A Two-dimensional Magnetohydrodynamic Simulation of Chromospheric Evaporation in a Solar Flare Based on a Magnetic 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.

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

The Astrophysical Journal ◽

10.1088/2041-8205/797/2/l14 ◽

2014 ◽

Vol 797 (2) ◽

pp. L14 ◽

Cited By ~ 77

Author(s):

Hui Tian ◽

Gang Li ◽

Katharine K. Reeves ◽

John C. Raymond ◽

Fan Guo ◽

...

Keyword(s):

Solar Flare ◽

Magnetic Reconnection ◽

Spectroscopic Observations ◽

Chromospheric Evaporation

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Magnetohydrodynamic Simulation of Solar Coronal Chromospheric Evaporation Jets Caused by Magnetic Reconnection Associated with Magnetic Flux Emergence

The Astrophysical Journal ◽

10.1086/423731 ◽

2004 ◽

Vol 614 (2) ◽

pp. 1042-1053 ◽

Cited By ~ 35

Author(s):

Takehiro Miyagoshi ◽

Takaaki Yokoyama

Keyword(s):

Magnetic Flux ◽

Magnetic Reconnection ◽

Flux Emergence ◽

Chromospheric Evaporation ◽

Magnetohydrodynamic Simulation ◽

Solar Coronal

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Large solar-type magnetic reconnection model for magnetar giant flare

Proceedings of the International Astronomical Union ◽

10.1017/s1743921309030282 ◽

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.

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