J/MNRAS/422/2024ivo://CDS.VizieR/J/MNRAS/422/2024doi:10.26093/cds/vizier.74222024CDSJackson A.P.Davis T.A.Wheatley P.J.2024-07-17T20:15:37Z2012-05-14T11:32:39ZCDS support team

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

cds-question@unistra.frlate-type-starsx-ray-sourcesvisible-astronomybroad-band-photometrysolar-system-planetsWe study the relationship between coronal X-ray emission and stellar age for late-type stars, and the variation of this relationship with spectral type. We select 717 stars from 13 open clusters and find that the ratio of X-ray to bolometric luminosity during the saturated phase of coronal emission decreases from 10^-3.1^ for late K-dwarfs to 10^-4.3^ for early F-type stars (across the range 0.29<(B-V)_0_<1.41). Our determined saturation timescales vary between 10^7.6^ and 10^8.3^ years, though with no clear trend across the whole FGK range. We apply our X-ray emission - age relations to the investigation of the evaporation history of 121 known transiting exoplanets using a simple energy -limited model of evaporation and taking into consideration Roche lobe effects and different heating/evaporation efficiencies. We confirm that a linear cut-off of the planet distribution in the M^2^/R^3^ versus a^-2^ plane is an expected result of population modification by evaporation and that the known transiting exoplanets display such a cut-off. We find that for an evaporation efficiency of 25 percent we expect around 1 in 5 of the known transiting exoplanets to have lost >10 percent of their mass since formation. In addition we provide estimates of the minimum formation mass for which a planet could be expected to survive for 4Gyrs for a range of stellar and planetary parameters. We emphasise the importance of the earliest periods of a planet's life for its evaporation history with 75 percent expect to occur within the first Gyr. This raises the possibility of using evaporation histories to distinguish different migration mechanisms. For planets with spin-orbit angles available from measurements of the Rossiter-McLaughlin effect no difference is found between the distributions of planets with misaligned orbits and those with aligned orbits. This suggests that dynamical effects accounting for misalignment occur early in the life of a planetary system, although additional data is required to test this.2012MNRAS.422.2024Jhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/422/2024CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/422/2024https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/422/2024http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/422/2024https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/422/2024https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/422/2024http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/422/2024GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/422/2024/stars (Data for individual cluster stars)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/422/2024/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/422/2024/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/422/2024/stars?GETtext/xml+votable180.050000true53.547083349.84166670.005555555555555556Cone search capability for table J/MNRAS/422/2024/tables (Host star parameters (table4), planet data (table3), and predictions for mass lost by the planets in our sample (table5))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/422/2024/tables?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/422/2024/tables?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/422/2024/tables?GETtext/xml+votable180.050000true102.0798833-3.10213330.0055555555555555565/118 784 4122 5886 6/75 309 333 336-337 339-342 349 375 461 463 485 496 753 790 840 876 917 1032 1042 1045 1075 1275 1768 1770-1771 1773-1774 2395 2532 2551 2584 2596 2711 3093-3095 3140 3344 3876 4687 4696 4698-4699 4720 4990 5009 5475 6017 6181 6349 6381 6539 6638 7036 7208 7240 8197 8237 8825 9173 9355 9482 9524 9811 10654 10730 12424 12644 12853 12983 13143 13439 13569 13680 13702 14757 14779 14825 14886 14914 14920 15129 15140 15143 15149 15160 15950 16405 16432 16947 17172 17226 18093 18766 20116 20339 22001 22034 22040 22065 22078 22120 22168-22169 22208 22505 23344 23396 23410 23423 23438 23454 23463 23479 23489-23490 23497 23499 23501 23504 23511 23515 23518-23519 23522-23523 23525-23527 23535 23537-23539 23541 23548 23550 24104 24192 