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Parallel sessions
Sessions
id
date time
2022-03-08 11:43:00
Dynamics and Structure of the Magnetic Field in the Sun's Atmosphere
Solar2
The magnetic field is at the heart of most phenomena in the solar atmosphere. It structures the atmosphere in closed and open flux regions, it guides plasma flows, it transports energy and helicity, and it provides the energy for coronal heating, solar flares, and coronal mass ejections with energy releases on a wide range of scales. The state of the magnetic field is the result of a delicate balance between energy input, provided mainly via flows and flux emergence at the photospheric boundary, as well as various forms of energy release in the atmosphere and outflow from the atmosphere. The efficiency of energy conversion in the atmosphere is in turn dependent on an interplay between the largest scales where the energy is stored and the much smaller scales where the energy is dissipated. Fundamental processes like these and the resulting state, structure and dynamics of the Sun's magnetic field remain critical topics for the major unsolved problems of solar physics. We invite contributions from both theory and observation related to the dynamics and structure of the Sun's magnetic field, including on questions of cross-scale coupling, turbulence, magnetic reconnection, energy and helicity transport, related phenomena, and tools to investigate these processes
Gunnar Hornig, David MacTaggart, Karen Meyer, Christopher Prior, Alexander Russell, Peter Wyper, Anthony Yeates
Fri. 09:00-10:30
09.00-09.15 Mykola Gordovskyy: Particle acceleration and their escape into the heliosphere in solar flares
09.15-09.30 Simon Candelaresi: Polynomial knot invariants in the dynamics of braided magnetic fields
09.30-09.45 Raheem Beg, Alexander J. B. Russell, Gunnar Hornig: Structure and topology of self-generated turbulent reconnection layers
09.45-10.00 Prantika Bhowmik: Exploring the origin of stealth coronal mass ejections using magnetofrictional simulations
10.00-10.15 Lilli Nadol: Coronal Magnetic Field Extrapolation Using a Specific Family of Analytical 3D Magnetohydrostatic Equilibria—Practical Aspects
10.15-10.30 Thomas Howson: The response of the coronal magnetic field to random foot point driving