Two-dimensional magnetohydrodynamic model of emerging magnetic flux in the solar atmosphere

1989 ◽  
Vol 345 ◽  
pp. 584 ◽  
Author(s):  
K. Shibata ◽  
T. Tajima ◽  
R. S. Steinolfson ◽  
R. Matsumoto
Keyword(s):  
Magnetic Flux ◽  
Solar Atmosphere ◽  
Two Dimensional ◽  
Magnetohydrodynamic Model

scholarly journals Nonlinear Evolution of Parker Instability of Isolated Magnetic Flux Sheet and Its Application to Emerging Magnetic Flux in the Solar Atmosphere

1989 ◽  
Vol 104 (2) ◽  
pp. 281-284
Author(s):  
K. Shibata ◽  
T. Tajima ◽  
R. Steinolfson ◽  
R. Matsumoto
Keyword(s):  
Magnetic Flux ◽  
Solar Atmosphere ◽  
Nonlinear Evolution ◽  
Magnetic Loop ◽  
Numerical Results ◽  
Solar Photosphere ◽  
Two Dimensional ◽  
Nonlinear Stage

AbstractA two dimensional MHD code is used to study the nonlinear evolution of the Parker instability in isolated horizontal magnetic flux imbedded in (or below) the solar photosphere. It is found that the magnetic loop expands self-similarly in the nonlinear stage. Numerical results explain many features observed in emerging flux regions.

The Characteristics of Thin Magnetic Flux Tubes in the Lower Solar Atmosphere Observed byHinode/SOT in the G band and in Ca ii H Bright Points

2017 ◽  
Vol 851 (1) ◽  
pp. 42 ◽  
Author(s):  
Jianping Xiong ◽  
Yunfei Yang ◽  
Chunlan Jin ◽  
Kaifan Ji ◽  
Song Feng ◽  
...  
Keyword(s):  
Magnetic Flux ◽  
Solar Atmosphere ◽  
Flux Tubes ◽  
Magnetic Flux Tubes ◽  
Lower Solar Atmosphere

scholarly journals Two-dimensional Radiative Magnetohydrodynamic Simulations of Partial Ionization in the Chromosphere. II. Dynamics and Energetics of the Low Solar Atmosphere

2017 ◽  
Vol 847 (1) ◽  
pp. 36 ◽  
Author(s):  
Juan Martínez-Sykora ◽  
Bart De Pontieu ◽  
Mats Carlsson ◽  
Viggo H. Hansteen ◽  
Daniel Nóbrega-Siverio ◽  
...  
Keyword(s):  
Solar Atmosphere ◽  
Two Dimensional ◽  
Magnetohydrodynamic Simulations

Magnetic properties of two-dimensional Josephson networks: Self-organized criticality in magnetic flux dynamics

JETP Letters ◽  
2000 ◽  
Vol 72 (1) ◽  
pp. 26-29 ◽  
Author(s):  
S. M. Ishikaev ◽  
É. V. Matizen ◽  
V. V. Ryazanov ◽  
V. A. Oboznov ◽  
A. V. Veretennikov
Keyword(s):  
Magnetic Properties ◽  
Magnetic Flux ◽  
Two Dimensional ◽  
Flux Dynamics ◽  
Self Organized ◽  
Self Organized Criticality

Magnetic Flux of "Vortices" on the Two-Dimensional Hall Surface

1984 ◽  
Vol 53 (27) ◽  
pp. 2591-2591 ◽  
Author(s):  
F. D. M. Haldane ◽  
Liang Chen
Keyword(s):  
Magnetic Flux ◽  
Two Dimensional

scholarly journals Observations of flux rope formation prior to coronal mass ejections

2013 ◽  
Vol 8 (S300) ◽  
pp. 209-214 ◽  
Author(s):  
Lucie M. Green ◽  
Bernhard Kliem
Keyword(s):  
Magnetic Flux ◽  
Magnetic Structure ◽  
Solar Atmosphere ◽  
Coronal Mass Ejections ◽  
Flux Rope ◽  
Active Regions ◽  
Magnetic Configuration ◽  
Magnetic Flux Rope ◽  
Source Regions ◽  
Flux Ropes

AbstractUnderstanding the magnetic configuration of the source regions of coronal mass ejections (CMEs) is vital in order to determine the trigger and driver of these events. Observations of four CME productive active regions are presented here, which indicate that the pre-eruption magnetic configuration is that of a magnetic flux rope. The flux ropes are formed in the solar atmosphere by the process known as flux cancellation and are stable for several hours before the eruption. The observations also indicate that the magnetic structure that erupts is not the entire flux rope as initially formed, raising the question of whether the flux rope is able to undergo a partial eruption or whether it undergoes a transition in specific flux rope configuration shortly before the CME.

scholarly journals Numerical simulations of the lower solar atmosphere heating by two-fluid nonlinear Alfvén waves

2020 ◽  
Vol 639 ◽  
pp. A45
Author(s):  
B. Kuźma ◽  
D. Wójcik ◽  
K. Murawski ◽  
D. Yuan ◽  
S. Poedts
Keyword(s):  
Magnetic Flux ◽  
Numerical Simulations ◽  
Solar Atmosphere ◽  
Flux Tube ◽  
Alfven Waves ◽  
Alfven Wave ◽  
Magnetic Flux Tube ◽  
Alfvén Waves ◽  
Two Fluid ◽  
Lower Solar Atmosphere

Context. We present new insight into the long-standing problem of plasma heating in the lower solar atmosphere in terms of collisional dissipation caused by two-fluid Alfvén waves. Aims. Using numerical simulations, we study Alfvén wave propagation and dissipation in a magnetic flux tube and their heating effect. Methods. We set up 2.5-dimensional numerical simulations with a semi-empirical model of a stratified solar atmosphere and a force-free magnetic field mimicking a magnetic flux tube. We consider a partially ionized plasma consisting of ion + electron and neutral fluids, which are coupled by ion-neutral collisions. Results. We find that Alfvén waves, which are directly generated by a monochromatic driver at the bottom of the photosphere, experience strong damping. Low-amplitude waves do not thermalize sufficient wave energy to heat the solar atmospheric plasma. However, Alfvén waves with amplitudes greater than 0.1 km s−1 drive through ponderomotive force magneto-acoustic waves in higher atmospheric layers. These waves are damped by ion-neutral collisions, and the thermal energy released in this process leads to heating of the upper photosphere and the chromosphere. Conclusions. We infer that, as a result of ion-neutral collisions, the energy carried initially by Alfvén waves is thermalized in the upper photosphere and the chromosphere, and the corresponding heating rate is large enough to compensate radiative and thermal-conduction energy losses therein.

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