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dc.contributor.authorLotekar, A.
dc.contributor.authorVasko, I. Y.
dc.contributor.authorMozer, F. S.
dc.contributor.authorHutchinson, Ian
dc.contributor.authorArtemyev, A. V.
dc.contributor.authorBale, S. D.
dc.contributor.authorBonnell, J. W.
dc.contributor.authorErgun, R.
dc.contributor.authorGiles, B.
dc.contributor.authorKhotyaintsev, Yu. V.
dc.contributor.authorLindqvist, P.‐A.
dc.contributor.authorRussell, C. T.
dc.contributor.authorStrangeway, R.
dc.date.accessioned2021-10-27T15:19:26Z
dc.date.available2021-10-27T15:19:26Z
dc.date.issued2020-09
dc.date.submitted2020-07
dc.identifier.issn2169-9380
dc.identifier.issn2169-9402
dc.identifier.urihttps://hdl.handle.net/1721.1/133143
dc.description.abstractWe present a statistical analysis of more than 2,400 electrostatic solitary waves interpreted as electron holes (EH) measured aboard at least three Magnetospheric Multiscale (MMS) spacecraft in the Earth's magnetotail. The velocities of EHs are estimated using the multispacecraft interferometry. The EH velocities in the plasma rest frame are in the range from just a few km/s, which is much smaller than ion thermal velocity VTi, up to 20,000 km/s, which is comparable to electron thermal velocity VTe. We argue that fast EHs with velocities larger than about 0.1VTe are produced by bump-on-tail instabilities, while slow EHs with velocities below about 0.05VTe can be produced by warm bistream and, probably, Buneman-type instabilities. We show that typically fast and slow EHs do not coexist, indicating that the instabilities producing EHs of different types operate independently. We have identified a gap in the distribution of EH velocities between VTi and 2VTi, which is considered to be the evidence for self-acceleration (Zhou & Hutchinson, 2018) or ion Landau damping of EHs. Parallel spatial scales and amplitudes of EHs are typically between λD and 10 λD and between 10−3 Te and 0.1 Te, respectively. We show that electrostatic potential amplitudes of EHs are below the threshold of the transverse instability and highly likely restricted by the nonlinear saturation criterion of electron streaming instabilities seeding electron hole formation: (Formula presented.), where ϖ = min(γ, 1.5 ωce), where γ is the increment of instabilities seeding EH formation, while ωce is electron cyclotron frequency. The implications of the presented results are discussed.en_US
dc.description.sponsorshipNASA (Grants 80NSSC18K0155, 80NSSC19K1063)en_US
dc.language.isoen
dc.publisherAmerican Geophysical Union (AGU)en_US
dc.relation.isversionofhttp://dx.doi.org/10.1029/2020ja028066en_US
dc.rightsCreative Commons Attribution-Noncommercial-Share Alikeen_US
dc.rights.urihttp://creativecommons.org/licenses/by-nc-sa/4.0/en_US
dc.sourceProf. Hutchinsonen_US
dc.titleMultisatellite MMS Analysis of Electron Holes in the Earth's Magnetotail: Origin, Properties, Velocity Gap, and Transverse Instabilityen_US
dc.typeArticleen_US
dc.identifier.citationLotekar, A. et al. "Multisatellite MMS analysis of electron holes in the Earth's magnetotail: Origin, properties, velocity gap, and transverse instability." Journal of Geophysical Research: Space Physics, 125, 9 (September 2020): e2020JA028066. © 2020 American Geophysical Unionen_US
dc.contributor.departmentMassachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciencesen_US
dc.relation.journalJournal of Geophysical Research: Space Physicsen_US
dc.eprint.versionAuthor's final manuscripten_US
dc.type.urihttp://purl.org/eprint/type/JournalArticleen_US
eprint.statushttp://purl.org/eprint/status/PeerRevieweden_US
dc.date.updated2021-10-26T18:07:45Z
dspace.orderedauthorsLotekar, A; Vasko, IY; Mozer, FS; Hutchinson, I; Artemyev, AV; Bale, SD; Bonnell, JW; Ergun, R; Giles, B; Khotyaintsev, YV; Lindqvist, P-A; Russell, CT; Strangeway, Ren_US
dspace.date.submission2021-10-26T18:07:50Z
mit.journal.volume125en_US
mit.journal.issue9en_US
mit.licenseOPEN_ACCESS_POLICY
mit.metadata.statusCompleteen_US


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