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We present a Bayesian seismology inversion technique for propagatingmagnetohydrodynamic (MHD) transverse waves observed in coronal waveguides. Thetechnique uses theoretical predictions for the spatial damping of propagatingkink waves in transversely inhomogeneous coronal waveguides. It combines waveamplitude damping length scales along the waveguide with theoretical resultsfor resonantly damped propagating kink waves to infer the plasma densityvariation across the oscillating structures. Provided the spatial dependence ofthe velocity amplitude along the propagation direction is measured and theexistence of two different damping regimes is identified, the technique wouldenable us to fully constrain the transverse density structuring, providingestimates for the density contrast and its transverse inhomogeneity lengthscale.

Determination of Transverse Density Structuring from Propagating MHD Waves in the Solar Atmosphere