Plasma Waves Around Massive Stars in (3+1)-General Relativistic Magnetohydrodynamics

dc.contributorUniversity of Kashan
dc.contributorUniversidade Estadual Paulista (UNESP)
dc.date.accessioned2022-04-29T08:40:44Z
dc.date.accessioned2022-12-20T03:05:12Z
dc.date.available2022-04-29T08:40:44Z
dc.date.available2022-12-20T03:05:12Z
dc.date.created2022-04-29T08:40:44Z
dc.date.issued2022-06-01
dc.identifierBrazilian Journal of Physics, v. 52, n. 3, 2022.
dc.identifier1678-4448
dc.identifier0103-9733
dc.identifierhttp://hdl.handle.net/11449/230552
dc.identifier10.1007/s13538-022-01051-5
dc.identifier2-s2.0-85126086173
dc.identifier.urihttps://repositorioslatinoamericanos.uchile.cl/handle/2250/5410686
dc.description.abstractIn this article, the propagation of plasma waves around rotating and non-rotating stars is studied in a TPM (Thorne-Price-Macdonald) (3+1)-general relativistic magnetohydrodynamics (GRMHD) formalism. For more simplicity, the plasma around the atmosphere of the stars is considered to be stationary. Using WKB approximation, we derive the local longitudinal and transverse dispersion relations and compare them to the special relativistic congener.
dc.languageeng
dc.relationBrazilian Journal of Physics
dc.sourceScopus
dc.subjectOne-fluid plasma equations
dc.subjectPlasma waves dispersion equations
dc.subjectPlasma waves propagation equations
dc.subjectTPM (Thorne-Price-Macdonald) (3+1)-general relativistic magnetohydrodynamics
dc.subjectWKB approximation
dc.titlePlasma Waves Around Massive Stars in (3+1)-General Relativistic Magnetohydrodynamics
dc.typeArtículos de revistas


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