3D magnetohydrodynamic simulations of runaway pulsars in core-collapse supernova remnants
[Context] Pulsars represent one of the possible final stages in the evolution of massive stars. If a supernova explosion is anisotropic, it can give the pulsar a powerful "kick", propelling it to supersonic speeds. The resulting pulsar wind nebula is significantly reshaped by its interacti...
| Autores: | , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2025 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/387945 |
| Acceso en línea: | http://hdl.handle.net/10261/387945 https://api.elsevier.com/content/abstract/scopus_id/105002274879 |
| Access Level: | acceso abierto |
| Palabra clave: | ISM: bubbles ISM: magnetic fields ISM: supernova remnants |
| Sumario: | [Context] Pulsars represent one of the possible final stages in the evolution of massive stars. If a supernova explosion is anisotropic, it can give the pulsar a powerful "kick", propelling it to supersonic speeds. The resulting pulsar wind nebula is significantly reshaped by its interaction with the surrounding medium as the pulsar moves through it. First, the pulsar crosses the supernova remnant (SNR), followed by the different layers of circumstellar medium (CSM) formed during different stages of the progenitor star's evolution. |
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