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Kinematic Evolution of a Slow CME in Corona Viewed by STEREO-B on 8 October 2007
Shen, Chenglong; Wang, Yuming; Gui, Bin; Ye, Pinzhong; Wang, S.; Shen, CL (reprint author), Univ Sci & Technol China, Sch Earth & Space Sci, CAS Key Lab Basic Plasma Phys, Hefei 230026, Anhui, Peoples R China.
Department空间科学部
Source PublicationSOLAR PHYSICS
2011
Volume269Issue:2Pages:389-400
ISSN0038-0938
Language英语
KeywordCoronal Mass Ejections Kinematic Evolution Heliospheric Magnetic Field
AbstractWe studied the kinematic evolution of the 8 October 2007 CME in the corona based on observations from Sun - Earth Connection Coronal and Heliospheric Investigation (SECCHI) onboard satellite B of Solar TErrestrial RElations Observatory (STEREO). The observational results show that this CME obviously deflected to a lower latitude region of about 30 degrees at the beginning. After this, the CME propagated radially. We also analyze the influence of the background magnetic field on the deflection of this CME. We find that the deflection of this CME at an early stage may be caused by a nonuniform distribution of the background magnetic-field energy density and that the CME tended to propagate to the region with lower magnetic-energy density. In addition, we found that the velocity profile of this gradual CME shows multiphased evolution during its propagation in the COR1-B FOV. The CME velocity first remained constant: 23.1 kms(-1). Then it accelerated continuously with a positive acceleration of approximate to 7.6 ms(-2).; We studied the kinematic evolution of the 8 October 2007 CME in the corona based on observations from Sun - Earth Connection Coronal and Heliospheric Investigation (SECCHI) onboard satellite B of Solar TErrestrial RElations Observatory (STEREO). The observational results show that this CME obviously deflected to a lower latitude region of about 30 degrees at the beginning. After this, the CME propagated radially. We also analyze the influence of the background magnetic field on the deflection of this CME. We find that the deflection of this CME at an early stage may be caused by a nonuniform distribution of the background magnetic-field energy density and that the CME tended to propagate to the region with lower magnetic-energy density. In addition, we found that the velocity profile of this gradual CME shows multiphased evolution during its propagation in the COR1-B FOV. The CME velocity first remained constant: 23.1 kms(-1). Then it accelerated continuously with a positive acceleration of approximate to 7.6 ms(-2).
Indexed BySCI
Funding Project中国科学院空间科学与应用研究中心
Document Type期刊论文
Identifierhttp://ir.nssc.ac.cn/handle/122/3174
Collection空间科学部
Corresponding AuthorShen, CL (reprint author), Univ Sci & Technol China, Sch Earth & Space Sci, CAS Key Lab Basic Plasma Phys, Hefei 230026, Anhui, Peoples R China.
Recommended Citation
GB/T 7714
Shen, Chenglong,Wang, Yuming,Gui, Bin,et al. Kinematic Evolution of a Slow CME in Corona Viewed by STEREO-B on 8 October 2007[J]. SOLAR PHYSICS,2011,269(2):389-400.
APA Shen, Chenglong,Wang, Yuming,Gui, Bin,Ye, Pinzhong,Wang, S.,&Shen, CL .(2011).Kinematic Evolution of a Slow CME in Corona Viewed by STEREO-B on 8 October 2007.SOLAR PHYSICS,269(2),389-400.
MLA Shen, Chenglong,et al."Kinematic Evolution of a Slow CME in Corona Viewed by STEREO-B on 8 October 2007".SOLAR PHYSICS 269.2(2011):389-400.
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