J/MNRAS/523/2193ivo://CDS.VizieR/J/MNRAS/523/2193doi:10.26093/cds/vizier.75232193CDSLiu Q.Lin J.Wang X.Gu S.Shi J.Zhang L.Xi G.Mo J.Cai Y.,Chen L.Chen Z.Guo F.Jiang X.Li G.Li W.Lin H.Lin W.Liu J.,Miao C.Ma X.Peng H.Xiang D.Yan S.Zhang J.Zhang X.2026-01-30T20:02:50Z2023-06-05T09:45:52ZCDS support team

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

cds-question@unistra.frsurveysstellar-flaresvisible-astronomystellar-spectral-typesTsinghua University-Ma Huateng Telescopes for Survey (TMTS) aims to detect fast-evolving transients in the Universe, which has led to discovery of thousands of short period variables and eclipsing binaries since 2020. In this paper, we present the observed properties of 125 flare stars identified by the TMTS within the first two years, with an attempt to constrain their eruption physics. As expected, most of these flares were recorded in late-type red stars with G_BP_-G_RP_>2.0mag, however, the flares associated with blue stars of them tend to be on average more energetic and have broader profiles. The peak flux (F_peak_) of the flare is found to depend strongly on the equivalent duration (ED) of the energy release, i.e., F_peak_{pro.to}ED^0.72+/-0.04^, which is consistent with the results derived from the Kepler and Evryscope samples. This relation is likely related to the magnetic loop emission, while for the more popular non-thermal electron heating model a specific time evolution may be required to generate this relation. We notice that flares produced by hotter stars have a flatter F_peak_{pro.to}ED relation compared to that from cooler stars, which is related to the statistical discrepancy in light-curve shape of flare events with different colors. With the spectra from the LAMOST, we found that flare stars have apparently stronger H{alpha} emission than inactive stars, especially at low temperature end, suggesting that chromospheric activity plays an important role in producing flares. On the other hand, the subclass having frequent flares are found to show H{alpha} emissions of similar strength in their spectra as that recorded with only a single flare but similar effective temperature, implying that the chromospheric activity may not be the only reason of triggering eruptions.2023MNRAS.523.2193Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/523/2193CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toJ/MNRAS/523/2172 : TMTS delta Scuti stars (Lin+, 2023)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/MNRAS/523/2193https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/MNRAS/523/2193http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/MNRAS/523/2193https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/MNRAS/523/2193https://vizier.iucaa.in/viz-bin/votable?-source=J/MNRAS/523/2193http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/MNRAS/523/2193GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/MNRAS/523/2193/table1 (Summary of properties of 125 flare stars from the first two-year survey of TMTS)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/MNRAS/523/2193/table1?https://vizier.iucaa.in/viz-bin/conesearch/J/MNRAS/523/2193/table1?