Journal
ASTROPHYSICAL JOURNAL
Volume 714, Issue 2, Pages 1762-1778Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/714/2/1762
Keywords
magnetic fields; magnetic reconnection; magnetohydrodynamics (MHD); Sun: corona; Sun: magnetic topology
Categories
Funding
- NASA
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Recent solar observations (e. g., obtained with Hinode and STEREO) have revealed that coronal jets are a more frequent phenomenon than previously believed. This higher frequency results, in part, from the fact that jets exhibit a homologous behavior: successive jets recur at the same location with similar morphological features. We present the results of three-dimensional (3D) numerical simulations of our model for coronal jets. This study demonstrates the ability of the model to generate recurrent 3D untwisting quasi-homologous jets when a stress is constantly applied at the photospheric boundary. The homology results from the property of the 3D null-point system to relax to a state topologically similar to its initial configuration. In addition, we find two distinct regimes of reconnection in the simulations: an impulsive 3D mode involving a helical rotating current sheet that generates the jet and a quasi-steady mode that occurs in a 2D-like current sheet located along the fan between the sheared spines. We argue that these different regimes can explain the observed link between jets and plumes.
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