The enduring mystery of the solar corona

Thursday, September 16, 2021

The author reviews why, after almost 8 decades, we still have a coronal heating problem.

A series of diagrams
Magnetic field lines are shown extending from the Sun into interplanetary space (a and b) and returning to the solar surface (other panels). Each shaded region shows how small scales are produced from larger-scale motions at the solar surface by phase mixing (panel b), resonant absorption (panel e), and the quasi-static evolution of current sheets as the near ideal MHD attempts to develop tangential discontinuities (panel f). In panels (a) the motions can be thought of as propagating and standing waves, and in panel (f) the motions are slow enough that a quasi-static evolution is envisaged.
Publication: Physics World
First HAO Author: Philip Judge

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