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/MNRAS/523/2193/table1?GETtext/xml+votable180.050000true4.59088011864.311050830.0055555555555555566/18 327 345 351 823 886 895 958 994 1033 1107 1151 1252 1255 1267 1327 1459 1464 1506 1572 1585 1593 1622 1642 1666 1684 1710 1785 1868 1910 1996 2022 2374 2417 2452 2488 2594 2834 2836 2906 2910 3031 3068 3082 3086 3088 3157 3183 3196 3278 3722 3730 3893 3969 3982 4328 4330 4339 4344 4507 4867 4870 4952 5441 6084 6435 6534 6556 6699 6749 6791 6820 6827 6887 6904 7693 9009 9111 9408 10339 10372 10394 10508 10692 11162 11186 11460 11462 14258 14353-14354 14364 15355 15622 15629 20348 21953 21959 21971 22195 22258 22383 22387 22398 22892 22980-22981 22995 23572 23699 23771 24200 24285 24326 24382 24423 24440 26369 27421 28147 28646 32509https://cdsarc.cds.unistra.fr/viz-bin/moc/J/MNRAS/523/2193?format=asciiOpticaldefaultJ/MNRAS/523/2193/table1Summary of properties of 125 flare stars from the first two-year survey of TMTSrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameTMTS name of the source (TMTS JHHMMSSss+DDMMSSs)meta.id;meta.maincharn_Name[*] Note on Name (G1)meta.notecharRAJ2000[4.59/337.34] Right Ascension (J2000)degpos.eq.ra;meta.mainDEJ2000[0.89/76.4] Declination (J2000)degpos.eq.dec;meta.mainSpTypeSpectra typemeta.notecharPlx[0.09/128.49]? Parallax of the sourcemaspos.parallaxfloatnullablee_Plx[0.02/1.29]? Uncertainty in parallaxmasstat.error;pos.parallaxfloatnullableDist[0.01/1.5]? Distance of the sourcekpcpos.distancedoublenullablee_Dist[0.0/0.3]? Uncertainty in distancekpcstat.errordoublenullableSimbadSimbad column added by the CDSmeta.ref.urlcharGMAG[4.3/12.317]? Absolute G-band magnitudemagphot.magfloatnullablee_GMAG[0.0011/0.4]? Uncertainty in absolute G-band magnitudemagstat.errorfloatnullableBP-RP[0.78/3.32]? Gaia color with reddening-removedmagphot.color;em.opt.B;em.opt.Rfloatnullablee_BP-RP[0.0013/0.09]? Uncertainty in Gaia colormagstat.errorfloatnullableTeff[3202.26/5913.13]? Effective temperature of the sourceKphys.temperature.effectivefloatnullablee_Teff[38.08/344.36]? Uncertainty in effective temperatureKstat.error;phys.temperature.effectivefloatnullablelogg[2.09/5.5]? logarithmic form of surface gravitylog(cm.s**-2)phys.gravityfloatnullablee_logg[0.05/0.5]? Uncertainty in logglog(cm.s**-2)stat.errorfloatnullable[Fe/H][-1.1/0.09]? Iron abundancephys.abund.Fefloatnullablee_[Fe/H][0.04/0.3]? Uncertainty in iron abundancestat.error;phys.abund.FefloatnullableEWHa[-1.48/10.0]? Equivalent width of H{alpha} line0.1nmspect.line.eqWidthfloatnullablee_EWHa[0.06/0.9]? Uncertainty in EWHa0.1nmstat.errorfloatnullableJ/MNRAS/523/2193/table2Summary of the flare parameters for 125 flare stars from the first two-year survey of TMTSn_Name[*] Note on Name (G1)meta.notecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameTMTS name of the source (TMTS JHHMMSSss+DDMMSSs)meta.id;meta.maincharTimeStart[58856/59579]? Time when TMTS observation started (MJD)dtime.epochdoublenullableFPeak[0.053/33.36] Fractional flux of flare peakphot.flux;arith.ratiofloate_FPeak[0.006/4.39] Uncertainty in Peak_fluxstat.errorfloatt0[-44/40973] Time of flare beginning since TimeStartstime;arith.diffdoublee_t0[6.21/1546.88] Uncertainty in t0sstat.errorfloatt1/2[38.21/1699.98]? Full-time width at half peak fluxstime.epochfloatnullablee_t1/2[5.25/355.62]? Uncertainty in t1/2sstat.errorfloatnullableDur[487.14/13787.71] Duration of the flarestime.durationdoublee_Dur[36.12/7718.42] Uncertainty in Dursstat.errorfloatED[12.98/6600.62] Equivalent durationstime.durationfloate_ED[1.96/2877.63] Uncertainty in EDsstat.errorfloatlogEL[31.58/35.88]? log of white-band energylog(1e-07W)phys.energyfloatnullablee_logEL[0.012/0.3]? Uncertainty in logELlog(1e-07W)stat.errorfloatnullablelogEbol[32.12/36.42]? log of bolometric energylog(1e-07W)phys.energyfloatnullablee_logEbol[0.012/0.3]? Uncertainty in logEbollog(1e-07W)stat.errorfloatnullable