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

Journal Article · · Journal of Geophysical Research. Space Physics
DOI:https://doi.org/10.1029/2021ja029979· OSTI ID:1978532

Here, using 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-⟂) 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 ~ ion skin depth and normal magnetic field Bn≈0 is formed by a shock compression process as the RD interacts with the Q-⟂ 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-⟂ 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.

Research Organization:
Auburn Univ., AL (United States)
Sponsoring Organization:
USDOE Office of Science (SC)
Grant/Contract Number:
SC0018071; FOA-0001664
OSTI ID:
1978532
Journal Information:
Journal of Geophysical Research. Space Physics, Vol. 126, Issue 12; ISSN 2169-9380
Publisher:
American Geophysical UnionCopyright Statement
Country of Publication:
United States
Language:
English

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