J/AJ/168/81ivo://CDS.VizieR/J/AJ/168/81doi:10.26093/cds/vizier.51680081CDSSaunders N.Grunblatt S.K.Chontos A.Dai F.Huber D.Zhang J.,Stefansson G.van Saders J.L.Winn J.N.Hey D.Howard A.W.Fulton B.,Isaacson H.Beard C.Giacalone S.Van Zandt J.Murphey J.M.A.,Rice M.Blunt S.Turtelboom E.Dalba P.A.Lubin J.Brinkman C.,Louden E.M.Page E.Watkins C.N.Collins K.A.Stockdale C.Tan T.-G.,Schwarz R.P.Massey B.Howell S.B.Vanderburg A.Ricker G.R.,Jenkins J.M.Seager S.Christiansen J.L.Daylan T.Falk B.,Brodheim M.Gibson S.R.Hill G.M.Holden B.Householder A.Kaye S.,Laher R.R.Lanclos K.Petigura E.A.Roy A.Rubenzahl R.A.Schwab C.,Shaum A.P.Sirk M.M.Smith C.L.Walawender J.Yeh S.2025-03-03T20:09:18Z2025-01-17T12:08:21ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frradial-velocitystellar-massesstellar-agesmetallicityexoplanetsvisible-astronomyspectroscopyThe degree of alignment between a star's spin axis and the orbital plane of its planets (the stellar obliquity) is related to interesting and poorly understood processes that occur during planet formation and evolution. Hot Jupiters orbiting hot stars (>~6250K) display a wide range of obliquities, while similar planets orbiting cool stars are preferentially aligned. Tidal dissipation is expected to be more rapid in stars with thick convective envelopes, potentially explaining this trend. Evolved stars provide an opportunity to test the damping hypothesis, particularly stars that were hot on the main sequence and have since cooled and developed deep convective envelopes. We present the first systematic study of the obliquities of hot Jupiters orbiting subgiants that recently developed convective envelopes using Rossiter-McLaughlin observations. Our sample includes two newly discovered systems in the Giants Transiting Giants survey (TOI-6029 b, TOI-4379 b). We find that the orbits of hot Jupiters orbiting subgiants that have cooled below ~6250K are aligned or nearly aligned with the spin axis of their host stars, indicating rapid tidal realignment after the emergence of a stellar convective envelope. We place an upper limit for the timescale of realignment for hot Jupiters orbiting subgiants at ~500Myr. Comparison with a simplified tidal evolution model shows that obliquity damping needs to be ~4 orders of magnitude more efficient than orbital period decay to damp the obliquity without destroying the planet, which is consistent with recent predictions for tidal dissipation from inertial waves excited by hot Jupiters on misaligned orbits.2024AJ....168...81Shttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/168/81CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toIV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)J/ApJ/703/L99 : Outlandish orbit of HAT-P-7b (Winn+, 2009)J/AJ/142/19 : Speckle observations of KOI (Howell+, 2011)J/A+A/552/A120 : WASP-71b light curve (Smith+, 2013)J/A+A/588/L6 : WASP-12 transit light curves (Maciejewski+ 2016)J/ApJ/836/77 : High-S/N optical spectra of FGKM stars (Yee+, 2017)J/AcA/68/371 : WASP and KELT planet transits (Maciejewski+, 2018)J/AJ/157/192 : Radial velocities and transit times for KOI 4 (Chontos+, 2019)J/AJ/159/280 : Gaia-Kepler stellar properties catalog. I. (Berger+, 2020)J/ApJ/888/L5 : Transits, occultation times and RVs of WASP-12b (Yee+, 2020)http://tess.mit.edu/followup/ : TESS Follow-up Observing Program (TFOP) homehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/168/81https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/168/81http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/168/81https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/168/81https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/168/81http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/168/81GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/AJ/168/81/table1 (Stellar properties derived for each of the host stars in our sample)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/AJ/168/81/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/AJ/168/81/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/AJ/168/81/table1?GETtext/xml+votable180.050000true297.215833364.354350.0055555555555555566/3057 15927 428271.9867573869263685e-19 3.916500758235022e-19https://cdsarc.cds.unistra.fr/viz-bin/moc/J/AJ/168/81?format=asciiOpticaldefaultJ/AJ/168/81/table1Stellar properties derived for each of the host stars in our samplelogg[3.88/4.02] Log of surface gravity (4)log(cm.s**-2)phys.gravityfloate_logg[0.02/0.03] Lower uncertainty on logglog(cm.s**-2)stat.error;stat.min;phys.gravityfloatE_logg[0.016/0.04] Upper uncertainty on logglog(cm.s**-2)stat.error;stat.max;phys.gravityfloate_Age[0.19/1.21] Lower uncertainty on AgeGyrstat.error;stat.min;time.agefloatE_Age[0.2/0.6] Upper uncertainty on AgeGyrstat.error;stat.max;time.agefloatLum[4.3/6.3] Luminosity (4)solLumphys.luminosityfloate_Lum[0.1/0.3] Lower uncertainty on LumsolLumstat.error;stat.min;phys.luminosityfloatE_Lum[0.2/0.3] Upper uncertainty on LumsolLumstat.error;stat.max;phys.luminosityfloatDist[310/618] Distance (4)pcpos.distancefloate_Dist[4.8/12] Lower uncertainty on Distpcstat.error;stat.min;pos.distancefloatE_Dist[6/11.6] Upper uncertainty on Distpcstat.error;stat.max;pos.distancefloatVPInteractive velocity plotmeta.ref.urlcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameTOI star numbermeta.id;meta.maincharPlPlanet ID componentmeta.id.part;meta.maincharn_Name[a] a: Flag on TOI-1181 (1)meta.notecharTIC[97766057/419523962] TIC star number (2)meta.idlongRAJ2000Hour of right ascension (J2000) (2)pos.eq.ra;meta.mainDEJ2000Degree of declination (J2000) (2)pos.eq.dec;meta.mainVmag[10.58/12.9] Johnson V magnitude (2)magphot.mag;em.opt.Vfloate_Vmag[0.006/0.1] Uncertainty on the Vmagmagstat.error;phot.mag;em.opt.VfloatGmag[10.47/12.41] Gaia G-band magnitude (2)magphot.mag;em.optfloate_Gmag[0.0002/0.0003] Uncertainty on the Gmagmagstat.error;phot.mag;em.optfloatTmag[10.079/11.9] T band magnitude (2)magphot.mag;em.optfloate_Tmag[0.006/0.09] Uncertainty on the Tmagmagstat.error;phot.mag;em.optfloatTeff[6020/6223] Effective temperature (3)Kphys.temperature.effectiveinte_Teff[81/100] Teff uncertaintyKstat.error;phys.temperature.effectiveint[Fe/H][0.16/0.38] Metallicity (3)log(Sun)phys.abund.Fefloate_[Fe/H][0.06] [Fe/H] uncertaintylog(Sun)stat.error;phys.abund.Fefloatvsini[5.9/10.6] Rotational velocity (3)km/sphys.veloc.rotatfloate_vsini[1] vsini uncertaintykm/sstat.error;phys.veloc.rotatfloatMs[1.37/1.55] Stellar mass (4)solMassphys.massfloate_Ms[0.02/0.11] Lower uncertainty on MssolMassstat.error;stat.min;phys.massfloatE_Ms[0.02/0.04] Upper uncertainty on MssolMassstat.error;stat.max;phys.massfloatRs[1.96/2.34] Stellar radius (4)solRadphys.size.radiusfloate_Rs[0.03/0.09] Lower uncertainty on RssolRadstat.error;stat.min;phys.size.radiusfloatE_Rs[0.027/0.04] Upper uncertainty on RssolRadstat.error;stat.max;phys.size.radiusfloatSimbadSimbad column added by the CDSmeta.ref.urlcharAge[2.3/4.51] Age (4)Gyrtime.agefloatJ/AJ/168/81/table3Radial velocity measurements of TOI-1181, TOI-6029, and TOI-4379 used in our analysisrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintBJDTime (midpoint) of observation, Barycentric Julian date at TDBdtime.epochdoubleRVel[-159/146] Radial Velocitym.s**-1phys.veloc;pos.heliocentricdoublee_RVel[2.3/14.1] Uncertainty in RVm.s**-1stat.error;phys.veloc;pos.heliocentricfloatNameTOI star numbermeta.id;meta.maincharInstInstrument ("Keck/HIRES" or "Keck/KPF")meta.id;instrcharRMcLObservation taken for Rossiter-McLaughlin effect ("False" or "True")meta.codechar