J/ApJS/239/12ivo://CDS.VizieR/J/ApJS/239/12doi:10.26093/cds/vizier.22390012CDSHu Q.Zheng J.Chen Yule Roux J.Zhao L.2019-03-26T14:44:53Z2019-02-14T09:18:59ZCDS support team

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

cds-question@unistra.frmagnetic-fieldsthe-sunWe have developed a new automated small-scale magnetic flux ropes (SSMFR) detection algorithm based on the Grad-Shafranov (GS) reconstruction technique. We have applied this detection algorithm to the Wind spacecraft in situ measurements during 1996-2016, covering two solar cycles, and successfully detected a total number of 74241 small-scale magnetic flux rope events with duration from 9 to 361min. This large number of small-scale magnetic flux ropes has not been discovered by any other previous studies through this unique approach. We perform statistical analysis of the small-scale magnetic flux rope events based on our newly developed database, and summarize the main findings as follows. (1) The occurrence of small-scale flux ropes has strong solar-cycle dependency with a rate of a few hundred per month on average. (2) The small-scale magnetic flux ropes in the ecliptic plane tend to align along the Parker spiral. (3) In low-speed (<400km/s) solar wind, the flux ropes tend to have lower proton temperature and higher proton number density, while in high-speed (>=400km/s) solar wind, they tend to have higher proton temperature and lower proton number density. (4) Both the duration and scale size distributions of the small-scale magnetic flux ropes obey a power law. (5) The waiting time distribution of small-scale magnetic flux ropes can be fitted by an exponential function (for shorter waiting times) and a power-law function (for longer waiting times). (6) The wall-to-wall time distribution obeys double power laws with the break point at 60 minutes (corresponding to the correlation length). (7) The small-scale magnetic flux ropes tend to accumulate near the heliospheric current sheet (HCS).2018ApJS..239...12Hhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/239/12CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/ApJ/737/L35 : Pulsed Alfven waves in the solar wind (Gosling+, 2011)http://fluxrope.info/ : Small-scale Magnetic Flux Rope Databasehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJS/239/12https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJS/239/12http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJS/239/12https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJS/239/12https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJS/239/12http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJS/239/12GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJS/239/12/table3Flux rope eventsVsw[188/911] Solar wind velocitykm/sphys.velocdoublerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeq[0/74240] Index identifiermeta.idintObs.SObservation start; mm/dd/yyyy hh:mmtime.epochnullableObs.EObservation end; mm/dd/yyyy hh:mmtime.epochnullableTime[9/361] Observation durationmintime.intervalintResDif[0/0.2] Residual (1)stat.fit.residualdoubleBavg[5/123.4] Average magnetic field strengthnTphys.magFielddoubleBmax[5/138] Maximum magnetic field strengthnTphys.magField;phys.atmol.collStrengthdoublebeta[0.0003/120]? Average plasma {beta} valuestat.fit.paramdoublenullablebetap[5.2e-06/129]? Average proton {beta} valuestat.fit.paramdoublenullableTpAvg[0.002/1.1]? Average proton temperatureMKphys.temperaturedoublenullabletheta[0/180] Polar angledegpos.posAngintphi[0/360]? Azimuthal angledegpos.posAngintnullablezAxis0[-1/1] Z-axis orientation_0_ (2)pos.framedoublezAxis1[-1/1] Z-axis orientation_1_ (2)pos.framedoublezAxis2[-1/1] Z-axis orientation_2_ (2)pos.framedoubleSize[4.7e-05/0.11] Scale sizeAUsrc.morph.scLengthdoubleNp[0.03/99] Mean proton number densitycm**-3meta.number;phys.density;stat.meandouble