An asynchronous and parallel time-marching method for three-dimensional (3D) time-dependent magnetohydrodynamic (MHD) simulation is used for large-scale solar wind simulation. It uses different local time steps in the corona and the heliosphere according to the local Courant-Friedrichs-Levy (CFL) conditions. The solar wind background with observed solar photospheric magnetic field as input is first presented. The simulation time for the background solar wind by using the asynchronous method is <1/6 of that by using the normal synchronous time-marching method with the same computation precision. Then, we choose the coronal mass ejection (CME) event of 13 November, 2003 as a test case. The time-dependent variations of the pressure and the velocity configured from a CME model at the inner boundary are applied to generate transient structures in order to study the dynamical interaction of a CME with the background solar wind flow between 1 and 230 Rs. This time-marching method is very effective in terms of computation time for large-scale 3D time-dependent numerical MHD problem. In this validation study, we find that this 3D MHD model, with the asynchronous and parallel time-marching method, provides a relatively satisfactory comparison with the ACE spacecraft obser- vations at L1 point.
We conduct simulations using the three-dimensional(3D)solar-interplanetary conservation element/solution element(SIP-CESE)maguetohydrodynamic(MHD)model and magnetogram data from a Carrington rotation(CR)1897 to compare the three commonly used heating methods,I.e.The Wentzel-Kramers-Brillouin(WKB)Alfvén wave heating method,the turbulence heating method and the volumetric heating method.Our results show that all three heating models can basically reproduce the bimodal structure of the solar wind observed near the solar minimum.The results also demonstrate that the major acceleration interval terminates about 4Rs for the turbulence heating method and 1ORs for both the WKB Alfvén wave heating method and the volumetric heating method.The turbulence heating and the volumetric heating methods can capture the observed changing trends by the WIND satellite,while the WKB Alfvén wave heating method does not.
