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- W767657464 abstract "The possible influence of magnetic fields on the dynamics of core-collapse supernovae and the evolution of nascent proto-neutron stars is largely unknown. One of the most promising agents amplifying the magnetic field in a core-collapse supernova explosion is the magneto-rotational instability (MRI; see, e.g., Balbus & Hawley, 1998). The MRI has been studied intensively in accretion disks where it excites turbulence and provides the effective viscosity required for the accretion of the gas. Nevertheless, the saturation level of the instability is still not fully understood. Pessah (2010) suggested that the MRI growth is terminated by secondary parasitic instabilities (Kelvin-Helmholtz and resistive tearing-mode instabilities, Goodman & Xu, 1994) growing on top of MRI modes. Hence, the saturation level of the MRI is determined by the interplay between the MRI and the parasites. Extending our previous set of simulations (Obergaulinger et al., 2008), we study this interplay in local, three-dimensional, non-ideal MHD simulations. Our final goal is the formulation of a simple model connecting the initial magnetic field, and the resistivity and viscosity of the matter with the termination and saturation of the MRI." @default.
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- W767657464 date "2012-01-01" @default.
- W767657464 modified "2023-09-27" @default.
- W767657464 title "Magneto-rotational instability in core-collapse supernovae" @default.
- W767657464 hasPublicationYear "2012" @default.
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