Impact of magnetic field gradients on the development of the MRI: Applications to binary neutron star mergers and proto-planetary disks
[Context] The magneto-rotational instability (MRI) plays a crucial role in accretion disk modelling, driving magnetohydrodynamic turbulence and facilitating enhanced angular momentum transport. Notably, MRI is believed to be pivotal in the development of large-scale poloidal magnetic fields during b...
| Autores: | , , , |
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| Tipo de recurso: | artículo |
| Estado: | Versión publicada |
| Fecha de publicación: | 2026 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/425139 |
| Acceso en línea: | http://hdl.handle.net/10261/425139 http://arxiv.org/abs/2505.01208v2 |
| Access Level: | acceso abierto |
| Palabra clave: | Accretion Accretion disks Magnetohydrodynamics (MHD) Stars: magnetic field Stars: neutron Turbulence |
| Sumario: | [Context] The magneto-rotational instability (MRI) plays a crucial role in accretion disk modelling, driving magnetohydrodynamic turbulence and facilitating enhanced angular momentum transport. Notably, MRI is believed to be pivotal in the development of large-scale poloidal magnetic fields during binary neutron star mergers. However, the few numerical simulations that start from weak seed magnetic fields and capture its growth until saturation show the effects of small-scale turbulence and winding but lack convincing evidence of MRI activity. |
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