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Properties of Magnetic Reconnection and FTEs on the Dayside Magnetopause With and Without Positive IMF Bx Component During Southward IMF
Univ Colorado, Lab Atmospher & Space Phys, Boulder, CO 80309 USA;Univ Helsinki, Dept Phys, Helsinki, Finland.
Univ Helsinki, Dept Phys, Helsinki, Finland.
NASA, Goddard Space Flight Ctr, Greenbelt, MD USA.
West Virginia Univ, Dept Phys & Astron, Morgantown, WV 26506 USA.
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2019 (English)In: Journal of Geophysical Research - Space Physics, ISSN 2169-9380, E-ISSN 2169-9402, Vol. 124, no 6, p. 4037-4048Article in journal (Refereed) Published
Abstract [en]

This paper describes properties and behavior of magnetic reconnection and flux transfer events (FTEs) on the dayside magnetopause using the global hybrid-Vlasov code Vlasiator. We investigate two simulation runs with and without a sunward (positive)B-x component of the interplanetary magnetic field (IMF) when the IMF is southward. The runs are two-dimensional in real space in the noon-midnight meridional (polar) plane and three-dimensional in velocity space. Solar wind input parameters are identical in the two simulations with the exception that the IMF is purely southward in one but tilted 45 degrees toward the Sun in the other. In the purely southward case (i.e., without B-x) the magnitude of the magnetos heath magnetic field component tangential to the magnetopause is larger than in the run with a sunward tilt. This is because the shock normal is perpendicular to the IMF at the equatorial plane, whereas in the other run the shock configuration is oblique and a smaller fraction of the total IMF strength is compressed at the shock crossing. Hence, the measured average and maximum reconnection rate are larger in the purely southward run. The run with tilted IMF also exhibits a north-south asymmetry in the tangential magnetic field caused by the different angle between the IMF and the bow shock normal north and south of the equator. Greater north-south asymmetries are seen in the FTE occurrence rate, size, and velocity as well; FTEs moving toward the Southern Hemisphere are larger in size and observed less frequently than FTEs in the Northern Hemisphere.

Place, publisher, year, edition, pages
2019. Vol. 124, no 6, p. 4037-4048
National Category
Fusion, Plasma and Space Physics
Identifiers
URN: urn:nbn:se:uu:diva-392051DOI: 10.1029/2019JA026821ISI: 000477723100013OAI: oai:DiVA.org:uu-392051DiVA, id: diva2:1349870
Funder
EU, European Research Council, 200141-QuESpaceEU, European Research Council, 682068-PRESTISSIMOAvailable from: 2019-09-10 Created: 2019-09-10 Last updated: 2019-09-10Bibliographically approved

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Dimmock, Andrew P.

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