Inversion of physical parameters in solar atmospheric seismology

Abstract

Magnetohydrodynamic (MHD) wave activity is ubiquitous in the solar atmosphere. MHD seismology aims to determine difficult to measure physical parameters in solar atmospheric magnetic and plasma structures by a combination of observed and theoretical properties of MHD waves and oscillations. This technique, similar to seismology or helio-seismology, demands the solution of two problems. The direct problem involves the computation of wave properties of given theoretical models. The inverse problem implies the calculation of unknown physical parameters, by means of a comparison of observed and theoretical wave properties. Solar atmospheric seismology has been successfully applied to different structures such as coronal loops, prominence fine structures, spicules, or jets. However, it is still in its infancy. Far more is there to come. We present an overview of recent results, with particular emphasis in the inversion procedure.

10 pages, 3 figures, review paper to appear in Astrophysics and Space Science Proceedings

References in corpus (4)

• Analytic approximate seismology of transversely oscillating coronal loops
• Transverse oscillations of flowing prominence threads observed with Hinode
• Damping of Fast Magnetohydrodynamic Oscillations in Quiescent Filament Threads
• Seismology of Standing Kink Oscillations of Solar Prominence Fine Structures

Cited by in corpus (7)

• Wave Heating of the Solar Atmosphere
• Bayesian Coronal Seismology
• Model comparison for the density structure across solar coronal waveguides
• Novel data analysis techniques in coronal seismology
• Determination of the cross-field density structuring in coronal waveguides using the damping of transverse waves
• Simultaneous longitudinal and transverse oscillations in filament threads after a failed eruption
• Global Coronal Magnetic Field Estimation Using Bayesian Inference