Observed damping of the slow magnetoacoustic mode

Abstract

Spectroscopic and stereoscopic imaging observations of slow magnetoacoustic wave propagation within a coronal loop are investigated to determine the decay length scale of the slow magnetoacoustic mode in three dimensions and the density profile within the loop system. The slow wave is found to have an e-folding decay length scale of $20,000_{-3000}^{+4000}$km with a uniform density profile along the loop base. These observations place quantitive constraints on the modelling of wave propagation within coronal loops. Theoretical forward modelling suggests that magnetic field line divergence is the dominant damping factor and thermal conduction is insufficient, given the observed parameters of the coronal loop temperature, density and wave mode period.

Accepted for publication in ApJ

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• Observations of Dissipation of Slow Magneto-acoustic Waves in a Polar Coronal Hole
• Spectroscopic Observations of Propagating Disturbances in a Polar Coronal Hole: Evidence of Slow Magneto-acoustic Waves
• Dispersion of Slow Magnetoacoustic Waves in the Active Region Fan Loops Introduced by Thermal Misbalance
• Magnetoacoustic Wave Energy Dissipation in the Atmosphere of Solar Pores
• Resonant absorption in expanding coronal magnetic flux tubes with uniform density
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• Phase speed and frequency-dependent damping of longitudinal intensity oscillations in coronal loop structures observed with AIA/SDO
• First detection of acoustic-like flux in the middle solar corona
• The Temperature-dependent Damping of Propagating Slow Magnetoacoustic Waves