Coronal loop physical parameters from the analysis of multiple observed transverse oscillations

Abstract

The analysis of quickly damped transverse oscillations of solar coronal loops using magneto-hydrodynamic seismology allow us to infer physical parameters that are difficult to measure otherwise. Under the assumption that such damped oscillations are due to the resonant conversion of global modes into Alfven oscillations of the tube surface, we carry out a global seismological analysis of a large set of coronal loops. A Bayesian hierarchical method is used to obtain distributions for coronal loop physical parameters by means of a global analysis of a large number of observations. The resulting distributions summarise global information and constitute data-favoured information that can be used for the inversion of individual events. The results strongly suggest that internal Alfven travel times along the loop are larger than 100 s and smaller than 540 s with 95% probability. Likewise, the density contrast between the loop interior and the surrounding is larger than 2.3 and below 6.9 with 95% probability.

9 pages, 6 figures, accepted for publication in A&A

References in corpus (4)

• Surface Alfven waves in solar flux tubes
• Analytic approximate seismology of transversely oscillating coronal loops
• 3D Extinction Mapping Using Hierarchical Bayesian Models
• Analytic approximate seismology of propagating MHD waves in the solar corona

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