scholarly journals IMAGING AND SPECTROSCOPIC OBSERVATIONS OF MAGNETIC RECONNECTION AND CHROMOSPHERIC EVAPORATION IN A SOLAR FLARE

2014 ◽  
Vol 797 (2) ◽  
pp. L14 ◽  
Author(s):  
Hui Tian ◽  
Gang Li ◽  
Katharine K. Reeves ◽  
John C. Raymond ◽  
Fan Guo ◽  
...  
Keyword(s):  
Solar Flare ◽  
Magnetic Reconnection ◽  
Spectroscopic Observations ◽  
Chromospheric Evaporation

scholarly journals Spectroscopic Observations of Magnetic Reconnection and Chromospheric Evaporation in an X-shaped Solar Flare

2017 ◽  
Vol 848 (2) ◽  
pp. 118 ◽  
Author(s):  
Y. Li ◽  
M. Kelly ◽  
M. D. Ding ◽  
J. Qiu ◽  
X. S. Zhu ◽  
...  
Keyword(s):  
Solar Flare ◽  
Magnetic Reconnection ◽  
Spectroscopic Observations ◽  
Chromospheric Evaporation

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.

scholarly journals SLIPPING MAGNETIC RECONNECTION, CHROMOSPHERIC EVAPORATION, IMPLOSION, AND PRECURSORS IN THE 2014 SEPTEMBER 10 X1.6-CLASS SOLAR FLARE

2016 ◽  
Vol 823 (1) ◽  
pp. 41 ◽  
Author(s):  
Jaroslav Dudík ◽  
Vanessa Polito ◽  
Miho Janvier ◽  
Sargam M. Mulay ◽  
Marian Karlický ◽  
...  
Keyword(s):  
Solar Flare ◽  
Magnetic Reconnection ◽  
Chromospheric Evaporation

scholarly journals Enhanced Turbulence and Heating Observed Preceding the Impulsive Phase in a Solar Flare

1989 ◽  
Vol 104 (2) ◽  
pp. 231-234
Author(s):  
Chung-Chieh Cheng ◽  
K.G. Widing
Keyword(s):  
Solar Flare ◽  
Transition Region ◽  
Normal Incidence ◽  
Impulsive Phase ◽  
Energetic Particles ◽  
Line Profiles ◽  
Chromospheric Evaporation

AbstractWe studied the unique EUV spectra of the 21 Jan. 1974 flare observed by the NRL Normal-Incidence Slit Spectrometer (SO 82B) onboard the Skylab. The results show that the pre-impulsive transition region plasmas exhibited enhanced turbulence and heating before the acceleration of energetic particles. The absence of blue-shifted components in the Fe XXI line profiles shows that the chromospheric evaporation is not important in this flare.

scholarly journals A topological analysis of the magnetic breakout model for an eruptive solar flare

2005 ◽  
Vol 461 (2059) ◽  
pp. 2099-2120 ◽  
Author(s):  
Rhona Maclean ◽  
Colin Beveridge ◽  
Dana Longcope ◽  
Daniel Brown ◽  
Eric Priest
Keyword(s):  
Solar Flare ◽  
Magnetic Reconnection ◽  
Topological Analysis ◽  
Null Point ◽  
Topological Approach ◽  
Sunspot Model ◽  
New Class ◽  
Linear Force ◽  
Field Lines

The magnetic breakout model gives an elegant explanation for the onset of an eruptive solar flare, involving magnetic reconnection at a coronal null point which leads to the initially enclosed flux ‘breaking out’ to large distances. In this paper we take a topological approach to the study of the conditions required for this breakout phenomenon to occur. The evolution of a simple delta sunspot model, up to the point of breakout, is analysed through several sequences of potential and linear force-free quasi-static equilibria. We show that any new class of field lines, such as those connecting to large distances, must be created through a global topological bifurcation and derive rules to predict the topological reconfiguration due to various types of bifurcation.

A loop-top hard X-ray source in a compact solar flare as evidence for magnetic reconnection

Nature ◽  
1994 ◽  
Vol 371 (6497) ◽  
pp. 495-497 ◽  
Author(s):  
S. Masuda ◽  
T. Kosugi ◽  
H. Hara ◽  
S. Tsuneta ◽  
Y. Ogawara
Keyword(s):  
Solar Flare ◽  
Magnetic Reconnection ◽  
X Ray
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