Abstract

We review our magnetic reconnection model of the solar coronal X-ray jets. The plasma of an X-ray jet is accelerated and heated by reconnection between the emerging flux and a pre-existing coronal field. Many observed characteristics of the X-ray jets could be successfully reproduced through the two-dimensional MHD numerical simulations based on this model. We also discuss the Alfven wave generated by the reconnection process. The simulation results show that the amount of Alfven wave energy is ≈3% of the total energy released by the magnetic reconnection.

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