hybrid COSPAR43 session on solar & stellar flux ropes

Submitted by mchane-y on Tue, 22/09/2020 - 14:46

Annonce transmise par B Schmieder (KU Leuven & LESIA) concernant une session solaire/stellaire pour le prochain meeting du COSPAR.

 

COSPAR 43 GA from January 28 to February 4, 2021

( hybrid meeting )



Colleagues are encouraged to submit an abstract to the E2.1 Session on «Magnetic Flux ropes in solar and stellar environments» at the upcoming 43rd COSPAR Scientific Assembly.

The assembly will be virtual for international participation.

The abstract submission website isreopened :

https://www.cospar2020.org/abstracts.php

Abstract submission deadline: 5th October 2020

Main Scientific Organizer: Brigitte Schmieder (Observatoire de Paris, France -­‐KU Leuven, Belgium)

Deputy Organizer: Cristina Mandrini (IAFE, Rep. Argentina)

Session details :

Rationale :

Magnetic flux bundles or ropes are the main building blocks forming active regions. Their destabilization can lead to the most violentevents -­‐-­‐flares, coronal mass ejections (CMEs), and energetic particle events. After eruption, they are observed over a wide range of spatial scales throughout the heliosphere. Specific configurations of these structures can produce the strongest geomagnetic storms as they impact the Earth's magnetosphere. Stellar CMEs, which in analogy to solar CMEs could be caused by the eruption of large-­‐scale flux ropes, may play an important role in mass and angular momentum losses of young Sun-­‐like stars. It is alsohighly probable that observed superflares might be associated with very large stellar CMEs. Such powerful events mayhave significant implications for the physical conditions and the eventual habitability of orbiting exoplanets. The proposed event aims toshed light on the fundamental physics of different sets offlux rope structures, their genesis, escape of confinement, interaction, relevance for solar/stellar environments and plausible impact on their planets.

Four sessions are planned :

    1. Solar and stellar dynamos, emergence of magnetic flux ropes, flux rope characteristics

    2. The disruption and eruption of flux ropes, evolution of coronal mass ejections (CMEs)

    3. Detection and models of flux rope evolution and interaction in the heliosphere

    4. The stars: flares, stellar prominence, stellar coronal mass ejections: observations and theory

The program should be adapted by the COSPAR logistics.