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 Alfve´n wave generated by the reconnection process. The simulation results show that the amount of Alfve´n wave energy is ≈3&percent; of the total energy released by the magnetic reconnection. ©1999 American Institute of Physics.