High frequency waves in the corona due to null points

Abstract

This work aims to understand the behavior of non-linear waves in the vicinity of a coronal null point. In previous works we have showed that high frequency waves are generated in such magnetic configuration. This paper studies those waves in detail in order to provide a plausible explanation of their generation. We demonstrate that slow magneto-acoustic shock waves generated in the chromosphere propagate through the null point and produce a train of secondary shocks that escape along the field lines. A particular combination of the shock wave speeds generates waves at a frequency of 80 mHz. We speculate that this frequency may be sensitive to the atmospheric parameters in the corona and therefore can be used to probe the structure of this solar layer.

References in corpus (4)

• Nonlinear Fast Magnetoacoustic Wave Propagation in the Neighbourhood of a 2D magnetic X-point: Oscillatory Reconnection
• MHD wave propagation in the neighbourhood of a two-dimensional null point
• MHD wave propagation from the sub-photosphere to the corona in an arcade-shaped magnetic field with a null point
• Simulated interaction of MHD shock waves with a complex network-like region

Cited by in corpus (9)

• Two-fluid simulations of waves in the solar chromosphere II. Propagation and damping of fast magneto-acoustic waves and shocks
• Generation mechanisms of quasi-parallel and quasi-circular flare ribbons in a confined flare
• Oscillatory Reconnection of a 2D X-point in a hot coronal plasma
• Fast-to-Alfvén mode conversion mediated by Hall current. II Application to the solar atmosphere
• High-frequency spicule oscillations generated via mode conversion
• Direct Imaging of Magnetohydrodynamic Wave Mode Conversion Near a 3D Null Point on the Sun
• The formation and dissipation of current sheets and shocks due to compressive waves in a stratified atmosphere containing a magnetic null
• Extreme-ultraviolet (EUV) observables of simulated plasmoid-mediated reconnection in the solar corona
• The independence of oscillatory reconnection periodicity from the initial pulse