A Solar Flare Model Based on Magnetic Reconnection between Current‐carrying Loops

1997 ◽  
Vol 486 (1) ◽  
pp. 521-533 ◽  
Author(s):  
D. B. Melrose
Keyword(s):  
Solar Flare ◽  
Magnetic Reconnection ◽  
Model Based ◽  
Flare Model

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 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

scholarly journals Large solar-type magnetic reconnection model for magnetar giant flare

2008 ◽  
Vol 4 (S259) ◽  
pp. 123-124
Author(s):  
Youhei Masada
Keyword(s):  
Solar Flare ◽  
Magnetic Reconnection ◽  
Radiative Heat ◽  
Energy Transport ◽  
Magnetic Energy ◽  
Baryonic Matter ◽  
Solar Type ◽  
Mass Ejection ◽  
Giant Flare ◽  
Reconnection Model

AbstractWe construct a magnetic reconnection model for magnetar giant flare in the framework of solar flare/coronal mass ejection theory. As is the case with the solar flare, the explosive magnetic reconnection plays a crucial role in the energetics of the magnetar flare. A key physics controlling the energy transport in the system, on the other hand, is the radiative process unlike that in the solar flare. After the release of the magnetic energy via the magnetic reconnection, the radiative heat flux drives the baryonic evaporation. Our model can predict that the baryonic matter evaporated in the preflare stage would be the origin of the radio emitting ejecta observed in association with the giant flare on 2004 December 27 from SGR1806-20.

scholarly journals Simultaneous Observation of a Flux Rope Eruption and Magnetic Reconnection during an X-class Solar Flare

2018 ◽  
Vol 853 (1) ◽  
pp. L18 ◽  
Author(s):  
X. L. Yan ◽  
L. H. Yang ◽  
Z. K. Xue ◽  
Z. X. Mei ◽  
D. F. Kong ◽  
...  
Keyword(s):  
Solar Flare ◽  
Magnetic Reconnection ◽  
Flux Rope ◽  
Simultaneous Observation

Hα, Extreme‐Ultraviolet, and Microwave Observations of the 2000 March 22 Solar Flare and Spontaneous Magnetic Reconnection

2003 ◽  
Vol 585 (1) ◽  
pp. 524-535 ◽  
Author(s):  
Jeongwoo Lee ◽  
Peter T. Gallagher ◽  
Dale E. Gary ◽  
Gelu M. Nita ◽  
G. S. Choe ◽  
...  
Keyword(s):  
Solar Flare ◽  
Magnetic Reconnection ◽  
Extreme Ultraviolet

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.

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