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Statistical storm time examination of MLT‐dependent plasmapause location derived from IMAGE EUV
dc.contributor.authorKatus, R. M.en_US
dc.contributor.authorGallagher, D. L.en_US
dc.contributor.authorLiemohn, M. W.en_US
dc.contributor.authorKeesee, A. M.en_US
dc.contributor.authorSarno‐smith, L. K.en_US
dc.date.accessioned2015-09-01T19:30:24Z
dc.date.available2016-08-08T16:18:39Zen
dc.date.issued2015-07en_US
dc.identifier.citationKatus, R. M.; Gallagher, D. L.; Liemohn, M. W.; Keesee, A. M.; Sarno‐smith, L. K. (2015). "Statistical storm time examination of MLTâ dependent plasmapause location derived from IMAGE EUV." Journal of Geophysical Research: Space Physics 120(7): 5545-5559.en_US
dc.identifier.issn2169-9380en_US
dc.identifier.issn2169-9402en_US
dc.identifier.urihttps://hdl.handle.net/2027.42/113122
dc.description.abstractThe location of the outer edge of the plasmasphere (the plasmapause) as a function of geomagnetic storm time is identified and investigated statistically in regard to the solar wind driver. Imager for Magnetopause‐to‐Aurora Global Exploration (IMAGE) extreme ultraviolet (EUV) data are used to create an automated method that locates and extracts the plasmapause. The plasmapause extraction technique searches a set range of possible plasmasphere densities for a maximum gradient. The magnetic local time (MLT)‐dependent plasmapause results are compared to manual extraction results. The plasmapause results from 39 intense storms are examined along a normalized epoch storm timeline to determine the average plasmapause L shell as a function of MLT and storm time. The average extracted plasmapause L shell follows the expected storm time plasmapause behavior. The results show that during the main phase, the plasmapause moves earthward and a plasmaspheric drainage plume forms near dusk and across the dayside during strong convection. During the recovery phase, the plume rejoins the corotationally driven plasma while the average plasmapause location moves farther from the Earth. The results are also examined in terms of the solar wind driver. We find evidence that shows that the different categories of solar wind drivers result in different plasmaspheric configurations. During magnetic cloud‐driven events the plasmaspheric drainage plume appears at the start of the main phase. During sheath‐driven events the plume forms later but typically extends further in MLT.Key PointsDeveloped an automated procedure to extract plasmapause from IMAGE EUV imagesValidate and evaluate results using statistical analysis of 39 intense stormsShow that plasmasphere dynamics vary systematically with CME‐v‐CIR drivingen_US
dc.publisherAGUen_US
dc.publisherWiley Periodicals, Inc.en_US
dc.subject.otherplasmapauseen_US
dc.subject.othergeomagnetic stormsen_US
dc.subject.otherIMAGE EUV dataen_US
dc.subject.othernormalized superposed epoch analysisen_US
dc.titleStatistical storm time examination of MLT‐dependent plasmapause location derived from IMAGE EUVen_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/2027.42/113122/1/jgra51890.pdf
dc.identifier.doi10.1002/2015JA021225en_US
dc.identifier.sourceJournal of Geophysical Research: Space Physicsen_US
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dc.owningcollnameInterdisciplinary and Peer-Reviewed


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