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Flux ropes in the Hermean magnetotail: Distribution, properties, and formation
dc.contributor.authorSmith, A. W.
dc.contributor.authorSlavin, J. A.
dc.contributor.authorJackman, C. M.
dc.contributor.authorPoh, G.‐k.
dc.contributor.authorFear, R. C.
dc.date.accessioned2017-10-23T17:30:46Z
dc.date.available2018-10-02T19:49:01Zen
dc.date.issued2017-08
dc.identifier.citationSmith, A. W.; Slavin, J. A.; Jackman, C. M.; Poh, G.‐k. ; Fear, R. C. (2017). "Flux ropes in the Hermean magnetotail: Distribution, properties, and formation." Journal of Geophysical Research: Space Physics 122(8): 8136-8153.
dc.identifier.issn2169-9380
dc.identifier.issn2169-9402
dc.identifier.urihttps://hdl.handle.net/2027.42/138858
dc.description.abstractAn automated method was applied to identify magnetotail flux rope encounters in MESSENGER (MErcury Surface, Space ENvironment, GEochemistry, and Ranging) magnetometer data. The method identified significant deflections of the northâ south component of the magnetic field coincident with enhancements in the total field or dawnâ dusk component. Two hundred fortyâ eight flux ropes are identified that possess wellâ defined minimum variance analysis (MVA) coordinate systems, with clear rotations of the field. Approximately 30% can be well approximated by the cylindrically symmetric, linearly forceâ free model. Flux ropes are most common moving planetward, in the postmidnight sector. Observations are intermittent, with the majority (61%) of plasma sheet passages yielding no flux ropes; however, the peak rate of flux ropes during a reconnection episode is â ¼5 minâ 1. Overall, the peak postmidnight rate is â ¼0.25 minâ 1. Only 25% of flux ropes are observed in isolation. The radius of flux ropes is comparable to the ion inertial length within Mercury’s magnetotail plasma sheet. No clear statistical separation is observed between tailward and planetward moving flux ropes, suggesting the nearâ Mercury neutral line (NMNL) is highly variable. Flux ropes are more likely to be observed if the preceding lobe field is enhanced over background levels. A very weak correlation is observed between the flux rope core field and the preceding lobe field orientation; a stronger relationship is found with the orientation of the field within the plasma sheet. The core field strength measured is â ¼6 times stronger than the local dawnâ dusk plasma sheet magnetic field.Key PointsTwo hundred fortyâ eight flux ropes identified in Mercury’s magnetotail (74 cylindrical and linearly forceâ free)Flux ropes most commonly observed by MESSENGER postmidnight, moving planetwardFlux ropes observed intermittently, but most often when the preceding lobe field is enhanced
dc.publisherAdvisory Group for Aerospace Res. and Dev., NATO
dc.publisherWiley Periodicals, Inc.
dc.subject.otherMercury’s magnetotail
dc.subject.otherMESSENGER
dc.subject.otherflux ropes
dc.titleFlux ropes in the Hermean magnetotail: Distribution, properties, and formation
dc.typeArticleen_US
dc.rights.robotsIndexNoFollow
dc.subject.hlbsecondlevelAstronomy and Astrophysics
dc.subject.hlbtoplevelScience
dc.description.peerreviewedPeer Reviewed
dc.description.bitstreamurlhttps://deepblue.lib.umich.edu/bitstream/2027.42/138858/1/jgra53697_am.pdf
dc.description.bitstreamurlhttps://deepblue.lib.umich.edu/bitstream/2027.42/138858/2/jgra53697.pdf
dc.identifier.doi10.1002/2017JA024295
dc.identifier.sourceJournal of Geophysical Research: Space Physics
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