摘要
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.
作者
杨利平
冯学尚
向长青
江朝伟
YANG Li-Ping;FENG Xue-Shang;XIANG Chang-Qing;JIANG Chao-Wei(SIGMA Weather Group,State Key Laboratory for Space Weather,Center for Space Science and Applied Research,Chinese Academy of Sciences,Beijing 100190;College of Earth Sciences,Graduate University of Chinese Academy of Sciences,Beijing 100049)
基金
Supported by the National Natural Science Foundation of China(41031066,40921063,40874091,40890162,40904050,40874077,and 41074122)
the Specialized Research Fund for State Key Laboratories.