesoPSL financed by the Region Ile de France and the project Equip@Meso (reference ANR-10-EQPX-29-01) of the programme Investissements d’Avenir supervised by the Agence Nationale pour la Recherche. Y.A. and M.J.H. acknowledge the support of the Swiss National Fund under grant 200020_172746. We acknowledge support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grants ESP2016-80435-C2-1-R, ESP2016-80435-C2-2-R, PGC2018-098153-B-C33, PGC2018-098153-B-C31, ESP2017-87676-C5-1-R, MDM-2017-0737 Unidad de Excelencia Maria de Maeztu-Centro de Astrobiología (INTA-CSIC), as well as the support of the Generalitat de Catalunya/CERCA programme. The MOC activities have been supported by the ESA contract No. 4000124370. X.B., S.C., D.G., M.F. and J.L. acknowledge their role as ESA-appointed CHEOPS science team members. A.Br. was supported by the SNSA. A.C.C. acknowledges support from STFC consolidated grant numbers ST/R000824/1 and ST/V000861/1, and UKSA grant number ST/R003203/1. This project was supported by the CNES. The Belgian participation to CHEOPS has been supported by the Belgian Federal Science Policy Office (BELSPO) in the framework of the PRODEX Programme, and by the University of Liège through an ARC grant for Concerted Research Actions financed by the Wallonia-Brussels Federation. L.D. is an F.R.S.-FNRS Postdoctoral Researcher. This work was supported by FCT - Fundação para a Ciência e a Tecnologia through national funds and by FEDER through COMPETE2020 - Programa Operacional Competitividade e Internacionalizacão by these grants: UID/FIS/04434/2019, UIDB/04434/2020, UIDP/04434/2020, PTDC/FIS-AST/32113/2017 & POCI-01-0145-FEDER-032113, PTDC/FIS-AST/28953/2017 & POCI-01-0145-FEDER-028953, PTDC/FIS-AST/28987/2017 & POCI-01-0145-FEDER-028987, O.D.S.D. is supported in the form of work contract (DL 57/2016/CP1364/CT0004) funded by national funds through FCT. M.F. and C.M.P. gratefully acknowledge the support of the Swedish National Space Agency (DNR 65/19, 174/18). DG gratefully acknowledges financial support from the CRT foundation under Grant No. 2018.2323 “Gaseousor rocky? Unveiling the nature of small worlds”. M.G. is an F.R.S.-FNRS Senior Research Associate. SH gratefully acknowledges CNES funding through the grant 837319. K.G.I. is the ESA CHEOPS Project Scientist and is responsible for the ESA CHEOPS Guest Observers Programme. She does not participate in, or contribute to, the definition of the Guaranteed Time Programme of the CHEOPS mission through which observations described in this paper have been taken, nor to any aspect of target selection for the programme. M.L. acknowledges support of the Swiss National Science Foundation under grant number PCEFP2_194576. LBo, GBr, VNa, IPa, GPi, RRa, GSc, VSi, and TZi acknowledge support from CHEOPS ASI-INAF agreement no. 2019-29-HH.0. This work was also partially supported by a grant from the Simons Foundation (PI Queloz, grant number 327127). IRI acknowledges support from the Spanish Ministry of Science and Innovation and the European Regional Development Fund through grant PGC2018-098153-B-C33, as well as the support of the Generalitat de Catalunya/CERCA programme. S.G.S. acknowledge support from FCT through FCT contract nr. CEECIND/00826/2018 and POPH/FSE (EC). GyMSz acknowledges the support of the Hungarian National Research, Development and Innovation Office (NKFIH) grant K-125015, a a PRODEX Experiment Agreement No. 4000137122, the Lendület LP2018-7/2021 grant of the Hungarian Academy of Science and the support of the city of Szom-bathely. V.V.G. is an F.R.S-FNRS Research Associate. N.A.W. acknowledges UKSA grant ST/R004838/1. 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. Some of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Support for MAST for non-HST data is provided by the NASA Office of Space Science via grant NNX13AC07G and by other grants and contracts. This paper includes data collected by the TESS mission. Funding for the TESS mission is provided by the NASA’s Science Mission Directorate. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Programme through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. Publisher Copyright: © The Authors 2023.

PY - 2023/1/1

Y1 - 2023/1/1

N2 - Context. Tidal orbital decay is suspected to occur for hot Jupiters in particular, with the only observationally confirmed case of this being WASP-12 b. 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.

AB - Context. Tidal orbital decay is suspected to occur for hot Jupiters in particular, with the only observationally confirmed case of this being WASP-12 b. 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.

KW - planet-star interactions

KW - planets and satellites: dynamical evolution and stability

KW - techniques: photometric

UR - http://www.scopus.com/inward/record.url?scp=85147138880&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85147138880&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/202244529

DO - 10.1051/0004-6361/202244529

M3 - Article

AN - SCOPUS:85147138880

SN - 0004-6361

VL - 669

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A124

ER -