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Magnetic Reconnection Inside Solar Wind Rotational Discontinuity During Its Interaction With the Quasi-Perpendicular Bow Shock and Magnetosheath


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dc.contributorZhifang Guo, guozf@mail.iggcas.ac.cnen_US
dc.creatorGuo, Zhifang
dc.creatorLin, Yu
dc.creatorWang, Xueyi
dc.creatorDu, Aimin
dc.date.accessioned2022-10-12T13:28:06Z
dc.date.available2022-10-12T13:28:06Z
dc.date.created2021
dc.identifier10.1029/2021JA029979en_US
dc.identifier.urihttps://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2021JA029979en_US
dc.identifier.urihttps://aurora.auburn.edu/handle/11200/50388
dc.identifier.urihttp://dx.doi.org/10.35099/aurora-456
dc.description.abstractUsing a three-dimensional global hybrid simulation, we investigate the formation and evolution of ion-scale magnetic reconnection inside an interplanetary rotational discontinuity (RD) owing to its interaction with the quasi-perpendicular (Q-perpendicular to) bow shock and the magnetosphere. The interplanetary magnetic field (IMF) is initially predominantly northward, while it changes to purely southward across the RD. A significantly thinned RD current layer with a width similar to ion skin depth and normal magnetic field B-n approximate to 0 is formed by a shock compression process as the RD interacts with the Q-perpendicular to shock. Magnetic reconnection thereupon takes place inside the thin RD current layer, where Hall magnetic and electric fields, reconnection electric field, and high-speed ion outflow jets are identified. Simultaneously, flux ropes form with an extension of a few ion inertial lengths. As the RD is transmitted into the magnetosheath, multiple reconnection sites lead to the formation of longer flux ropes. Moreover, magnetosheath reconnection is also found at new reconnection sites inside the RD. No reconnection is found in the Q-perpendicular to shock alone outside the RD. The flux ropes propagate poleward and tailward in the magnetosheath. In addition, magnetopause reconnection takes place under the southward IMF on the sunward side of the RD after the RD passes through the magnetopause.en_US
dc.formatPDFen_US
dc.publisherAmerican Geophysical Unionen_US
dc.relation.ispartofJournal of Geophysical Research: Space Physicsen_US
dc.relation.ispartofseries2169-9380en_US
dc.rights©American Geophysical Union 2021. This is this the version of record co-published by the American Geophysical Union and John Wiley & Sons, Inc. It is made available under the CC-BY-NC-ND 4.0 license. Item should be cited as: Guo, Zhifang, et al. "Magnetic Reconnection Inside Solar Wind Rotational Discontinuity During Its Interaction With the Quasi‐Perpendicular Bow Shock and Magnetosheath." Journal of Geophysical Research: Space Physics 126.12 (2021): e2021JA029979.en_US
dc.subjectfield reconnectionen_US
dc.subjectmagnetopauseen_US
dc.subjectaccelerationen_US
dc.titleMagnetic Reconnection Inside Solar Wind Rotational Discontinuity During Its Interaction With the Quasi-Perpendicular Bow Shock and Magnetosheathen_US
dc.typeTexten_US
dc.type.genreJournal Article, Academic Journalen_US
dc.citation.volume126en_US
dc.citation.issue12en_US
dc.citation.spagee2021JA029979en_US
dc.description.statusPublisheden_US
dc.description.peerreviewYesen_US
dc.creator.orcid0000-0002-3728-6319en_US

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