Возникновение и движение быстрых корональных выбросов массы типа “гало”, не связанных с эруптивными волокнами

  • Yu.S. Zagainova ИЗМИРАН им. Н.В. Пушкова, г. Москва, Троицк, Россия
  • V.G. Fainshtein ИСЗФ СО РАН, г. Иркутск, Россия


We used GOES/SXI, SOHO/EIT, TRACE, MarkIV-coronameter and SOHO/LASCO data to study the formation and movement of 6 fast halo coronal mass ejections (HCMEs), unrelated to eruptive filaments. We have drawn a conclusion about the existence of two CME types having different time profiles of the coronal mass ejection velocity. Types of time profiles are determined by features of the active region (AR), in which CME occurs. HCMEs occurring in one and the same AR at different time (homologous CMEs) have the same time profiles. Several hours before being recorded by the GOES/SXI, all CMEs under study are observed in the SOHO/EIT field-of-view, in λ 195 Å, as emission loops (in one case – as a complex of loops). We have drawn a conclusion that CME occurs due to the imbalance in these emission loops. We have established the dependence of amplitude on duration of the HCME main acceleration.


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How to Cite
Zagainova Y., Fainshtein V., 2013. Izvestiya Krymskoi Astrofizicheskoi Observatorii, vol. 109, no. 3, pp. 50-59. Available at: https://jn.craocrimea.ru/index.php/izvcrao/article/view/401 (Accessed: 2December2020)
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