Abstract
An astrophysical dynamo converts the kinetic energy of fluids into magnetic energy. Dynamo is a non-local process. Here, we consider whether a dynamo can operate at the magnetopauses of magnetic rapidly rotating planets. We analyze the main necessary condition for the work of this type of dynamo—the rotation transfer from the planet to the magnetopause. We show the role of the current disc around a rapidly rotating magnetic planet in the redistribution of angular momentum depending on the direction of the external magnetic field, using the example of the Jupiter’s magnetodisc.
Highlights
Two non-local processes are very important for space plasma physics: reconnection and dynamo
The magnetic reconnection of the interplanetary and magnetospheric magnetic fields plays a significant role in the magnetospheric magnetic field structure and, for the angular momentum transfer along highly conducting open magnetic field lines
The possibility of the magnetic field amplification outside the magnetopause of a rapidly rotating magnetic planet by the dynamo mechanism powered by the energy of braking rotation in the dynamo region is discussed
Summary
Two non-local processes are very important for space plasma physics: reconnection and dynamo. The dynamo, e.g., [2] vice versa, converts the kinetic energy of electrically conducting fluids into magnetic energy This process takes place in a small diffusion region, but the generated amplified magnetic field exists on a large spatial scale. The magnetorotational instability was described, for example, by Balbus and Hawley [3] They showed how MHD turbulence arises in the accretion discs in the presence of a weak magnetic field and outwardly decreasing differential rotation. The authors obtained a turbulent MRI-driven dynamo with a magnetic field in the proto-neutron stars > 2 × 1015 G, which confirms the idea that magnetorotational instability can generate a strong magnetic field of magnetar This mechanism can work at the magnetopause of a rapidly rotating magnetic planet. We consider how plasma flows can amplify and modify a weak background poloidal magnetic field just outside the magnetopauses of magnetized fast-rotating planets using Jupiter as an example
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