A comparative study on 3-D solar win

A comparative study on 3-D solar wind structure observed by Ulysses and MHD simulation

During Ulysses' first rapid pole-to-pole transit from September 1994 to June 1995, its observations showed that middle- or high-speed solar winds covered all latitudes except those between -20° and +20° near the ecliptic plane,where the velocity was 300-450 km/s. At poleward 40°,however, only fast solar winds at the speed of 700-870 km/s were observed. In addition, the transitions from low-speed wind to high-speed wind or vice versa were abrupt. In this paper, the large-scale structure of solar wind observed by Ulysses near solar minimum is simulated by using the three-dimensional numerical MHD model. The model combines TVD Lax-Friedrich scheme and MacCormack Ⅱ scheme and decomposes the calculation region into two regions: one from 1 to 22 Rs and the other from 18 Rs to 1 AU.Based on the observations of the solar photospheric magnetic field and an addition of the volumetric heating to MHD equations, the large-scale solar wind structure mentioned above is reproduced by using the three-dimensional MHD model and the numerical results are roughly consistent with Ulysses' observations. Our simulation shows that the initial magnetic field topology and the addition of volume heating may govern the bimodal structure of solar wind observed by Ulysses and also demonstrates that the three-dimensional MHD numerical model used here is efficient in modeling the large-scale solar wind structure.

作 者： FENG Xueshang XIANG Changqing ZHONG Dingkun FAN Quanlin   作者單位： SIGMA Weather Group, Key Laboratory of Space Weather; Key Laboratory of Geospace Environment and Geodesy, Ministry of Education,Center for Space Science and Applied Research, Chinese Academy of Sciences, Beijing 100080, China  刊 名： 科學通報（英文版）  SCI 英文刊名： CHINESE SCIENCE BULLETIN  年，卷(期)： 2005 50(7)  分類號：   關鍵詞： Ulysses observation   solar wind structure   numerical simulation  

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