Energy release and plasma heating by forced magnetic reconnection

1998 ◽  
Vol 5 (5) ◽  
pp. 1506-1513 ◽  
Author(s):  
G. E. Vekstein ◽  
Rekha Jain
Keyword(s):  
Magnetic Reconnection ◽  
Energy Release ◽  
Plasma Heating ◽  
Forced Magnetic Reconnection

scholarly journals Forced magnetic reconnection and plasmoid coalescence

2019 ◽  
Vol 623 ◽  
pp. A15 ◽  
Author(s):  
M. A. Potter ◽  
P. K. Browning ◽  
M. Gordovskyy
Keyword(s):  
Magnetic Reconnection ◽  
Current Sheet ◽  
Energy Release ◽  
External Perturbation ◽  
Mhd Equations ◽  
Magnetic Islands ◽  
Initial Current ◽  
Reconnection Region ◽  
Non Linear ◽  
Forced Magnetic Reconnection

Context. Forced magnetic reconnection, a reconnection event triggered by external perturbation, should be ubiquitous in the solar corona. Energy released during such cases can be much greater than that which was introduced by the perturbation. The exact dynamics of magnetic reconnection events are determined by the structure and complexity of the reconnection region: the thickness of reconnecting layers, the field curvature; the presence, shapes and sizes of magnetic islands. It is unclear how the properties of the external perturbation and the initial current sheet affect the reconnection region properties, and thereby the reconnection dynamics and energy release profile. Aims. We investigate the effect of the form of the external perturbation and initial current sheet on the evolution of the reconnection region and the energy release process. Chiefly we explore the non-linear interactions between multiple, simultaneous perturbations, which represent more realistic scenarios. Future work will use these results in test particle simulations to investigate particle acceleration over multiple reconnection events. Methods. Simulations are performed using Lare2d, a 2.5D Lagrangian-remap solver for the visco-resistive MHD equations. The model of forced reconnection is extended to include superpositions of sinusoidal driving disturbances, including localised Gaussian perturbations. A transient perturbation is applied to the boundaries of a region containing a force-free current sheet. The simulation domain is sufficiently wide to allow multiple magnetic islands to form and coalesce. Results. Island coalescence contributes significantly to energy release and involves rapid reconnection. Long wavelength modes in perturbations dominate the evolution, without the presence of which reconnection is either slow, as in the case of short wavelength modes, or the initial current sheet remains stable, as in the case of noise perturbations. Multiple perturbations combine in a highly non-linear manner: reconnection is typically faster than when either disturbance is applied individually, with multiple low-energy events contributing to the same total energy release.

Magnetic reconnection and energy release in a long-duration stellar flare

1986 ◽  
Vol 6 (8) ◽  
pp. 145-148 ◽  
Author(s):  
G. Poletto ◽  
R. Pallavicini ◽  
R.A. Kopp
Keyword(s):  
Magnetic Reconnection ◽  
Energy Release ◽  
Stellar Flare ◽  
Long Duration

Plasma heating by collisionless magnetic reconnection: Analysis and computation

1993 ◽  
Vol 98 (A3) ◽  
pp. 4013-4040 ◽  
Author(s):  
R. W. Moses ◽  
J. M. Finn ◽  
K. M. Ling
Keyword(s):  
Magnetic Reconnection ◽  
Plasma Heating

Possible two-step solar energy release mechanism due to turbulent magnetic reconnection

2005 ◽  
Vol 12 (5) ◽  
pp. 052901 ◽  
Author(s):  
Quan-Lin Fan ◽  
Xue-Shang Feng ◽  
Chang-Qing Xiang
Keyword(s):  
Solar Energy ◽  
Magnetic Reconnection ◽  
Energy Release ◽  
Release Mechanism

scholarly journals Hard X-ray Spectrum of the Above-the-Looptop Source in Impulsive Solar Flares

2000 ◽  
Vol 195 ◽  
pp. 413-414
Author(s):  
S. Masuda
Keyword(s):  
Magnetic Reconnection ◽  
Energy Release ◽  
Solar Flares ◽  
Count Rate ◽  
High Quality ◽  
X Ray ◽  
Flare Energy

Extended AbstractThe Hard X-ray Telescope (HXT: Kosugi et al. 1991) onboard Yohkoh has observed that, in impulsive solar flares, a hard X-ray source is located above the apex of a soft X-ray flaring loop, in addition to double footpoint sources (Masuda et al. 1994, 1995). This observation suggests that flare energy-release, probably magnetic reconnection, takes place not in the soft X-ray loop but above the loop. It is important to derive the hard X-ray spectrum of the above-the-looptop source accurately in order to understand how electrons are energized there. The above-the-looptop source was most clearly observed during the 13 January 1992 flare. However, the count rate, especially in the H-band (53–93 keV), is too small to synthesize high-quality images and to derive an accurate spectrum.

Sign in / Sign up

Export Citation Format

Share Document