scholarly journals Magnetohydrodynamic Numerical Simulations of Solar X-Ray Jets Based on the Magnetic Reconnection Model That Includes Chromospheric Evaporation

2003 ◽  
Vol 593 (2) ◽  
pp. L133-L136 ◽  
Author(s):  
Takehiro Miyagoshi ◽  
Takaaki Yokoyama
Keyword(s):  
Numerical Simulations ◽  
Magnetic Reconnection ◽  
X Ray ◽  
Chromospheric Evaporation ◽  
Reconnection Model

scholarly journals MHD Simulation of Chromospheric Evaporation in a Solar Flare Based on Magnetic Reconnection Model

1998 ◽  
Vol 188 ◽  
pp. 213-214
Author(s):  
T. Yokoyama ◽  
K. Shibata
Keyword(s):  
Heat Conduction ◽  
Solar Flare ◽  
Magnetic Reconnection ◽  
The Other ◽  
Simple Loop ◽  
X Ray ◽  
Long Duration ◽  
Chromospheric Evaporation ◽  
Anisotropic Heat Conduction ◽  
Reconnection Model

Two-dimensional magnetohydrodynamic simulation of a solar flare is performed using a newly developed MHD code including nonlinear anisotropic heat conduction effect (Fig. 1; Yokoyama & Shibata 1997a). The numerical simulation starts with a vertical current sheet which is line-tied at one end to a dense chromosphere. The flare energy is released by the magnetic reconnection mechanism stimulated initially by the resistivity perturbation in the corona. The released thermal energy is transported into the chromosphere by heat conduction and drives chromospheric evaporation. Owing to the heat conduction effect, the adiabatic slow-mode MHD shocks emanated from the neutral point are dissociated into conduction fronts and isothermal shocks (Yokoyama & Shibata 1997b). Temperature and derived soft X-ray distributions are similar to the cusp-like structure of long-duration-event (LDE) flares observed by the soft X-ray telescope aboard Yohkoh satellite. On the other hand density and radio maps show a simple loop configuration which is consistent with the observation with Nobeyama Radio Heliograph. Two interesting new features are found. One is a pair of high density humps on the evaporated plasma loops formed at the collision site between the reconnection jet and the evaporation flow. The other is the loop-top blob behind the fast-mode MHD shock.

Magnetic reconnection model for X-ray flare loop interaction

1995 ◽  
Vol 226 (1) ◽  
pp. 31-46 ◽  
Author(s):  
Zhen-Da Zhang ◽  
Xiao-Qing Li ◽  
R. N. Smartt
Keyword(s):  
Magnetic Reconnection ◽  
Flare Loop ◽  
X Ray ◽  
Reconnection Model

Magnetic reconnection model of X-ray plasmas in the Galactic center

2000 ◽  
Vol 25 (3-4) ◽  
pp. 505-508
Author(s):  
T. Yokoyama ◽  
S. Tanuma ◽  
T. Kudoh ◽  
K. Shibata
Keyword(s):  
Magnetic Reconnection ◽  
Galactic Center ◽  
X Ray ◽  
Reconnection Model

scholarly journals MHD Numerical Simulations of Magnetic Reconnection Associated with Emerging Flux

1993 ◽  
Vol 141 ◽  
pp. 500-503
Author(s):  
K. Shibata ◽  
S. Nozawa ◽  
R. Matsumoto
Keyword(s):  
Magnetic Field ◽  
Numerical Simulations ◽  
Magnetic Reconnection ◽  
Coronal Magnetic Field ◽  
Two Dimensional ◽  
Magnetic Islands ◽  
X Ray ◽  
Hot Plasma ◽  
Mass Ejection ◽  
Coronal Field

AbstractTwo-dimensional (2D) magnetohydrodynamic (MHD) numerical simulations have been performed to study magnetic reconnection between emerging flux and the overlying coronal magnetic field, taking into account of gravity. It is found that (1) reconnection starts when most of chromospheric mass in the current sheet between the emerging flux and the coronal field has drained down along the loop because of gravity, (2) multiple magnetic islands, which confine cool, dense chromospheric plasma, are created in the sheet; the islands coalesce dynamically and are ejected along the sheet, together with the ambient hot plasma, at Alfven speed. The coexistence of hot and cool plasmas in the mass ejection (jet) associated with the reconnection seems to explain those X-ray jets observed by Yohkoh, which are identified with Hα surges.

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