Modeling the effects of a lightbridge on oscillations in a solar pore

Abstract

Solar pores are ideal magnetic structures for wave propagation and transport of energy radially-outwards across the upper layers of the solar atmosphere. We aim to model the excitation and propagation of magnetohydrodynamic waves in a pore with a lightbridge modelled as two interacting magnetic flux tubes separated by a thin, weaker field, layer. We solve the three-dimensional MHD equations numerically and calculate the circulation as a measure of net torsional motion. We find that the interaction between flux tubes results in the natural excitation of propagating torsional Alfvén waves, but find no torsional waves in the model with a single flux tube. The torsional Alfvén waves propagate with wave speeds matching the local Alfvén speed where wave amplitude peaks.

References in corpus (18)

• Multiwavelength studies of MHD waves in the solar chromosphere: An overview of recent results
• Nonlinear Instability of kink oscillations due to shear motions
• Magnetic Structure of Sunspots
• Fine strand-like structure in the solar corona from MHD transverse oscillations
• Resonant absorption in complicated plasma configurations: applications to multi-stranded coronal loop oscillations
• Observations of sausage modes in magnetic pores
• Light Bridge in a Developing Active Region. I. Observation of Light Bridge and its Dynamic Activity Phenomena
• Generation of Magnetohydrodynamic Waves in Low Solar Atmospheric Flux Tubes by Photospheric Motions
• Three-dimensional structure of a sunspot light bridge
• Dynamics of the solar atmosphere above a pore with a light bridge
• Detection of the strongest magnetic field in a sunspot light bridge
• Decay of a simulated mixed-polarity magnetic field in the solar surface layers
• The instability and non-existence of multi-stranded loops, when driven by transverse waves
• Magnetoacoustic Wave Energy Dissipation in the Atmosphere of Solar Pores
• A novel approach to identify resonant MHD wave modes in solar pores and sunspot umbrae: $B-\omega$ analysis
• Oscillations In The Line-of-Sight Magnetic Field Strength In A Pore Observed By The GREGOR Infrared Spectrograph (GRIS)
• Damped transverse oscillations of interacting coronal loops
• Atmosphere above a large solar pore