MHDWAVE

The computer code uses two-dimensional magnetohydrodynamic numerical models for a study of a spatial and temporal evolution of impulsively generated fast and slow sausage magnetoacoustic waves propagating along a waveguide (e.g., dense slab, Harris current sheet). These models also allow to study basic parameters of a nonpropagating entropy wave that occurred and stayed in situ of the initial perturbation. The wave signals computed in the numerical models are used for computations of the temporal and spatial wavelet spectra to estimate basic parameters of waveguides and their perturbations.

• The used 2D MHD models, initial conditions and equilibrium are described in models.lst
• Perturbations were selected to generate sausage magnetoacoustic waves pertub.lst

Waves propagating along a Dense slab and their wavelet spectra

• Temporal evolution of the magnetoacoustic waves: evol1.lst
Computed temporal evolution of physical parameters for the Dense slab (optional):
• mass density
• magnetic field total
• longitudinal magnetic field
• transverse magnetic field
• gas pressure
• current density
• plasma energy density
• plasma velocity
• Alfven speed
• sound speed
• flow velocity
• Wavelet methods, temporal & spatial wavelet spectra and their additional structures: spect1.lst
• Mutual interactions of propagating magnetoacoustic waves: mutual.lst

Waves propagating along the Harris current sheet and their wavelet spectra

• Temporal evolution of the magnetoacoustic waves: evol2.lst
Computed temporal evolution of physical parameters for the Harris current sheet (optional):
• mass density
• magnetic field total
• longitudinal magnetic field
• transverse magnetic field
• gas pressure
• current density
• plasma energy density
• plasma velocity
• Alfven speed
• sound speed
• flow velocity
• Wavelet methods, temporal wavelet spectra and their additional structures: spect2.lst

References:

• Mészárosová, H., et al.: 2009, Astron. Astrophys. 502, L13
• Mészárosová, H., et al.: 2009, Astrophysical Journal 697, L108
• Mészárosová, H., et al.: 2011, Solar Phys 273, 393
• Mészárosová, H., et al.: 2013, Solar Phys 283, 473
• Mészárosová, H., et al.: 2016, Astron. Astrophys. 593, A80
• Mészárosová, H., and P. Gömöry: 2020, Astron. Astrophys. 643, A140

The code is written in Fortran 90 and IDL.

Program is available upon request.

Last update: 2.10.2022