Geoeffectiveness of the coronal mass ejections associated with solar proton events

作     者：Gui-Ming Le Chuan Li Yu-Hua Tang Liu-Guan Ding Zhi-Qiang Yin Yu-Lin Chen Yang-Ping Lu Min-Hao Chen Zhong-Yi Li 

作者机构：Key Laboratory of Space Weather National Center for Space Weather China Meteorological Administration Beijing 100081 China School of Astronomy and Space Science Nanjing University Xianlin Campus Nanjing 210046 China National Astronomical Observatories Chinese Academy of-Sciences Beijing 100012 China School of Mathematics and Statistics Nanjing University of Information Science and Technology Nanjing 210044China 

出 版 物：《Research in Astronomy and Astrophysics》 (天文和天体物理学研究（英文版）)

年 卷 期：2016年第16卷第1期

页      面：117-128页

核心收录：

学科分类：07[理学] 070401[理学-天体物理] 0704[理学-天文学] 

基　　金：supported by the National Basic Research Program of China (973 Program,Grant No.2012CB957801) the National Natural Science Foundation of China (Grant Nos.41074132,41274193,41674166,41031064 and 11303017) the National Standard Research Program (Grant No.200710123) the project 985 of Nanjing University,the Advanced Discipline Construction Project of Jiangsu Province and the NKBRSF (Grant No.2014CB744203) 

主　　题：Sun: coronal mass ejections (CMEs)    Sun: particle emission    Sun: solar terrestrial rela  tions 

摘      要：The intensity-time profiles of solar proton events（SPEs） are grouped into three types in the present study. The Type-I means that the intensity-time profile of an SPE has one peak, which occurs shortly after the associated solar flare and coronal mass ejection（CME）. The Type-II means that the SPE profile has two peaks： the first peak occurs shortly after the solar eruption, the second peak occurs at the time when the CME-driven shock reaches the Earth, and the intensity of the second peak is lower than the first *** the intensity of the second peak is higher than the first one, or the SPE intensity increases continuously until the CME-driven shock reaches the Earth, this kind of intensity-time profile is defined as Type-III. It is found that most CMEs associated with Type-I SPEs have no geoeffectiveness and only a small part of CMEs associated with Type-I SPEs can produce minor（–50 n T ≤ Dst ≤–30 n T） or moderate geomagnetic storms（–100 n T≤ Dst ≤–50 n T）, but never an intense geomagnetic storm（–200 n T ≤ Dst 〈-100 n T）. However,most of the CMEs associated with Type-II and Type-III SPEs can produce intense or great geomagnetic storms（Dst ≤-200 n T）. The solar wind structures responsible for the geomagnetic storms associated with SPEs with different intensity-time profiles have also been investigated and discussed.