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

scholarly journals Observation of Reconnection Inflow of a Solar Flare

2001 ◽  
Vol 203 ◽  
pp. 344-346
Author(s):  
T. Yokoyama ◽  
K. Akita ◽  
T. Morimoto ◽  
K. Inoue ◽  
J. Newmark
Keyword(s):  
Mach Number ◽  
Solar Flare ◽  
Magnetic Reconnection ◽  
Reconnection Rate ◽  
X Ray ◽  
North East ◽  
The North ◽  
Upper Limit ◽  
Long Duration ◽  
East Limb

We find an important piece of evidence for magnetic reconnection inflow in a flare on March 18, 1999. The flare occurred on the north-east limb, displaying a nice cusp-shaped soft X-ray loop and a plasmoid ejection typical for the long-duration-events. As the plasmoid is ejected, magnetic reconnection occurs at the disconnecting point. A clear ingoing pattern toward the magnetic X-point is seen. The velocity of this apparent motion is about 5 km sec−1, which is an upper limit on reconnection inflow speed. Based on this observation, we derive the reconnection rate as MA = 0.001 − 0.03, where MA is a Alfvén Mach number of the inflow.

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 Magnetic Reconnection during the Post-impulsive Phase of a Long-duration Solar Flare: Bidirectional Outflows as a Cause of Microwave and X-Ray Bursts

2020 ◽  
Vol 900 (1) ◽  
pp. 17 ◽  
Author(s):  
Sijie Yu ◽  
Bin Chen ◽  
Katharine K. Reeves ◽  
Dale E. Gary ◽  
Sophie Musset ◽  
...  
Keyword(s):  
Solar Flare ◽  
Magnetic Reconnection ◽  
Impulsive Phase ◽  
X Ray ◽  
Long Duration

X-ray plasma ejection and magnetic reconnection

2000 ◽  
Vol 26 (3) ◽  
pp. 461-464 ◽  
Author(s):  
Masamitsu Ohyama ◽  
Kazunari Shibata
Keyword(s):  
Magnetic Reconnection ◽  
X Ray

Diagnostics of solar flare hard X-ray sources

Solar Physics ◽  
1978 ◽  
Vol 58 (1) ◽  
pp. 139-148 ◽  
Author(s):  
Peter Hoyng ◽  
Joshua W. Knight ◽  
Daniel S. Spicer
Keyword(s):  
Solar Flare ◽  
X Ray

scholarly journals Using the maximum X-ray flux ratio and X-ray background to predict solar flare class

Space Weather ◽  
2015 ◽  
Vol 13 (5) ◽  
pp. 286-297 ◽  
Author(s):  
L. M. Winter ◽  
K. Balasubramaniam
Keyword(s):  
Solar Flare ◽  
Flux Ratio ◽  
X Ray ◽  
X Ray Background

scholarly journals Electron Bremsstrahlung Hard X-Ray Spectra, Electron Distributions, and Energetics in the 2002 July 23 Solar Flare

2003 ◽  
Vol 595 (2) ◽  
pp. L97-L101 ◽  
Author(s):  
Gordon D. Holman ◽  
Linhui Sui ◽  
Richard A. Schwartz ◽  
A. Gordon Emslie
Keyword(s):  
Solar Flare ◽  
X Ray ◽  
Electron Bremsstrahlung ◽  
Electron Distributions

Correlations of solar-flare electron events with radio and X-ray emission from the sun

1968 ◽  
Vol 46 (10) ◽  
pp. S757-S760 ◽  
Author(s):  
R. P. Lin
Keyword(s):  
Solar Flare ◽  
Solar Radio ◽  
Interplanetary Space ◽  
The Sun ◽  
Radio Bursts ◽  
Radio Observations ◽  
X Ray ◽  
Type Iii ◽  
Electron Event ◽  
Burst Emission

The > 40-keV solar-flare electrons observed by the IMP III and Mariner IV satellites are shown to be closely correlated with solar radio and X-ray burst emission. In particular, intense type III radio bursts are observed to accompany solar electron-event flares. The energies of the electrons, the total number of electrons, and the size of the electron source at the sun can be inferred from radio observations. The characteristics of the electrons observed in interplanetary space are consistent with these radio observations. Therefore these electrons are identified as the exciting agents of the type III emission. It has been noted that the radio and X-ray bursts are part of the flash phase of flares. The observations indicate that a striking feature of the flash phase is the production of electrons of 10–100 keV energies.

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