Volume 577, May 2015
|Number of page(s)||8|
|Published online||19 May 2015|
Numerical simulations of sheared magnetic lines at the solar null line⋆
Group of Astrophysics, University of Maria Curie-Skłodowska,
ul. Radziszewskiego 10,
2 Central (Pulkovo) Astronomical Observatory, Russian Academy of Sciences, 196140 St. Petersburg, Russia
Accepted: 26 February 2015
Aims. We perform numerical simulations of sheared magnetic lines at the magnetic null line configuration of two magnetic arcades that are settled in a gravitationally stratified and magnetically confined solar corona.
Methods. We developed a general analytical model of a 2.5D solar atmospheric structure. As a particular application of this model, we adopted it for the curved magnetic field lines with an inverted Y shape that compose the null line above two magnetic arcades, which are embedded in the solar atmosphere that is specified by the realistic temperature distribution. The physical system is described by 2.5D magnetohydrodynamic equations that are numerically solved by the FLASH code.
Results. The magnetic field line shearing, implemented about 200 km below the transition region, results in Alfvén and magnetoacoustic waves that are able to penetrate solar coronal regions above the magnetic null line. As a result of the coupling of these waves, partial reflection from the transition region and scattering from inhomogeneous regions the Alfvén waves experience fast attenuation on time scales comparable to their wave periods, and the physical system relaxes in time. The attenuation time grows with the large amplitude and characteristic growing time of the shearing.
Conclusions. By having chosen a different magnetic flux function, the analytical model we devised can be adopted to derive equilibrium conditions for a diversity of 2.5D magnetic structures in the solar atmosphere.
Key words: magnetohydrodynamics (MHD) / waves / Sun: corona / Sun: magnetic fields
Movie associated to Fig. 5 is available in electronic form at http://www.aanda.org
© ESO, 2015
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