In this paper , results of 2.5-dimensional magnetohydrodynamical simulations are reported for the magnetic reconnection of non-perfectly antiparallel magnetic fields .
The magnetic field has a component perpendicular to the computational plane , that is , guide field .
The angle \theta between magnetic field lines in two half regions is a key parameter in our simulations whereas the initial distribution of the plasma is assumed to be simple ; density and pressure are uniform except for the current sheet region .
Alfvén waves are generated at the reconnection point and propagate along the reconnected field line .
The energy fluxes of the Alfvén waves and magneto-acoustic waves ( slow mode and fast mode ) generated by the magnetic reconnection are measured .
Each flux shows the similar time evolution independent of \theta .
The percentage of the energies ( time integral of energy fluxes ) carried by the Alfvén waves and magneto-acoustic waves to the released magnetic energy are calculated .
The Alfvén waves carry 38.9 % , 36.0 % , and 29.5 % of the released magnetic energy at the maximum ( \theta = 80 ^ { \circ } ) in the case of \beta = 0.1 , 1 , and 20 respectively , where \beta is the plasma \beta ( the ratio of gas pressure to magnetic pressure ) .
The magneto-acoustic waves carry 16.2 % ( \theta = 70 ^ { \circ } ) , 25.9 % ( \theta = 60 ^ { \circ } ) , and 75.0 % ( \theta = 180 ^ { \circ } ) of the energy at the maximum .
Implications of these results for solar coronal heating and acceleration of high-speed solar wind are discussed .