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Magnetic swirls and associated fast magnetoacoustic kink waves in a solar chromospheric flux tube  

Błażej Kuźma   Submitted: 2017-10-24 04:22

We perform numerical simulations of impulsively generated magnetic swirls in an isolated flux tube which is rooted in the solar photosphere. These swirls are triggered by an initial pulse in a horizontal component of the velocity. The initial pulse is launched either: (a) centrally, within the localized magnetic flux tube; or (b) off-central, in the ambient medium. The evolution and dynamics of the flux tube is described by three-dimensional, ideal magnetohydrodynamic equations. These equations are numerically solved to reveal that in case (a) dipole-like swirls associated with the fast magnetoacoustic kink and m=1 Alfvén waves are generated. In case (b), the fast magnetoacoustic kink and m=0 Alfvén modes are excited. In both these cases, the excited fast magnetoacoustic kink and Alfvén waves consist of similar flow pattern and magnetic shells are also generated with clockwise and counter-clockwise rotating plasma within them, which can be the proxy of dipole-shaped chromospheric swirls. The complex dynamics of vortices and wave perturbations reveals the channelling of sufficient amount of energy to fulfill energy losses in the chromosphere (~ 104 W m-1) and in the corona (~ 102 W m-1). Some of these numerical findings are reminiscent of signatures in recent observational data.

Authors: K. Murawski, P. Kayshap, A. K. Srivastava, D. J. Pascoe, P. Jelínek, B. Kuźma, V. Fedun
Projects: None

Publication Status: Mon. Not. R. Astron. Soc. (accepted)
Last Modified: 2017-10-24 11:57
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Numerical simulations of solar spicules: Adiabatic and non-adiabatic studies  

Błażej Kuźma   Submitted: 2016-10-03 03:56

Aims. We aim to study the formation and evolution of solar spicules using numerical simulations of vertical velocity pulse launched from upper chromosphere. Methods. With the use of the PLUTO code we numerically solve adiabatic and non-adiabatic magnetohydrodynamic (MHD) equations in 2D cylindrical geometry. We follow the evolution of spicules triggered by pulses in a vertical component of velocity in the upper chromosphere. Then we compare the results obtained with and without non-adiabatic terms in the MHD equations. Results. Our numerical results reveal that the velocity pulse is steepened into a shock which propagates upwards into the corona.The chromospheric cold and dense plasma follows the shock and rises into the corona with the mean speed of 20-25 km s-1. The nonlinear wake behind the pulse in the stratified atmosphere leads to quasi-periodic rebound shocks, which lead to quasi-periodic rising of chromospheric plasma into the corona with the period close to the acoustic cut-off period of the chromosphere. We found that the effect of non-adiabatic terms on spicule evolution is minor; the general properties of spicules such as their heights and rising-time remain slightly affected by these terms. Conclusions. In the framework of the axisymmetric model we devised, we show that the solar spicules can be triggered by the vertical velocity pulses and the thermal conduction and radiative cooling terms do not exert any significant influence on the dynamics of these spicules.

Authors: B. Kuźma , K. Murawski, T.V. Zaqarashvili, P. Konkol, and A. Mignone
Projects: None

Publication Status: accepted
Last Modified: 2016-10-03 12:30
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Magnetic swirls and associated fast magnetoacoustic kink waves in a solar chromospheric flux tube
Numerical simulations of solar spicules: Adiabatic and non-adiabatic studies

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