J/ApJ/891/54ivo://CDS.VizieR/J/ApJ/891/54doi:10.26093/cds/vizier.18910054CDSLing A.G.Kahler S.W.2021-10-04T14:16:13Z2021-09-07T08:05:59ZCDS support team

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

cds-question@unistra.frthe-sunstellar-flaresx-ray-sourcesWe recently repeated an earlier analysis by Garcia showing that large (>=M3.0) solar X-ray flares associated with solar energetic particle (SEP) events have significantly lower peak X-ray flux ratios R=(0.04-0.5nm)/(0.1-0.8nm), proxies for flare peak temperatures, than those without SEP events. As we expect SEP events to be produced by shocks ahead of fast coronal mass ejections (CMEs), a smaller R for an X-ray flare of a given peak flux Fp should also be more likely to be accompanied by a fast (Vcme>1000km/s) CME. We confirm this expectation, examine the role played by the ratios R in correlations between Fp and CME speeds Vcme, and then compare CME widths W, Vcme, and R with each other. We consider an apparent conflict between a global scaling model of eruptive events showing Vcme scaling with higher R and our confirmation that the Garcia analysis implies that faster CMEs are associated with flares of lower R. The R values are examined for 16 large flares of the well-studied AR 12192, for which nearly all flares had no associated CMEs. Those flares share the same high values of R as other active region (AR) flares with no CMEs. We also find that small (<M3.0) flares of filament eruptions leading to SEP events share the lower R values of larger flares with fast CMEs.2020ApJ...891...54Lhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/891/54CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/A+A/304/563 : Cool X-ray flares of Sun with GOES (Phillips+, 1995)J/ApJ/831/105 : Global energetics of solar flares. IV. CME (Aschwanden, 2016)J/ApJ/833/284 : Quasi-periodic pulsations in solar flares (Inglis+, 2016)J/ApJ/871/16 : Sun active regions from 1976-2017 (Jiang+, 2019)J/ApJ/881/1 : Global energetics of solar flares. VIII. (Aschwanden+, 2019)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/891/54https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/891/54http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/891/54https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/891/54https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/891/54http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/891/54GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapX-raydefaultJ/ApJ/891/54/table3X-ray flares >M3 and associated coronal mass ejections (CMEs) and solar energetic particle (SEP) eventsR[0.15/0.69] Peak X-ray Ratiophot.flux;arith.ratiodoubleLocSolar Location of flaremeta.notecharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintEvent[1998/2017] Year of the flaretime.epochPeakHour of X-ray flare peaktime.epochClassFlare Classsrc.classcharVcme[113/3387]? CME Speedkm/sphys.velocintnullableWidth[11/360]? CME Widthdegphys.angSize;srcintnullableDay[1/31]? SEP Onset daydtime.epochintnullableHour? SEP Onset UT hourhtime.epochintnullableIp[1.4/8000]? SEP Peak intensity (1)em.X-ray;stat.maxfloatnullable