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Decoding the Pre-Eruptive Magnetic Field Configurations of Coronal Mass Ejections View all abstracts by submitter

Spiros Patsourakos   Submitted: 2021-02-19 05:07

A clear understanding of the nature of the pre-eruptive magnetic field configurations of Coronal Mass Ejections (CMEs) is required for understanding and eventually predicting solar eruptions. Only two, but seemingly disparate, magnetic configurations are considered viable; namely, sheared magnetic arcades (SMA) and magnetic flux ropes (MFR). They can form via three physical mechanisms (flux emergence, flux cancellation, helicity condensation). Whether the CME culprit is an SMA or an MFR, however, has been strongly debated for thirty years. We formed an International Space Science Institute (ISSI) team to address and resolve this issue and report the outcome here. We review the status of the field across modeling and observations, identify the open and closed issues, compile lists of SMA and MFR observables to be tested against observations and outline research activities to close the gaps in our current understanding. We propose that the combination of multi-viewpoint multi-thermal coronal observations and multi-height vector magnetic field measurements is the optimal approach for resolving the issue conclusively. We demonstrate the approach using MHD simulations and synthetic coronal images.

Authors: Patsourakos, S., Vourlidas, A., Török, T., Kliem, B., Antiochos, S. K., Archontis, V., Aulanier, G., Cheng, X., Chintzoglou, G., Georgoulis, M. K., Green, L. M., Leake, J. E., Moore, R., Nindos, A., Syntelis, P., Yardley, S. L., Yurchyshyn, V., Zhang, J.
Projects: None

Publication Status: Space Science Reviews, 2020, Volume 216, Issue 8, article id.131
Last Modified: 2021-02-20 22:48
Go to main E-Print page  Are the brightest coronal loops always rooted in mixed-polarity magnetic flux?  Properties of stream interaction regions at Earth and Mars during the declining phase of SC 24  Edit Entry  Download Preprint  Delete Entry 

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