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The origin, early evolution and predictability of solar eruptions View all abstracts by submitter

Tibor Torok   Submitted: 2018-01-15 18:39

Coronal mass ejections (CMEs) were discovered in the early 1970s when space-borne coronagraphs revealed that eruptions of plasma are ejected from the Sun. Today, it is known that the Sun produces eruptive flares, filament eruptions, coronal mass ejections and failed eruptions; all thought to be due to a release of energy stored in the coronal magnetic field during its drastic reconfiguration. This review discusses the observations and physical mechanisms behind this eruptive activity, with a view to making an assessment of the current capability of forecasting these events for space weather risk and impact mitigation. Whilst a wealth of observations exist, and detailed models have been developed, there still exists a need to draw these approaches together. In particular more realistic models are encouraged in order to asses the full range of complexity of the solar atmosphere and the criteria for which an eruption is formed. From the observational side, a more detailed understanding of the role of photospheric flows and reconnection is needed in order to identify the evolutionary path that ultimately means a magnetic structure will erupt.

Authors: L.M. Green, T. Torok, B. Vrsnak, W. Manchester IV, A. Veronig
Projects: None

Publication Status: Accepted for publication in Space Science Reviews
Last Modified: 2018-01-16 11:11
Go to main E-Print page  Probing Twisted Magnetic Field Using Microwave Observations in an M Class Solar Flare on 11 February, 2014  Polar Field Correction for HMI Line-of-Sight Synoptic Data  Edit Entry  Download Preprint  Delete Entry 

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