Analytic approximate seismology of propagating MHD waves in the solar corona

TL;DR

This paper introduces an analytical seismological inversion method for propagating MHD waves in the solar corona, enabling indirect inference of plasma and magnetic field parameters using wave observations and asymptotic theory.

Contribution

It presents a new analytical inversion scheme that combines observational data with approximate asymptotic expressions for MHD wave properties.

Findings

The inversion scheme effectively estimates physical parameters from wave data.

It demonstrates applicability through an example analysis.

The method enhances understanding of solar atmospheric plasma and magnetic fields.

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.