J/ApJ/897/L10ivo://CDS.VizieR/J/ApJ/897/L10doi:10.26093/cds/vizier.18979010CDSHayakawa H.Ribeiro P.Vaquero J.M.Gallego M.C.Knipp D.J.,Mekhaldi F.Bhaskar A.Oliveira D.M.Notsu Y.Carrasco V.M.S.,Caccavari A.Veenadhari B.Mukherjee S.Ebihara Y.2021-11-15T09:20:23Z2021-10-21T08:52:34ZCDS support team

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

cds-question@unistra.frsolar-systemthe-sunstellar-flaresmagnetic-fieldsWhile the Sun is generally more eruptive during its maximum and declining phases, observational evidence shows certain cases of powerful solar eruptions during the quiet phase of solar activity. Occurring in the weak Solar Cycle 14 just after its minimum, the extreme space weather event in 1903 October-November is one of these cases. Here, we reconstruct the time series of geomagnetic activity based on contemporary observational records. With the mid-latitude magnetograms, the 1903 magnetic storm is thought to be caused by a fast coronal mass ejection (~1500km/s) and is regarded as a superstorm with an estimated minimum of the equivalent disturbance storm time index (Dst') of ~-531nT. The reconstructed time series has been compared with the equatorward extension of auroral oval (~44.1 in invariant latitude) and the time series of telegraphic disturbances. This case study shows that potential threats posed by extreme space weather events exist even during weak solar cycles or near their minima.2020ApJ...897L..10Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/897/L10CatalogResearchIsServedByTAP VizieR generic servicerelated-toB/planets : VizieR Solar system catalogues (CDS & ObsParis, 2018-)J/ApJ/747/L41 : Solar flares probabilities (Bloomfield+, 2012)J/ApJ/752/126 : Modeling the magnetic field in solar corona (Yamamoto+, 2012)J/ApJ/757/94 : Solar flares observed with GOES and AIA (Aschwanden, 2012)J/ApJ/774/L27 : Solar flares predictors (Yang+, 2013)J/A+A/562/L10 : Solar activity reconstructed for 3 millennia (Usoskin+, 2014)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/897/L10https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/897/L10http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/897/L10https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/897/L10https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/897/L10http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/897/L10GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJ/897/L10/table1Reference stations used in this articlerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintObsObservatorymeta.id;instr.obstycharLATGeographic latitudedegpos.earth.latcharLONGeographic longitudedegpos.earth.loncharMLATMagnetique latitudedegpos.earth.latcharMLONMagnetique longitudedegpos.earth.lonchardTTime difference with GMTtime.epoch;arith.diffcharRange[570/777] Maximum {Delta}H range (1)pos.earth.latintRefReferences (2)meta.refcharJ/ApJ/897/L10/fig4Hourly D0(t)/cos{lambda} of four reference stations and the Dst' reconstructed time seriesrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintObsObservation date, monthtime.epoch;obsHourHour of observation, GMThtime.epochintD0RawCOI[-348/80]? Disturbance, Coimbra, {Delta}HnTphys.magFieldfloatnullableD0RawCLA[-564/72.3]? Disturbance, Colaba, {Delta}HnTphys.magFieldfloatnullableD0RawCUA[-439/-1.55]? Disturbance, Cuajimalpa, {Delta}HnTphys.magFieldfloatnullableD0RawZKW[-554/44.1]? Disturbance, Zi-ka-wei, {Delta}HnTphys.magFieldfloatnullableD0CorCOI[-492/114]? Disturbance, Coimbra, {Delta}H with latitude-correctionnTphys.magFieldfloatnullableD0CorCLA[-572/73.4]? Disturbance, Colaba, {Delta}H with latitude-correctionnTphys.magFieldfloatnullableD0CorCUA[-509/-1.79]? Disturbance, Cuajimalpa, {Delta}H with latitude-correctionnTphys.magFieldfloatnullableD0CorZKW[-590/47]? Disturbance, Zi-ka-wei, {Delta}H with latitude-correctionnTphys.magFieldfloatnullableDst[-531/26] Reconstructed Disturbance storm time estimatenTphys.magFieldint