The third order accurate upwind compact difference scheme has been applied to the numerical study of the magnetic reconnection process possibly occurring near the interplanetary current sheet, under the framework of t...The third order accurate upwind compact difference scheme has been applied to the numerical study of the magnetic reconnection process possibly occurring near the interplanetary current sheet, under the framework of the two-dimensional compressible magnetohydrodynamics (MHD). Our results here show that the driven reconnection near the current sheet can occur within 10-30 min for the interplanetary high magnetic Reynolds number, RM =2 000-10 000, the stable magnetic reconnection structure can be formed in hour-order of magnitude, and there are some basic properties such as the multiple X-line reconnections, vortical velocity structures, filament current systems, splitting and collapse of the high-density plasma bulk. These results are helpful in understanding and identifying the magnetic reconnection phenomena near the interplanetary current sheets.展开更多
The conventional nonreflecting projective charac teristic boundary condition for MHD equations is improved in order to remove spurious oscillations caused by the presence of zero point of the components of magnetic fi...The conventional nonreflecting projective charac teristic boundary condition for MHD equations is improved in order to remove spurious oscillations caused by the presence of zero point of the components of magnetic field. The improved boundary condition is easier to be implemented in programming, and its application to the simulation of asymmetric corona can give us stable coronal static structures.展开更多
基金the National Natural Foundation of China (Grant Nos. 49674243 and 49874040).
文摘The third order accurate upwind compact difference scheme has been applied to the numerical study of the magnetic reconnection process possibly occurring near the interplanetary current sheet, under the framework of the two-dimensional compressible magnetohydrodynamics (MHD). Our results here show that the driven reconnection near the current sheet can occur within 10-30 min for the interplanetary high magnetic Reynolds number, RM =2 000-10 000, the stable magnetic reconnection structure can be formed in hour-order of magnitude, and there are some basic properties such as the multiple X-line reconnections, vortical velocity structures, filament current systems, splitting and collapse of the high-density plasma bulk. These results are helpful in understanding and identifying the magnetic reconnection phenomena near the interplanetary current sheets.
基金This work was supported by the National Natural Science Foundation of China (Grant Nos. 49990450 and 499925412).
文摘The conventional nonreflecting projective charac teristic boundary condition for MHD equations is improved in order to remove spurious oscillations caused by the presence of zero point of the components of magnetic field. The improved boundary condition is easier to be implemented in programming, and its application to the simulation of asymmetric corona can give us stable coronal static structures.
