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Non-Spiral Interplanetary Magnetic Field and Coronal Mass Ejections

非螺旋行星际磁场和日冕物质抛射

基本信息

批准号：
14540416
负责人：
NAKAGAWA Tomoko
金额：
$ 1.02万
依托单位：
Tohoku Intsitute of Technology
依托单位国家：
日本
项目类别：
Grant-in-Aid for Scientific Research (C)
财政年份：
2002
资助国家：
日本
起止时间：
2002 至 2003
项目状态：
已结题

来源：
https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-14540416/
关键词：
CME acceleration of solar wind solar wind plasma IMF interplanetary space non-spiral field NOZOMI SOHO LASCO 「SOHO」衛星太陽風惑星空間磁場 ICME 太陽風の加速平面状磁場構造宇宙天気予報

项目摘要

The speeds of propagation of CMEs in interplanetary space are less distributed than their initial speeds measured on their departure from the limb of the Sun. Gopalswamy et al.(2000, 2001) presented a linear relationship between initial speeds of limb CMEs and their average acceleration during their travel time in interplanetary space. The linear relationship suggests that some dragging force is acting on CMEs. If similar relationship holds within 20 solar radii from the Sun, it would give information on the initial speed of 'ambient' solar wind in the vicinity of the Sun. The relationship between the initial acceleration and the initial speeds of limb CMEs was examined by using SOHO/LASCO CME Catalogue. For the cases for which correlation coefficient was fairly good (from -0.6 to -I), the 'ambient' solar wind speed within 20 solar radii was estimated to be 150 -570 km/s. It is somewhat slower than but close to the speeds of real solar wind measured in interplanetary space.Interplanetary counterparts of a halo CME which occurred on April 13, 1999, were observed by NOZOMI and ACE on April 16-18, when the two spacecraft were within 3 degrees in heliocentric longitude and 0.2 AU in heliocentric distance. The interplanetary magnetic fields had filamentary structures with large Bz components, and the Bz component was positive at NOZOMI while negative at ACE. Both magnetic fields were different from a magnetic cloud. It implies that the CME had a number of filamentary structures of magetic field lines with various directions. An interplanetary magnetic field of this kind can be used for detection of candidates of interplanetary counterparts of CMEs.

日冕物质抛射在行星际空间中的传播速度比它们离开太阳边缘时测量的初始速度分布更小。Gopalswamy等人(2000 2001年）提出了一个线性关系的肢体CME的初始速度和他们的平均加速度在其旅行时间在行星际空间。这种线性关系表明，一些拖曳力作用于日冕物质抛射。如果类似的关系在距离太阳20个太阳半径内成立，它将提供太阳附近“环境”太阳风初始速度的信息。利用SOHO/LASCO CME星表研究了临边CME的初速度与初加速度的关系。对于相关系数相当好的情况（从-0.6到-I），在20个太阳半径内的“环境”太阳风速度估计为150 - 570 km/s。1999年4月13日发生的日冕日冕物质抛射的行星际对应物，由NOZOMI和ACE在4月16-18日观测到，当时两个航天器的日心经度在3度以内，日心距离在0.2 Au单位以内。行星际磁场具有Bz分量较大的周期性结构，NOZOMI的Bz分量为正，ACE的Bz分量为负。两者的磁场，都不同于磁云。这意味着CME具有多个不同方向的磁力线的连续结构。这种行星际磁场可以用来探测CME的行星际对应物的候选者。