Plasma Waves Around Massive Stars in (3+1)-General Relativistic Magnetohydrodynamics
In 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. U...
| Autores: | , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2022 |
| País: | Brasil |
| Institución: | Universidade Estadual Paulista (UNESP) |
| Repositorio: | Repositório Institucional da UNESP |
| Idioma: | inglés |
| OAI Identifier: | oai:repositorio.unesp.br:11449/230552 |
| Acceso en línea: | http://dx.doi.org/10.1007/s13538-022-01051-5 http://hdl.handle.net/11449/230552 |
| Access Level: | acceso abierto |
| Palabra clave: | One-fluid plasma equations Plasma waves dispersion equations Plasma waves propagation equations TPM (Thorne-Price-Macdonald) (3+1)-general relativistic magnetohydrodynamics WKB approximation |
| Sumario: | In 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. |
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