24194 24201-24203 24206 24209 24315 24409 25132 25194 25885 25950 26062 26771 28400 28711 28717 28821-28822 28890-28891 30240-30241 30293 30295 30436 30450-30451 30466 31641 32727 32749 35210 36142 36667 37229-37231 37240 37242 37246-37247 37316 37329 37592-37593 37787-37788 37790-37791 37923 37933 37944 38452 39181 39183 39487 42936 43775 43847 43960 44648 45922 46421 46429 46437 47476https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/422/2024?format=asciiX-rayOpticaldefaultJ/MNRAS/422/2024/starsData for individual cluster starsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameSIMBAD identifiermeta.id;meta.maincharClusterCluster namemeta.id.parentcharDistDistance to star/clusterpcpos.distance;pos.heliocentricfloatf_Dist[1]? Hyades distance flag (1)meta.codeintnullabler_DistReference(s) for distancemeta.ref;pos.framecharlog(Age)Log of age (base 10)log(yr)time.agefloatr_log(Age)Reference(s) for agemeta.ref;pos.framecharVmagV magnitudemagphot.mag;em.opt.Vfloat(B-V)0De-reddened B-V colour indexmagphot.color;em.opt.B;em.opt.Vfloatlog(Lx)Log of X-ray luminosity (base 10)log(W)phys.luminosity;em.X-rayfloatlog(Lx/Lb)Log of bolometric-to-X-ray ratiophys.luminosity;arith.ratiofloatRefReference for X-ray and photometric datameta.ref;pos.framecharSimbadSimbad column added by the CDSmeta.refchar_RARight Ascension (J2000) from SIMBAD (not part of the original data)degpos.eq.ra;meta.main_DEDeclination (J2000) from SIMBAD (not part of the original data)degpos.eq.dec;meta.mainJ/MNRAS/422/2024/tablesHost star parameters (table4), planet data (table3), and predictions for mass lost by the planets in our sample (table5)recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintStarStar namemeta.id;meta.maincharMassStar masssolMassphys.massfloatSpTypeMK spectral typesrc.spTypecharB-V? B-V colour index only when used for SpType (1)phot.color;em.opt.B;em.opt.VfloatnullableVmag? V magnitudemagphot.mag;em.opt.Vfloatnullablembol? Bolometric magnitude (2)magphot.mag.bolfloatnullableDist? Distancepcpos.distance;pos.heliocentricintnullableAgeAgeGyrtime.agefloatn_Age[+] Note for assumed age of 4Gyr (3)meta.notecharlog(EX)Total X-ray energy emitted by the star (4)log(J)em.energyfloatn_log(EX)[*] Note on log(EX) (5)meta.notecharrefSReferencesmeta.ref;pos.framecharOSNameOther star namemeta.idcharSimbadSimbad column added by the CDSmeta.refcharPl[b-g] Planet designationmeta.code.multipcharMPPlanet mass(1.898187x10+27kg)phys.massfloatRPPlanet radius(7.1492x10+7m)phys.angSize;srcfloatPerOrbital perioddtime.perioddoubleaSemi-major axis of planet orbitAUphys.size.smajAxisfloatecc? Eccentricity of planet orbitsrc.orbital.eccentricityfloatnullable|lam|? Absolute spin-orbit misalignment angledegsrc.orbitalintnullablegPSurface gravity (1)m.s**-2phys.gravityfloatrhoPMean density (1)kg.m**-3phys.density;stat.meanint<a>Mean orbital distance (1)AUpos.distance;src.orbitalfloat1/K(eps)Roche lobe mass loss enhancement factor (1/K({epsilon}) (1)arith.factor;phys.mass.lossfloatlog(-PE)Planetary binding energy (1)log(J)phys.energyfloatrefReference, in refs.dat filemeta.ref;pos.frame;meta.filecharONameOther planet namemeta.idcharMi1RInitial mass M_i_ in constant radius approximation for {eta}=1 (1)(1.898187x10+27kg)phys.massfloatMi1dInitial mass M_i_ in constant density approximation for {eta}=1 (1)(1.898187x10+27kg)phys.massfloatMi0.25RInitial mass M_i_ in constant radius approximation for {eta}=0.25 (1)(1.898187x10+27kg)phys.massfloatMi0.25dInitial mass M_i_ in constant density approximation for {eta}=0.25 (1)(1.898187x10+27kg)phys.massfloatdM1RFraction of initial mass lost {beta} in constant radius approximation for {eta}=1phys.mass;arith.ratiodoubledM1rFraction of initial mass lost {beta} in constant density approximation for {eta}=1phys.mass;arith.ratiodoubledM0.25RFraction of initial mass lost {beta} in constant radius approximation for {eta}=0.25phys.mass;arith.ratiodoubledM0.25dFraction of initial mass lost {beta} with constant density approximation for {eta}=0.25phys.mass;arith.ratiodoubleNote[*] missing photometry or distance (2)meta.notechar_RAPosition from Simbad (right ascension part)degpos.eq.ra;meta.main_DEPosition from Simbad (declination part)degpos.eq.dec;meta.mainJ/MNRAS/422/2024/refsReferencesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefReference codemeta.notecharBibcodeBibcodemeta.bib.bibcodecharAuthorAuthor's namemeta.bib.authorcharComCommentsmeta.notechar