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dc.contributor.authorLiu, Xu
dc.contributor.authorChen, Lunjin
dc.date.accessioned2019-11-13T16:36:57Z
dc.date.available2019-11-13T16:36:57Z
dc.date.created2019-04-15
dc.identifier.issn1070-664X
dc.identifier.urihttps://hdl.handle.net/10735.1/7104
dc.descriptionDue to copyright restrictions full text access from Treasures at UT Dallas is restricted to current UTD affiliates (use the provided Link to Article).
dc.description.abstractWe present a general relativistic linear growth rate formula of electromagnetic waves for any wave normal angle and a general distribution function in a uniform magnetized plasma with a dominant cold plasma component and a tenuous hot plasma component. Such a general linear growth rate formula can be applied to different plasma environments, such as the Jovian Magnetosphere and laboratory plasma. The relativistic resonant condition for different wave modes is discussed and summarized. Then, the formula is applied to a parametric study for local instability of Earth's plasmaspheric hiss. We study the effects of the electron temperature, electron temperature anisotropy, types of distribution functions, plasma density, background magnetic field, and wave normal angle on the relativistic linear growth rate of the whistler mode. We find that (1) the energetic electrons with larger energy resonate with the lower frequency wave. The relativistic effect becomes significant for the electron with energy >100 keV. (2) The anisotropy only increases the growth rate and expands the growth wave band. (3) The high density and low background magnetic field tend to decrease the wave frequency and increase the growth rate. (4) The field-aligned growth rate is larger than the oblique growth rate, and the lower frequency whistler waves are easier to propagate obliquely. © 2019 Author(s).
dc.description.sponsorshipThis work was supported by NASA Grant Nos. NNX15AF55G and NNX17A152G and AFOSR Grant No. FA9550-16-1-0344.
dc.language.isoen
dc.publisherAmerican Institute of Physics Inc.
dc.relation.urihttps://dx.doi.org/10.1063/1.5089749
dc.rights©2019 The Authors
dc.subjectAnisotropy
dc.subjectAtmospherics
dc.subjectDistribution (Probability theory)
dc.subjectElectromagnetic waves
dc.subjectElectrons
dc.subjectMagnetic fields
dc.subjectPlasma (Ionized gases)
dc.subjectMagnetosphere
dc.subjectPlasma density
dc.subjectPlasma diagnostics
dc.subjectPlasma stability
dc.subjectElectrons, Energetic
dc.subjectJupiter (Planet)—Magnetosphere
dc.subjectElectron temperature
dc.subjectPlasmas, Magnetized
dc.titleInstability in a Relativistic Magnetized Plasma
dc.type.genrearticle
dc.description.departmentSchool of Natural Sciences and Mathematics
dc.description.departmentWilliam B. Hanson Center for Space Sciences
dc.identifier.bibliographicCitationLiu, X., and L. Chen. 2019. "Instability in a relativistic magnetized plasma." Physics of Plasmas 26(4): art. 042902, doi: 10.1063/1.5089749
dc.source.journalPhysics of Plasmas
dc.identifier.volume26
dc.identifier.issue4
dc.contributor.utdAuthorLiu, Xu
dc.contributor.utdAuthorChen, Lunjin
dc.contributor.ORCID0000-0002-7211-0546 (Liu, X)
dc.contributor.ORCID0000-0003-2489-3571 (Chen, L)


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