Double degenerate mergers as progenitors of high-field magnetic white dwarfs
High-field magnetic white dwarfs have been long suspected to be the result of stellar mergers. However, the nature of the coalescing stars and the precise mech anism that produces the magnetic field are still unknown. Here we show that the hot, convective, diffe rentially rotating corona present in...
| Autores: | , , , , , , , , |
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| Tipo de documento: | artigo |
| Data de publicação: | 2011 |
| País: | España |
| Recursos: | Universitat Politècnica de Catalunya (UPC) |
| Repositório: | UPCommons. Portal del coneixement obert de la UPC |
| Idioma: | inglês |
| OAI Identifier: | oai:upcommons.upc.edu:2117/24427 |
| Acesso em linha: | https://hdl.handle.net/2117/24427 https://dx.doi.org/10.1088/0004-637X/749/1/25 |
| Access Level: | Acceso aberto |
| Palavra-chave: | Stars--Evolution Double stars White dwarfs stars binaries: general stars: evolution stars: interiors stars: magnetic field stars: rotation white dwarfs Estels binaris Estels nans Estels -- Formació Àrees temàtiques de la UPC::Física::Astronomia i astrofísica |
| Resumo: | High-field magnetic white dwarfs have been long suspected to be the result of stellar mergers. However, the nature of the coalescing stars and the precise mech anism that produces the magnetic field are still unknown. Here we show that the hot, convective, diffe rentially rotating corona present in the outer layers of the remnant of the merger of two degenerate cores is able to produce magnetic fields of the required strength that do not decay for long timescales. We also show, using an state-of-the-art Monte Carlo simulator, that the expected number of high-field magn etic white dwarfs produced in this way is consistent with that found in the Solar neighborhood. |
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