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Properties of Magnetic Reconnection and FTEs on the Dayside Magnetopause With and Without Positive IMF Bx Component During Southward IMF

Properties of Magnetic Reconnection and FTEs on the Dayside Magnetopause With and Without Positive IMF Bx Component During Southward IMF
Properties of Magnetic Reconnection and FTEs on the Dayside Magnetopause With and Without Positive IMF Bx Component During Southward IMF

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) Bx 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° toward the Sun in the other. In the purely southward case (i.e., without Bx) the magnitude of the magnetosheath 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.

flux transfer event, hybrid-Vlasov, magnetic reconnection, magnetopause, numerical modeling
2169-9380
Hoilijoki, S.
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Ganse, U.
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Sibeck, D. G.
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Cassak, P. A.
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Turc, L.
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Battarbee, M.
48baf4c9-f9dd-44f6-89e5-74775883f66a
Fear, R. C.
8755b9ed-c7dc-4cbb-ac9b-56235a0431ab
Blanco-Cano, X.
f9b77158-e499-4568-961e-ea4defc8fd8a
Dimmock, A. P.
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Kilpua, E. K.J.
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Jarvinen, R.
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Juusola, L.
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Pfau-Kempf, Y.
3de39040-e983-4df8-bd86-675073991614
Palmroth, M.
8a0f55b3-8eed-43b1-97dc-60b8b26e058d
Hoilijoki, S.
f04ec08e-8b58-4cde-8516-810d8627464d
Ganse, U.
25d8c4de-5293-4a74-b97b-9072056585e8
Sibeck, D. G.
6004631a-1492-4a41-89dd-5296d8e324d2
Cassak, P. A.
d26a5fc1-c3c0-465e-8402-cbd556db2438
Turc, L.
5fcf17c5-c395-4008-9cf5-f89068cd73a9
Battarbee, M.
48baf4c9-f9dd-44f6-89e5-74775883f66a
Fear, R. C.
8755b9ed-c7dc-4cbb-ac9b-56235a0431ab
Blanco-Cano, X.
f9b77158-e499-4568-961e-ea4defc8fd8a
Dimmock, A. P.
c6c79aa9-e9a4-4ed0-8576-0ded64545417
Kilpua, E. K.J.
21ac6c5c-d312-4c52-bed3-f0eb8816e951
Jarvinen, R.
786315de-57e0-47b0-9d76-d883aad03eb0
Juusola, L.
c0689612-21cb-4f50-a53c-09495159f003
Pfau-Kempf, Y.
3de39040-e983-4df8-bd86-675073991614
Palmroth, M.
8a0f55b3-8eed-43b1-97dc-60b8b26e058d

Hoilijoki, S., Ganse, U., Sibeck, D. G., Cassak, P. A., Turc, L., Battarbee, M., Fear, R. C., Blanco-Cano, X., Dimmock, A. P., Kilpua, E. K.J., Jarvinen, R., Juusola, L., Pfau-Kempf, Y. and Palmroth, M. (2019) Properties of Magnetic Reconnection and FTEs on the Dayside Magnetopause With and Without Positive IMF Bx Component During Southward IMF. Journal of Geophysical Research: Space Physics. (doi:10.1029/2019JA026821).

Record type: Article

Abstract

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) Bx 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° toward the Sun in the other. In the purely southward case (i.e., without Bx) the magnitude of the magnetosheath 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.

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Accepted/In Press date: 22 April 2019
e-pub ahead of print date: 1 May 2019
Keywords: flux transfer event, hybrid-Vlasov, magnetic reconnection, magnetopause, numerical modeling

Identifiers

Local EPrints ID: 432105
URI: https://eprints.soton.ac.uk/id/eprint/432105
ISSN: 2169-9380
PURE UUID: 746bd32b-f449-48fd-9bc3-db7fd6bb2e4e
ORCID for R. C. Fear: ORCID iD orcid.org/0000-0003-0589-7147

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Date deposited: 02 Jul 2019 16:30
Last modified: 03 Dec 2019 05:01

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Contributors

Author: S. Hoilijoki
Author: U. Ganse
Author: D. G. Sibeck
Author: P. A. Cassak
Author: L. Turc
Author: M. Battarbee
Author: R. C. Fear ORCID iD
Author: X. Blanco-Cano
Author: A. P. Dimmock
Author: E. K.J. Kilpua
Author: R. Jarvinen
Author: L. Juusola
Author: Y. Pfau-Kempf
Author: M. Palmroth

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