科研之友
微信
新浪微博
Facebook
分享链接
摘要
In this paper, the 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, a guide field. The angle theta between the magnetic field lines in two half regions was a key parameter in our simulations, whereas the initial distribution of the plasma was assumed to be simple; the density and pressure were uniform, except for the current sheet region. Alfven waves were generated at the reconnection point and propagated along the reconnected field line. The energy fluxes of the Alfven waves and the magneto-acoustic waves (slow mode and fast mode) generated by magnetic reconnection were measured. Each flux shows a similar time evolution independent of theta. The percentages of the energies (time integral of energy fluxes) carried by the Alfven waves and magneto-acoustic waves to the released magnetic energy were calculated. The Alfven waves carry 38.9%, 36.0%, and 29.5% of the released magnetic energy at the maximum (theta = 80 degrees) in the cases 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 degrees), 25.9% (theta = 60 degrees), and 75.0% (theta = 180 degrees) of the energy at the maximum. Implications of these results for solar coronal heating and acceleration of high-speed solar wind are discussed.
- 出版日期2010
