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Interpreting ~1 Hz magnetic compressional waves in Mercury's inner magnetosphere in terms of propagating ion‐Bernstein waves

dc.contributor.authorBoardsen, S. A.en_US
dc.contributor.authorKim, E.‐h.en_US
dc.contributor.authorRaines, J. M.en_US
dc.contributor.authorSlavin, J. A.en_US
dc.contributor.authorGershman, D. J.en_US
dc.contributor.authorAnderson, B. J.en_US
dc.contributor.authorKorth, H.en_US
dc.contributor.authorSundberg, T.en_US
dc.contributor.authorSchriver, D.en_US
dc.contributor.authorTravnicek, P.en_US
dc.date.accessioned2015-08-05T16:46:40Z
dc.date.available2016-07-05T17:27:57Zen
dc.date.issued2015-06en_US
dc.identifier.citationBoardsen, S. A.; Kim, E.‐h. ; Raines, J. M.; Slavin, J. A.; Gershman, D. J.; Anderson, B. J.; Korth, H.; Sundberg, T.; Schriver, D.; Travnicek, P. (2015). "Interpreting ~1â Hz magnetic compressional waves in Mercury's inner magnetosphere in terms of propagating ionâ Bernstein waves." Journal of Geophysical Research: Space Physics 120(6): 4213-4228.en_US
dc.identifier.issn2169-9380en_US
dc.identifier.issn2169-9402en_US
dc.identifier.urihttps://hdl.handle.net/2027.42/112180
dc.description.abstractWe show that ~1 Hz magnetic compressional waves observed in Mercury's inner magnetosphere could be interpreted as ion‐Bernstein waves in a moderate proton beta ~0.1 plasma. An observation of a proton distribution with a large planetary loss cone is presented, and we show that this type of distribution is highly unstable to the generation of ion‐Bernstein waves with low magnetic compression. Ray tracing shows that as these waves propagate back and forth about the magnetic equator; they cycle between a state of low and high magnetic compression. The group velocity decreases during the high‐compression state leading to a pileup of compressional wave energy, which could explain the observed dominance of the highly compressional waves. This bimodal nature is due to the complexity of the index of refraction surface in a warm plasma whose upper branch has high growth rate with low compression, and its lower branch has low growth/damping rate with strong compression. Two different cycles are found: one where the compression maximum occurs at the magnetic equator and one where the compression maximum straddles the magnetic equator. The later cycle could explain observations where the maximum in compression straddles the equator. Ray tracing shows that this mode is confined within ±12° magnetic latitude which can account for the bulk of the observations. We show that the Doppler shift can account for the difference between the observed and model wave frequency, if the wave vector direction is in opposition to the plasma flow direction. We note that the Wentzel‐Kramers‐Brillouin approximation breaks down during the pileup of compressional energy and that a study involving full wave solutions is required.Key PointsThe ion‐Bernstein (IB) mode is highly unstable to proton loss cones at MercuryThe IB mode can become highly compressional as it propagatesRay tracing of the IB mode predicts compression peaking the off equatoren_US
dc.publisherWiley Periodicals, Inc.en_US
dc.publisherCambridge Univ. Pressen_US
dc.subject.otherplanetary loss cone instabilityen_US
dc.subject.otherray tracingen_US
dc.subject.otherion‐Bernstein modeen_US
dc.subject.otherMercury's magnetosphereen_US
dc.titleInterpreting ~1 Hz magnetic compressional waves in Mercury's inner magnetosphere in terms of propagating ion‐Bernstein wavesen_US
dc.typeArticleen_US
dc.rights.robotsIndexNoFollowen_US
dc.subject.hlbsecondlevelAstronomy and Astrophysicsen_US
dc.subject.hlbtoplevelScienceen_US
dc.description.peerreviewedPeer Revieweden_US
dc.description.bitstreamurlhttp://deepblue.lib.umich.edu/bitstream/2027.42/112180/1/jgra51808.pdf
dc.identifier.doi10.1002/2014JA020910en_US
dc.identifier.sourceJournal of Geophysical Research: Space Physicsen_US
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dc.owningcollnameInterdisciplinary and Peer-Reviewed


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