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Global MHD simulations of the Response of Jupiter’s Magnetosphere and Ionosphere to Changes in the Solar Wind and IMF
dc.contributor.authorSarkango, Yash
dc.contributor.authorJia, Xianzhe
dc.contributor.authorToth, Gabor
dc.date.accessioned2019-09-30T15:31:37Z
dc.date.availableWITHHELD_11_MONTHS
dc.date.available2019-09-30T15:31:37Z
dc.date.issued2019-07
dc.identifier.citationSarkango, Yash; Jia, Xianzhe; Toth, Gabor (2019). "Global MHD simulations of the Response of Jupiter’s Magnetosphere and Ionosphere to Changes in the Solar Wind and IMF." Journal of Geophysical Research: Space Physics 124(7): 5317-5341.
dc.identifier.issn2169-9380
dc.identifier.issn2169-9402
dc.identifier.urihttps://hdl.handle.net/2027.42/151316
dc.description.abstractWe have developed a new global magnetohydrodynamic (MHD) model for Jupiter’s magnetosphere based on the BATSRUS code and an ionospheric electrodynamics solver. Our model includes the Io plasma torus at its appropriate location and couples the global magnetosphere with the planetary ionosphere through field‐aligned currents. Through comparisons with available particle and field observations as well as empirical models, we show that the model captures the overall configuration of the magnetosphere reasonably well. In order to understand how the magnetosphere responds to different solar wind drivers, we have carried out time‐dependent simulations using various kinds of upstream conditions, such as a forward shock and a rotation in the interplanetary magnetic field (IMF). Our model predicts that compression of the magnetosphere by a forward shock of typical strength generally weakens the corotation enforcement currents on the dayside and produces an enhancement on the nightside. However, the global response varies depending on the IMF orientation. A forward shock with a typical Parker‐spiral IMF configuration has a larger impact on the magnetospheric configuration and large‐scale current systems than with a parallel IMF configuration. Plasmoids are found to form in the simulation due to tail reconnection and have complex magnetic topology, as they evolve and propagate down tail. For a fixed mass input rate in the Io plasma torus, the frequency of plasmoid occurrence in our simulation is found to vary depending on the upstream solar wind driving.Key PointsA new global MHD model is introduced for Jupiter’s magnetosphere that self‐consistently includes the Io plasma torus at the right locationTime‐dependent simulations show that the global magnetosphere responds differently to different types of drivers in the solar windPlasmoids form in the tail with occurrence frequency dependent on the external driving
dc.publisherCambridge University Press
dc.publisherWiley Periodicals, Inc.
dc.subject.otherJupiter
dc.subject.otherplasmoid
dc.subject.otheraurora
dc.subject.othersimulation
dc.subject.othermagnetosphere
dc.subject.otherMHD
dc.titleGlobal MHD simulations of the Response of Jupiter’s Magnetosphere and Ionosphere to Changes in the Solar Wind and IMF
dc.typeArticle
dc.rights.robotsIndexNoFollow
dc.subject.hlbsecondlevelAstronomy and Astrophysics
dc.subject.hlbtoplevelScience
dc.description.peerreviewedPeer Reviewed
dc.description.bitstreamurlhttps://deepblue.lib.umich.edu/bitstream/2027.42/151316/1/jgra55090.pdf
dc.description.bitstreamurlhttps://deepblue.lib.umich.edu/bitstream/2027.42/151316/2/jgra55090_am.pdf
dc.identifier.doi10.1029/2019JA026787
dc.identifier.sourceJournal of Geophysical Research: Space Physics
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dc.owningcollnameInterdisciplinary and Peer-Reviewed


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