RCM-E and AMIE studies of the Harang reversal formation during a steady magnetospheric convection event

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dc.citation.firstpage7228en_US
dc.citation.issueNumber9en_US
dc.citation.journalTitleJournal of Geophysical Research: Space Physicsen_US
dc.citation.lastpage7242en_US
dc.citation.volumeNumber119en_US
dc.contributor.authorYang, Jianen_US
dc.contributor.authorToffoletto, Franken_US
dc.contributor.authorLu, Gangen_US
dc.contributor.authorWiltberger, Michaelen_US
dc.date.accessioned2015-12-18T19:47:52Zen_US
dc.date.available2015-12-18T19:47:52Zen_US
dc.date.issued2014en_US
dc.description.abstractThis paper presents the results of a modeling study on the formation of the Harang reversal (HR) during a steady magnetospheric convection event. The Harang reversal is identified as the boundary of the northward and southward electric field in the nightside auroral zone using the Assimilative Mapping of Ionospheric Electrodynamics (AMIE) procedure. We simulate the event with the Rice Convection Model-Equilibrium (RCM-E) by adjusting its boundary conditions to approximately match Time History of Events and Macroscale Interactions during Substorms (THEMIS) and GOES observations in the nightside magnetosphere. Our results show that the HR is collocated with an upward region 1 field-aligned current, where converging ionospheric currents cause a southward/northward electric field on the poleward/equatorward side of the HR. Our results also indicate that the electric field reversal is slightly poleward of the ionospheric east–west current reversal and is to the northeast of the ground magnetic reversal, which is consistent with previous observations. We also test the sensitivity of the HR formation to a variety of parameters in the RCM-E simulations. We find that (1) the reduction of the flux tube entropy parameter PV5/3 near the midnight sector plays a major role in the formation of the HR; (2) a run carried out assuming uniform conductance produced the same major features as the run with more realistic precipitation-enhanced conductance; and (3) the detailed pattern of the polar cap potential distribution plays a minor role, but its dawn-dusk asymmetry significantly controls the location of the HR with respect to midnight. The RCM-E simulations also predict PV5/3 and flow distributions associated with the magnetospheric source of the HR in the plasma sheet, which can be further tested against observations.en_US
dc.identifier.citationYang, Jian, Toffoletto, Frank, Lu, Gang, et al.. "RCM-E and AMIE studies of the Harang reversal formation during a steady magnetospheric convection event." <i>Journal of Geophysical Research: Space Physics,</i> 119, no. 9 (2014) Wiley: 7228-7242. http://dx.doi.org/10.1002/2014JA020207.en_US
dc.identifier.doihttp://dx.doi.org/10.1002/2014JA020207en_US
dc.identifier.urihttps://hdl.handle.net/1911/87474en_US
dc.language.isoengen_US
dc.publisherWileyen_US
dc.rightsArticle is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use.en_US
dc.titleRCM-E and AMIE studies of the Harang reversal formation during a steady magnetospheric convection eventen_US
dc.typeJournal articleen_US
dc.type.dcmiTexten_US
dc.type.publicationpublisher versionen_US
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