1 code implementation • 3 Dec 2018 • Christopher B. Smiet, Hugo J. de Blank, Tobias A. de Jong, David N. L. Kok, Dirk Bouwmeester
In simulations this equilibrium is observed when highly tangled field lines relax in a high-pressure (relative to the magnetic field strength) environment, a situation that occurs when the twisted field of a coronal loop is ejected into the interplanetary solar wind.
Plasma Physics Solar and Stellar Astrophysics
