A global model of the magnetorotational instability in proto-neutron stars
Résumé
The magnetorotational instability (MRI) is a promising mechanism to amplify the magnetic field in fast-rotating proto-neutron stars. Many local studies have shown that the magnetic field could be amplified on small scales. However, the efficiency of the MRI at generating a large-scale field similar to the dipolar magnetic field of magnetars (10 14 − 10 15 G) is still unknown. We used a three dimensional pseudo-spectral code to develop an idealized global model of the MRI in a proto-neutron star. We show that a dipole field strength consistent with the values of magnetar field intensity can be generated by the MRI, even though it is lower than the small-scale magnetic field. Overall, our results support the ability of the MRI to form magnetar-like dipolar magnetic fields.
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