Magneto-seismology of solar atmospheric loops by means of longitudinal oscillations

TL;DR

This paper advances solar magneto-seismology by developing MHD wave theory to infer magnetic and density structures in coronal loops through observed slow magnetoacoustic oscillations.

Contribution

It introduces a refined theoretical framework linking observed wave frequencies to the magnetic and density profiles in solar coronal loops.

Findings

Theoretical model relates wave frequencies to loop properties.

Application to observations demonstrates practical utility.

Enhanced understanding of solar atmospheric structure.

Abstract

There is increasingly strong observational evidence that slow magnetoacoustic modes arise in the solar atmosphere. Solar magneto-seismology is a novel tool to derive otherwise directly un-measurable properties of the solar atmosphere when magnetohydrodynamic (MHD) wave theory is compared to wave observations. Here, MHD wave theory is further developed illustrating how information about the magnetic and density structure along coronal loops can be determined by measuring the frequencies of the slow MHD oscillations. The application to observations of slow magnetoacoustic waves in coronal loops is discused.