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Statistical Study of Foreshock Transients in the Midtail Foreshock


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dc.creatorLiu, Terry
dc.creatorZhang, Hui
dc.creatorWang, Chih-Ping
dc.creatorAngelopoulos, Vassilis
dc.creatorVu, Andrew
dc.creatorWang, Xueyi
dc.creatorLin, Yu
dc.date.accessioned2022-11-08T22:10:08Z
dc.date.available2022-11-08T22:10:08Z
dc.date.created2021
dc.identifier10.1029/2021JA029156en_US
dc.identifier.urihttps://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2021JA029156en_US
dc.identifier.urihttps://aurora.auburn.edu/handle/11200/50460
dc.identifier.urihttp://dx.doi.org/10.35099/aurora-528
dc.description.abstractIn the dayside foreshock, many foreshock transients have been observed and simulated. Because of their strong dynamic pressure perturbations, foreshock transients can disturb the local bow shock, magnetosheath, magnetopause, and thus the magnetosphere-ionosphere system. They can also accelerate particles contributing to shock acceleration. Recent observations and simulations showed that foreshock transients also exist in the midtail foreshock, which can continuously disturb the nightside bow shock, magnetosheath, and magnetopause while propagating tailward for tens of minutes. To further understand the characteristics of midtail foreshock transients, we studied them statistically using Acceleration Reconnection Turbulence & Electrodynamics of Moon's Interaction with the Sun observations. We selected 111 events that have dynamic pressure decrease along the local bow shock normal by more than 50%. We show that the dynamic pressure decrease is contributed by both density decrease and speed decrease. Around 90% of the events have electron temperature increase by more than 10% with a temperature change ratio proportional to the solar wind speed. Midtail foreshock transients more likely occur at the dawnside than the duskside. They are more significant closer to the bow shock and rather stable along the tailward direction. They have similar formation conditions compared to the dayside foreshock transients, except the ones related to the bow shock geometry. Our study indicates that the characteristics of foreshock transients based on dayside observations need to be generalized. Our study also implies that foreshock transients can exist for tens of minutes (even longer for larger planar shocks), continuously disturbing the local shock and accelerating/heating particles.en_US
dc.formatPDFen_US
dc.publisherAmerican Geophysical Unionen_US
dc.relation.ispartofJOURNAL OF GEOPHYSICAL RESEARCH-SPACE PHYSICSen_US
dc.relation.ispartofseries2169-9380en_US
dc.rights©American Geophysical Union 2021. This is this the version of record co-published by the American Geophysical Union and John Wiley & Sons, Inc. It is made available under the CC-BY-NC-ND 4.0 license. Item should be cited as: Liu, T. Z., Zhang, H., Wang, C. P., Angelopoulos, V., Vu, A., Wang, X., & Lin, Y. (2021). Statistical study of foreshock transients in the midtail foreshock. Journal of Geophysical Research: Space Physics, 126(5), e2021JA029156.en_US
dc.titleStatistical Study of Foreshock Transients in the Midtail Foreshocken_US
dc.typeTexten_US
dc.type.genreJournal Article, Academic Journalen_US
dc.citation.volume126en_US
dc.citation.issue5en_US
dc.description.statusPublisheden_US
dc.description.peerreviewYesen_US
dc.creator.orcid0000-0001-5346-7112en_US
dc.creator.orcid0000-0003-1778-4289en_US
dc.creator.orcid0000-0003-2393-6808en_US

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