J/A+A/698/A180ivo://CDS.VizieR/J/A+A/698/A180doi:10.26093/cds/vizier.36980180CDSGalletta G.Colombo S.Prisinzano L.Micela G.2025-08-11T20:02:02Z2025-06-13T09:04:40ZCDS support team

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

cds-question@unistra.frdwarf-starsm-starsphotometryvisible-astronomyFlares are a form of stellar activity that occur over short timescales but produce highly energetic outbursts. Studying stellar flares is crucial because they can significantly alter the circumstellar environment by producing intense high-energy radiation. Understanding stellar flares is essential for clarifying the environment in which planets evolve, as flares can influence planetary atmospheres by driving photoevaporation and photochemical processes. M dwarfs are of significant interest due to their high flare activity rates and the potential presence of exoplanets within their habitable zones, whose atmospheres may be influenced by flare-emitted radiation. We aimed to define the flaring properties of an unbiased sample of M dwarfs with limited volume. Using data from the Transiting Exoplanet Survey Satellite (TESS), we characterized the frequency, energy distribution, and temporal properties of flares in nearby stars. We selected a volume-limited sample of M dwarfs within 10pc from Earth from the Gaia DR3 catalog. We analyzed TESS light curves using an iterative Gaussian process fitting technique to remove long-term stellar activity signals, enabling the identification and characterization of impulsive flare events. For each flare, we derived the amplitudes, timescales, and total energy emitted. We analyzed 173 stars and detected 17229 flares, with 0 to 76 flares per TESS sector. We examined the frequency and energy distribution of stellar flares using three representative stars to illustrate the diversity in flare activity. We observed flares with a minimum energy of ~10^29^erg and typical durations ranging from 2 to 8000 seconds. We modeled the cumulative flare energy distribution using one-slope and two-slope fits, yielding average slopes of -0.79+/-0.64 and -1.23+/-1.32, respectively. We defined the Flare Energy Index (GF.01) to characterize the flare frequency and revealed two distinct populations. Fainter stars exhibited fewer high-energy flares, whereas brighter stars exhibited more frequent low-energy flares. We analyzed two highly active stars with the largest number of TESS sectors, G 227-22 and G 258-33, were analyzed over a long time baseline to explore their flare properties and energy distributions.2025A&A...698A.180Ghttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/698/A180CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toIV/39 : TESS Input Catalog version 8.2 (TIC v8.2) (Paegert+, 2021)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/698/A180https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/698/A180http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/698/A180https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/698/A180https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/698/A180http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/698/A180GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/A+A/698/A180/stars (List of targets)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/A+A/698/A180/stars?https://vizier.iucaa.in/viz-bin/conesearch/J/A+A/698/A180/stars?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/A+A/698/A180/stars?GETtext/xml+votable180.050000true259.7623333-46.63697220.0055555555555555566/22 131 250 309 527 546 725 811 2737 3005 3345 3715 3751 3791 4444 4462 4867 5000 5333 5420 5534 5590 6552 6672 6726 6894 6974 7103 7264 7395 7512 8023 8123 8281 8440 9585 9629 10037 10149 10448 11496 11636 12679 12865 13451 13688 13743 13875 14772 14858 15311 15346 15355 15548 15602 15960 16041 16391 16502 16754 16758 17058 17348 18268 18496 18666 19466 20071 20100 20459 20507 20896 21149 21151 21953 22014 22289 22309 22645 22709 22739 22807 23047 23564 23735 23867 23910 23997 24227 24616 24713 25009 26279 26327 26487 26538 26560 26583 26972 27201 27289 27392 27459 27462 27762 28343 28548 28646 30505 32115 32229 32335 33533 33655 33964 34181 34448 34535 35247 35670 36511 36614 36971 37122 37257 37332 37379 38322 38456 38551 39331 40250 40496 40505 40623 40941 41591 42054 42255 42285 42290 42314 42528 42652 42784 43187 43411 43413 43580 43598 43723 44921 45322 45752 46566 46632 46718 46776 47061 47347 47414 48173 48274https://cdsarc.cds.unistra.fr/viz-bin/moc/J/A+A/698/A180?format=asciiOpticaldefaultJ/A+A/698/A180/starsList of targetsrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of the target starmeta.id;meta.maincharRAJ2000Simbad right ascension (J2000)pos.eq.ra;meta.mainDEJ2000Simbad declination (J2000)pos.eq.dec;meta.mainSimbadSimbad column added by the CDSmeta.ref.urlcharJ/A+A/698/A180/table3Table of TESS sector activityrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNameName of the target starmeta.id;meta.maincharSectorTESS sector (e.g., "s39", "s2", etc.)meta.idcharFlareNumber of flares detectedmeta.numberintLbolBolometric luminositysolLumphys.luminositydoublee_LbolBolometric luminosity errorsolLumstat.errordoubleSlopeSlope of the flare distributionarith.gradfloate_SlopeSlope of the flare distribution errorstat.errorfloatEBreak? Break energy in erg1e-07Wphys.energydoublenullable