scholarly journals Magnetic Flux Braiding: Force‐free Equilibria and Current Sheets

1998 ◽  
Vol 500 (1) ◽  
pp. 471-482 ◽  
Author(s):  
A. W. Longbottom ◽  
G. J. Rickard ◽  
I. J. D. Craig ◽  
A. D. Sneyd
Keyword(s):  

1979 ◽  
Vol 40 (C7) ◽  
pp. C7-507-C7-510
Author(s):  
N. A. Koshilev ◽  
N. A. Strokin ◽  
A. A. Shisko ◽  
A. V. Mikhalev




2015 ◽  
Vol 22 (6) ◽  
pp. 062102 ◽  
Author(s):  
P. L. Pritchett
Keyword(s):  


2004 ◽  
Vol 618 (2) ◽  
pp. L153-L156 ◽  
Author(s):  
K. Galsgaard ◽  
F. Moreno-Insertis ◽  
V. Archontis ◽  
A. Hood


2017 ◽  
Vol 44 (15) ◽  
pp. 7653-7662 ◽  
Author(s):  
Takuya Hara ◽  
Yuki Harada ◽  
David L. Mitchell ◽  
Gina A. DiBraccio ◽  
Jared R. Espley ◽  
...  


2020 ◽  
Vol 645 ◽  
pp. A3
Author(s):  
N. Yadav ◽  
R. H. Cameron ◽  
S. K. Solanki

Context. Vortex flows exist across a broad range of spatial and temporal scales in the solar atmosphere. Small-scale vortices are thought to play an important role in energy transport in the solar atmosphere. However, their physical properties remain poorly understood due to the limited spatial resolution of the observations. Aims. We explore and analyze the physical properties of small-scale vortices inside magnetic flux tubes using numerical simulations, and investigate whether they contribute to heating the chromosphere in a plage region. Methods. Using the three-dimensional radiative magnetohydrodynamic simulation code MURaM, we perform numerical simulations of a unipolar solar plage region. To detect and isolate vortices we use the swirling strength criterion and select the locations where the fluid is rotating with an angular velocity greater than a certain threshold. We concentrate on small-scale vortices as they are the strongest and carry most of the energy. We explore the spatial profiles of physical quantities such as density and horizontal velocity inside these vortices. Moreover, to learn their general characteristics, a statistical investigation is performed. Results. Magnetic flux tubes have a complex filamentary substructure harboring an abundance of small-scale vortices. At the interfaces between vortices strong current sheets are formed that may dissipate and heat the solar chromosphere. Statistically, vortices have higher densities and higher temperatures than the average values at the same geometrical height in the chromosphere. Conclusions. We conclude that small-scale vortices are ubiquitous in solar plage regions; they are denser and hotter structures that contribute to chromospheric heating, possibly by dissipation of the current sheets formed at their interfaces.





1979 ◽  
Vol 44 ◽  
pp. 189-191
Author(s):  
M.H. Gokhale ◽  
K.R. Sivaraman

Quiescent prominences are known to occur invariably above the neutral lines in the large scale photospheric fields. This suggests that such prominences may be coronal current sheets across which the magnetic fields reconnect (cf. e.g. Raadu and Kuperus, 1973). In the absence of any satisfactory model for quiescent prominences (cf. Report of Working Group 1 in this Colloquium), the reconnection hypothesis remains as yet unsettled. However, if it is true, we have here an evidence to show that the quiescent prominences outside the active regions might account for the reconnection of almost all the photospheric magnetic flux emerging in the active regions as required by the theories of the 11-yr cycle of activity (e.g. Babcock, 1961).





Sign in / Sign up

Export Citation Format

Share Document