Numerical simulations of kink instability in line-tied coronal Loops

Details Numerical simulations of kink instability in line-tied coronal Loops Numerical simulations of kink instability in line-tied coronal Loops

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001a%26a...373.1089g&link_type=abstract

Astronomy and Astrophysics, v.373, p.1089-1098 (2001)

Astronomy and Astrophysics

Astrophysics

26

Mhd, Sun

Scientific paper

The results from numerical simulations carried out using a new shock-capturing, Lagrangian-remap, 3D MHD code, Lare3d are presented. We study the evolution of the m=1 kink mode instability in a photospherically line-tied coronal loop that has no net axial current. During the non-linear evolution of the kink instability, large current concentrations develop in the neighbourhood of the infinite length mode rational surface. We investigate whether this strong current saturates at a finite value or whether scaling indicates current sheet formation. In particular, we consider the effect of the shear, defined by r phi ' / phi where phi = L Btheta / r Bz is the fieldline twist of the loop, on the current concentration. We also include a non-uniform resistivity in the simulations and observe the amount of free magnetic energy released by magnetic reconnection.

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