Onset of Fast Magnetic Reconnection in Partially Ionized Gases
arXiv:1105.1559 · doi:10.1088/0004-637X/739/2/72
Abstract
We consider quasi-stationary two-dimensional magnetic reconnection in a partially ionized incompressible plasma. We find that when the plasma is weakly ionized and the collisions between the ions and the neutral particles are significant, the transition to fast collisionless reconnection due to the Hall effect in the generalized Ohm's law is expected to occur at much lower values of the Lundquist number, as compared to a fully ionized plasma case. We estimate that these conditions for fast reconnection are satisfied in molecular clouds and in protostellar disks.
19 pages, 1 figure, 1 table
References in corpus (5)
- Magnetic fields in protoplanetary disks
- A catastrophe model for fast magnetic reconnection onset
- Magnetohydrodynamic waves in solar partially ionized plasmas: two-fluid approach
- Self-Regulation of Solar Coronal Heating Process via Collisionless Reconnection Condition
- Chromospheric magnetic reconnection: Two-fluid simulations of coalescing current loops
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