Analytic approximate seismology of propagating MHD waves in the solar corona

Abstract

Observations show that propagating magnetohydrodynamic (MHD) waves are ubiquitous in the solar atmosphere. The technique of MHD seismology uses the wave observations combined with MHD wave theory to indirectly infer physical parameters of the solar atmospheric plasma and magnetic field. Here we present an analytical seismological inversion scheme for propagating MHD waves. This scheme uses in a consistent manner the observational information on wavelengths and damping lengths, along with observed values of periods or phase velocities, and is based on approximate asymptotic expressions for the theoretical values of wavelengths and damping lengths. The applicability of the inversion scheme is discussed and an example is given.

arXiv commentAccepted for publication in ApJ. arXiv admin note: text overlap with arXiv:0804.3877

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• Model comparison for the density structure across solar coronal waveguides
• Resonant absorption of surface sausage and surface kink modes under photospheric conditions
• Coronal loop physical parameters from the analysis of multiple observed transverse oscillations
• Magnetohydrodynamic Slow Mode with Drifting He${}^{++}$: Implications for Coronal Seismology and the Solar Wind
• The effect of flow on resonant absorption of slow MHD waves in magnetic flux tubes