J/A+A/638/A20ivo://CDS.VizieR/J/A+A/638/A20doi:10.26093/cds/vizier.36380020CDSMagaudda E.Stelzer B.Covey K.R.Raetz St.Matt S.P.Scholz A.2024-12-23T20:00:43Z2020-06-03T07:57:38ZCDS support team

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

cds-question@unistra.frm-starsx-ray-sourcesstellar-massesstellar-radiiThe relation of activity to rotation in M dwarfs is of high astrophysical interest because it provides observational evidence of the stellar dynamo, which is poorly understood for low-mass stars, especially in the fully convective regime. Previous studies have shown that the relation of X-ray activity to rotation consists of two different regimes: the saturated regime for fast-rotating stars and unsaturated regime for slowly rotating stars. The transition between the two regimes lies at a rotation period of ~10d. We present here a sample of 14 M dwarf stars observed with XMM-Newton and Chandra, for which we also computed rotational periods from Kepler Two-Wheel (K2) Mission light curves. We compiled X-ray and rotation data from the literature and homogenized all data sets to provide the largest uniform sample of M dwarfs (302 stars) for X-ray activity and rotation studies to date. We then fit the relation between LX-Prot using three different mass bins to separate partially and fully convective stars. We found a steeper slope in the unsaturated regime for fully convective stars and a nonconstant LX level in the saturated regime for all masses. In the LX/Lbol-R_O_ space we discovered a remarkable double gap that might be related to a discontinuous period evolution. Then we combined the evolution of Prot predicted by angular momentum evolution models with our new results on the empirical LX-Prot relation to provide an estimate for the age decay of X-ray luminosity. We compare predictions of this relationship with the actual X-ray luminosities of M stars with known ages from 100Myr to a few billion years. We find remarkably good agreement between the predicted LX and the observed values for partially convective stars. However, for fully convective stars at ages of a few billion years, the constructed LX-age relation overpredicts the X-ray luminosity because the angular momentum evolution model underpredicts the rotation period of these stars. Finally, we examine the effect of different parameterizations for the Rossby number (R_O_) on the shape of the activity-rotation relation in LX/Lbol-R_O_ space, and we find that the slope in the unsaturated regime and the location of the break point of the dual power-law depend sensitively on the choice of R_O_.2020A&A...638A..20Mhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/638/A20CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/638/A20https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/638/A20http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/638/A20https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/638/A20https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/638/A20http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/638/A20GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/638/A20/tableb1 (Stellar parameters and activity-rotation properties for 288 stars (updated version, 23/12/2024))https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/638/A20/tableb1?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/638/A20/tableb1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/638/A20/tableb1?GETtext/xml+votable180.050000true2.0267747.950660.0055555555555555566/280 309-310 339-340 368 470 796 838 850 867 965 983 989 999 1066-1067 1079 1099 1122 1133 1146 1148 1159 1199 1205 1212 1255 1264 1511 1556 1559-1560 1571-1572 1599 1605 1611 1613 1646 1723 1819 1853 1890 1948 2321 2335 2422 2468 2494 2534 2597 2616 2660 2671 2747 2755-2756 2783 2793 2800 2858 2974 3031 3163 4015 4444 4468 4773 5119 5207 5319 5331 5387 5420 5438 5452 5532 5534 5590 5743 5787-5788 5802 5819 5822 5850 5853 5915 5917 5927 6231 6245 6295 6385 6410 6543 6561 6599 6606 6725 6836 6850 6894 6924 7189 7202 7264 7810 8170 8224 8440 8627 8733 8739 8915 9168 9281 9293-9294 9311 9316 9332 9445 9570 9599 9616 9681-9683 9687 9689 9712 9759 9770 9773 9797 9831 9844 9856 9902 9905 9912 9923 9926 9954 10005 10016 10027-10028 10035 10146 10149 10225 10303 10481 10490 10626 10771 10893 10905 10912 11015 12157 12683 12865 13157 13182 13451 13495 13536 13541 13548 13625 13713 13728 13750 13792 13795 13855 14266 14277 14781 14935 15010 15021 15028 15052 15062 15960 17019 17058 17124 18195 18496 18538 18553 18588 18634 18761 19466 20131 20291 22289 22510 22645 22873 22878 22964 23094 23140 23548 23564 23731 23857 23878 23887 23892 24004 24040 24053 24227 24288 24312-24313 24541 25192 25444 25793 25954 26133 26555 26972 27004 27201 27692 27694 27706 27792 28341 28646 28955 29196 29352 29939 30146 30176 30429 30729 30893 31229 31781 32104 32500 32505 32650 32676 32699-32700 32715 32743 33116 33937 35150 35950 36483 36511 37419 38247 38430 38551 41591 42420 42903 44371 45269 45607 45803 46598 47347 48274 48500https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/638/A20?format=asciiX-raydefaultJ/A+A/638/A20/tableb1Stellar parameters and activity-rotation properties for 288 stars (updated version, 23/12/2024)RadiusStellar radiussolRadphys.angSize;srcfloate_RadiusError on stellar radiussolRadstat.error;phys.size.radiusfloatlog(Lbol)Bolometric luminosity from Gaia distancelog(solLum)phys.luminosityfloatlog(e_Lbol)Error on the bolometric luminositylog(solLum)phys.luminosityfloatV-JV-J from UCAC4 and 2MASS catalogsmagphot.color;em.opt.V;em.IR.JfloatProtRotational period from K2 lightcurvesdtime.periodfloatlog(LX)X-ray luminositylog(1e-07W)phys.luminosity;em.X-rayfloatlog(e_LX)? Error on the X-ray luminositylog(1e-07W)phys.luminosity;em.X-rayfloatnullablelog(LX/Lbol)X-ray factional luminosity in logarithmic scalephys.luminosity;arith.ratiofloatlog(e_LX/Lbol)? Error on the X-ray fractional luminositystat.error;phys.luminosity;em.X-rayfloatnullableRo-CS11? Rossby number from Eq.36 in Cranmer & Saar, 2011ApJ...741...54Cstat.paramdoublenullableRo-Brun17? Rossby number from Eq.33 in Brun et al., 2017ApJ...836..192Bstat.paramdoublenullableRo-Wr18Rossby number from Eq.5 in Wright et al., 2018MNRAS.479.2351Wstat.paramdoubleDistDistancepcpos.distancefloate_DistError on distancepcstat.errorfloatFlagGaiaQuality flag from Lindegren et al., 2018A&A...616A...2L and this paper criteria (2)meta.code.errorcharl_log(LX/Lbol)[0/1] Undetected X-ray source (3)meta.code.errorcharSNameSimbad namemeta.idcharRAJ2000Simbad right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Simbad declination (J2000)degpos.eq.dec;meta.mainSeqSequential numbermeta.recordintName2Common namemeta.idcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRefCatalogs references (1)meta.refcharNameName of the source from SIMBADmeta.id;meta.maincharKsMAGAbsolute magnitude in K-bandmagphys.magAbsfloate_KsMAGError on the absolute magnitude in K-bandmagstat.errorfloatMassStellar masssolMassphys.massfloate_MassError on stellar masssolMassstat.error;phys.massfloat