2017/10/23 by K. Murawski, Pradeep Kayshap, P. Kayshap +7 · 28 citations
Physics and Astronomy · #Astro and Planetary Science #Astronomy #Astrophysics #Chromosphere #Dipole #Energy flux #Flux (metallurgy) #Flux tube #Ionosphere and magnetosphere dynamics #Magnetic field #Magnetic flux #Magnetohydrodynamic drive #Magnetohydrodynamics #Mechanics #Photosphere #Physics #Plasma #Solar and Space Plasma Dynamics #Vortex #astro-ph.SR
paper · pdf · doi:10.1093/mnras/stx2763
published in Monthly Notices of the Royal Astronomical Society 474(1), 77-87 (Oxford University Press)
arxiv created 2017/10/23 · openalex publication_date 2017/10/23 · arxiv updated 2017/12/13 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We perform numerical simulations of impulsively generated magnetic swirls in an isolated flux tube that 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 are 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 a 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 fulfil 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.