ISWI Webinars

The ISWI Webinar committee organizes and  hosts virtual seminars on topics of interest to the community. The webinars are recorded and the playlist with the previous seminars, which will also include future sessions, can be accessed through the following links:

UN page with links: 

The next ISWI Seminar will be October 25, 2023

We are pleased to announce the next ISWI Seminar of 2023 will be by Dr. Hebe Cremades scheduled for October 25th at 3 PM Central European Time (9 AM EDT; 6:30 PM IST).

To register for the virtual seminar, please send an email to: Please include “ISWI Seminar Registration” in the subject line. There is a limit of 300 participants, so please register your interest as soon as possible. The MS Teams link will be sent to registered participants 2 days before the event.

Title: Considerations on the morphology of coronal mass ejections

Speaker: Dr Hebe Cremades
Mendoza Group for Heliophysics Studies (GEHMe, University of Mendoza) and CONICET

Coronal mass ejections (CMEs) are undoubtedly the most spectacular transient events that can be observed in the solar corona. Enabled by the fleet of solar- and heliospheric-dedicated spacecraft with the capability of detecting them remotely and/or in situ, CMEs and their interplanetary counterparts have been characterized with increasing detail throughout the years. Nevertheless, several aspects of CMEs remain elusive, including their three-dimensional magnetic configuration, mainly due to limitations inherent to remote-sensing and in situ observations. Still, they provide valuable pieces of information that have high potential to shed light in this respect. The study of CME morphology on the basis of remote-sensing observations is an approach to that end, since it holds a close relationship with the CME magnetic field configuration. Findings on CME morphology are key for the interpretation and modeling of in situ observations of these events at multiple spacecraft. In particular, the extent of CMEs, expansion rates along orthogonal directions, departures from the archetypical flux rope structure, and factors affecting the characterization of CME morphology will be addressed.