Vorticity and magnetic dynamo from subsonic expansion waves II. Dependence on the magnetic Prandtl number, forcing scale, and cooling time
[Context] The amplification of astrophysical magnetic fields takes place via dynamo instability in turbulent environments. Vorticity is usually present in any dynamo, but its role is not yet fully understood.
| Autores: | , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2024 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/371858 |
| Acceso en línea: | http://hdl.handle.net/10261/371858 |
| Access Level: | acceso abierto |
| Palabra clave: | ISM: magnetic fields Galaxies: evolution Intergalactic medium Galaxies: magnetic field |
| Sumario: | [Context] The amplification of astrophysical magnetic fields takes place via dynamo instability in turbulent environments. Vorticity is usually present in any dynamo, but its role is not yet fully understood. |
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