J/ApJ/924/43ivo://CDS.VizieR/J/ApJ/924/43doi:10.26093/cds/vizier.19240043CDSChen YuHu Q.2023-10-18T12:34:53Z2023-09-13T14:32:40ZCDS support team

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

cds-question@unistra.frthe-sunmagnetic-fieldsWe report small-scale magnetic flux ropes via the in situ measurements from the Parker Solar Probe during the first six encounters, and present additional analyses to supplement our prior work in Chen+ (2021ApJ...914..108C). These flux ropes are detected by the Grad-Shafranov-based algorithm, with their durations and scale sizes ranging from 10s to <~1hr and from a few hundred kilometers to 10^-3^au, respectively. They include both static structures and those with significant field-aligned plasma flows. Most structures tend to possess large cross helicity, while the residual energy is distributed over wide ranges. We find that these dynamic flux ropes mostly propagate in the antisunward direction relative to the background solar wind, with no preferential signs of magnetic helicity. The magnetic flux function follows a power law and is proportional to scale size. We also present case studies showing reconstructed two-dimensional (2D) configurations, which confirm that both the static and dynamic flux ropes have a common configuration of spiral magnetic field lines (also streamlines). Moreover, the existence of such events hints at interchange reconnection as a possible mechanism for generating flux rope-like structures near the Sun. Lastly, we summarize the major findings, and discuss the possible correlation between these flux rope-like structures and turbulence due to the process of local Alfvenic alignment.2022ApJ...924...43Chttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJ/924/43CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/ApJ/737/L35 : Pulsed Alfven waves in the solar wind (Gosling+, 2011)J/ApJS/230/21 : Solar wind 3D magnetohydrodynamic simulation (Chhiber+, 2017)J/ApJS/239/12 : Small-scale magnetic flux ropes in the solar wind (Hu+, 2018)J/ApJ/871/93 : Solar wind speed from 5yr data with ACE (Wang+, 2019)J/A+A/635/A79 : Pitch-angle distributions of solar wind (Carcaboso+, 2020)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJ/924/43https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJ/924/43http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJ/924/43https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJ/924/43https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJ/924/43http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJ/924/43GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/ApJ/924/43/table3List of small-scale magnetic flux ropes (SFRs) and associated properties during the first six Parker Solar Probe (PSP) encountersrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintSeq[1/5841] Event index numbermeta.id;meta.mainintStEvent start date (UT)stime.startnullableEndEvent end date (UT)stime.endnullableDur[10/3697] Event durationstime.durationintBavg[25/151] Average magnetic field strengthnTphys.magField;phys.atmol.collStrengthfloatBetap[0.024/6.24] Average proton betastat.fit.paramfloatVSW[187.28/668.42] Average solar wind speedkm/sphys.veloc;stat.meanfloattheta[0/180] Polar angledegpos.posAngintphi[0/360]? Azimuthal angledegsrc.orbitalintnullablezaxis0[-0.985/0.985] Flux rope z-axis 0 component (1)stat.fit.paramfloatzaxis1[-0.97/0.97] Flux rope z-axis 1 component (1)stat.fit.paramfloatzaxis2[-1/1] Flux rope z-axis 2 component (1)stat.fit.paramfloatSize[0.39/596] Flux rope scale size1e-05AUsrc.morph.scLengthfloatWTS[-0.99/1.24] Walen test slopestat.fit.paramfloatMAavg[0.029/0.9] Average Alfvenic Mach numberphys.veloc;arith.difffloatRD[0.12/0.35] Heliocentric distance where event identifiedAUpos.distance;pos.heliocentricfloatCH[-0.985/0.992] Density of normalized cross helicity; {sigma}_c_phys.density;arith.ratiofloatRE[-0.998/-0.1] Density of normalized residual energy; {sigma}_r_phys.energy.densityfloatAm[-1.85/10.4] Extreme value of magnetic flux functionT.mstat.fit.paramfloat