J/A+A/684/A112ivo://CDS.VizieR/J/A+A/684/A112doi:10.26093/cds/vizier.36840112CDSFritzewski D.J.Aerts C.Mombarg J.S.G.Gossage S.Van Reeth T.2024-11-29T20:01:28Z2024-04-09T10:10:00ZCDS support team

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

cds-question@unistra.frstellar-agesstellar-evolutionary-modelsGalactic archaeology largely relies on precise ages of distant evolved stars in the Milky Way. Nowadays, asteroseismology can deliver ages for many red giants observed with high-cadence, high-precision photometric space missions such as CoRoT, Kepler, K2, TESS, and soon PLATO. Our aim is to quantify the age uncertainties of currently slowly rotating red giants due to the cumulative effect of their fast rotation during core-hydrogen burning: their rotation in earlier evolutionary phases caused mixing of elements, resulting in heavier helium cores and the prolongation of their main-sequence lifetime. These rotational effects are usually ignored when age-dating red giants, despite our knowledge of fast rotation for stars with M>=1.3M_{sun}_. We used a sample of 490 F-type gravito-inertial pulsators (gamma Doradus stars) with precise asteroseismic estimates of their internal rotation rate from Kepler asteroseismology and with luminosity estimates from Gaia. For this sample, which includes stars rotating from nearly zero to about 60% of the critical rate, we computed the cumulative effect on the age in their post-main-sequence evolution caused by rotational mixing on the main sequence. We used stellar model grids with different physical prescriptions that mimic rotational mixing to assess systematic uncertainties on the age. With respect to non-rotating models, the sample of 490 gamma Doradus stars, as red giant progenitors, reveals age differences up to 5% by the time they start hydrogen-shell burning when relying on the theory of rotationally induced diffusive mixing as included in the MIST isochrones. Using rotational mixing based on an advective-diffusive approach that includes meridional circulation leads to an age shift of 20% by the time of the tip of the red giant branch. The age-dating of red giants is affected by the cumulative effect of rotational mixing during the main sequence. Such rotationally induced age shifts should be taken into account in addition to other effects if the aim is to perform Galactic archaeological studies at the highest precision.2024A&A...684A.112Fhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/684/A112CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toI/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)J/MNRAS/491/3586 : 611 {gamma} Doradus stars Kepler data (Li+, 2020)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/684/A112https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/684/A112http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/684/A112https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/684/A112https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/684/A112http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/684/A112GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/684/A112/tablea1 (Asteroseismic and stellar properties)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/684/A112/tablea1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/684/A112/tablea1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/684/A112/tablea1?GETtext/xml+votable180.050000true291.2342836.729130.0055555555555555564/922 5/3645-3647 3683 3695 3704 3706 3732 3734 3740 3783 3792 6/14567 14577-14579 14730-14731 14744 14746 14749-14751 14768 14770-14774 14776 14779 14792 14794 14828 14830 14914 14916 14918 14920 14922 14926 14932-14933 14935 14940-14942 14945-14947 14950 14952 14955-14956 14958-14959 14964-14966 14969 14972 14974-14975 15040 15057 15059-15060 15104-15105 15107 15109-15111 15113 15115 15118 15120-15122 15124-15126 15129-15131 15137 15141 15145-15146 15149-15150 15153-15158 15160 15172-15174 15176 15178 15200https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/684/A112?format=asciidefaultJ/A+A/684/A112/tablea1Asteroseismic and stellar propertiesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintKICKepler Input Catalog ID (KIC)meta.id;meta.mainintRA_ICRSRight ascension from Gaia DR3 (ICRS) at Ep=2016.0 (Cat. I/355) (RA)degpos.eq.ra;meta.mainDE_ICRSDeclination from Gaia DR3 (ICRS) at Ep=2016.0 (Cat. I/355) (DEC)degpos.eq.dec;meta.mainSimbadSimbad column added by the CDSmeta.ref.urlcharLumPhotometric luminosity (Lum)solLumphys.luminosityfloate_LumUncertainty of photometric luminosity (err_Lum)solLumstat.errorfloatTeffEffective temperature from Gaia DR3 (Cat. I/355) (Teff)Kphys.temperature.effectiveinte_TeffUncertainty of Teff (err_Teff)Kstat.error;phys.temperature.effectiveintPi0Buoyancy travel time (Pi0) (1)sem.freq;src.varinte_Pi0Lower uncertainty of Pi0 (errl_Pi0) (1)sstat.errorintE_Pi0Upper uncertainty of Pi0 (erru_Pi0) (1)sstat.error;stat.maxintfrotNear-core rotation rate (frot) (1)d**-1em.freq;src.vardoublee_frotLower uncertainty of frot (errl_frot) (1)d**-1stat.errordoubleE_frotUpper uncertainty of frot (erru_frot) (1)d**-1stat.error;stat.maxdoubleXc'Normalised core hydrogen mass fraction (Xc')phys.abund.Xfloate_Xc'Lower uncertainty of Xc' (errl_Xc')stat.errorfloatE_Xc'Upper uncertainty of Xc' (erru_Xc')stat.error;stat.maxfloatAgeAsteroseismic age (age)Gyrtime.agefloate_AgeLower uncertainty of age (errl_age)Gyrstat.error;time.agefloatE_AgeUpper uncertainty of age (erru_age)Gyrstat.error;stat.maxfloatMassAsteroseismic mass (mass)solMassphys.massfloate_MassLower uncertainty of mass (errl_mass)solMassstat.error;phys.massfloatE_MassUpper uncertainty of mass (erru_mass)solMassstat.error;stat.maxfloatRadAsteroseismic radius (radius)solRadphys.size.radiusfloate_RadLower uncertainty of radius (errl_radius)solRadstat.errorfloatE_RadUpper uncertainty of radius (erru_radius)solRadstat.error;stat.maxfloatvvcritRatio of current rotation rate to critical rotation rate (vvcrit)stat.fit.paramfloatM-age-TAMSAge of rotating MIST track at TAMS (MIST_age_TAMS)Gyrtime.agefloatNR-M-age-TAMSAge non-rot. MIST track at TAMS (NR_MIST_age_TAMS)Gyrtime.agefloatTAMS-fracFraction of rotating to non-rotating age at TAMS (TAMS_frac)meta.numberfloatM-age-TRGBAge of rotating MIST track at TRGB (MIST_age_TRGB)Gyrtime.agefloatNR-M-age-TRGBAge non-rot. MIST track at TRGB (NR_MIST_age_TRGB)Gyrtime.agefloatTRGB-fracFraction of rotating to non-rotating age at TRGB (TRGB_frac)meta.numberfloatM-age-ZAHeBAge of rotating MIST track at ZAHeB (MIST_age_ZAHeB)Gyrtime.agefloatNR-M-age-ZAHeBAge non-rot. MIST track at ZAHeB (NR_MIST_age_ZAHeB)Gyrtime.agefloatZAHeB-fracFraction of rotating to non-rotating age at ZAHeB (ZAHeB_frac)meta.numberfloatM-age-TAHeB? Age of rotating MIST track at TAHeB (MIST_age_TAHeB)Gyrtime.agefloatnullableNR-M-age-TAHeBAge non-rot. MIST track at TAHeB (NR_MIST_age_TAHeB)Gyrtime.agefloatTAHeB-frac? Fraction of rotating to non-rotating age at TAHeB (TAHeB_frac)meta.numberfloatnullable