Solar Prominences: Theory and models (Fleshing out the magnetic skeleton)

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Friday, August 24, 2018

Magnetic fields suspend the relatively cool material of solar prominences in an otherwise hot corona. A comprehensive understanding of solar prominences ultimately requires complex and dynamic models, constrained and validated by observations spanning the solar atmosphere.

Painting the dips'' of a magnetic skeleton results in sheet-like prominences image
"Painting the dips" of a magnetic skeleton results in sheet-like prominences, independent of magnetic topology. a) Demonstration of the small region this would represent for a sample, dipped field line within a flux rope field model, and b) demonstration for many field lines within the rope (after Gibson and Fan, 2006). c) Painted dips within 3D sheared-arcade model of Aulanier et al., 2002. d) Painted dips within 3D analytic model of spheromak-type magnetic flux rope (Lites and Low, 1997

Observations give us information about the structure of the "magnetic skeleton" that supports and surrounds the prominence. Energetically-sophisticated magnetohydrodynamic simulations then add flesh and blood to the skeleton, demonstrating how a thermally varying plasma may pulse through to form the prominence, and how the plasma and magnetic skeleton dynamically interact.

Publication Name: Living Reviews in Solar Physics

First HAO Author's Name: Sarah Gibson

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