Mapping the magnetic field in the solar corona through magnetoseismology

TL;DR

This paper demonstrates how magnetoseismology applied to pervasive transverse MHD waves observed with CoMP can produce detailed maps of the solar corona's magnetic field strength and direction, enhancing understanding of solar magnetism.

Contribution

It introduces a novel application of magnetoseismology to widespread propagating waves, enabling two-dimensional mapping of coronal magnetic fields from spectroscopic observations.

Findings

Mapped plasma density and wave phase speed in the corona.

Produced two-dimensional magnetic field strength and direction maps.

Compared magnetic and density variations with height in different solar regions.

Abstract

Magnetoseismology, a technique of magnetic field diagnostics based on observations of magnetohydrodynamic (MHD) waves, has been widely used to estimate the field strengths of oscillating structures in the solar corona. However, previously magnetoseismology was mostly applied to occasionally occurring oscillation events, providing an estimate of only the average field strength or one-dimensional distribution of field strength along an oscillating structure. This restriction could be eliminated if we apply magnetoseismology to the pervasive propagating transverse MHD waves discovered with the Coronal Multi-channel Polarimeter (CoMP). Using several CoMP observations of the Fe xiii 1074.7 nm and 1079.8 nm spectral lines, we obtained maps of the plasma density and wave phase speed in the corona, which allow us to map both the strength and direction of the coronal magnetic field in the plane of sky. We also examined distributions of the electron density and magnetic field strength, and compared their variations with height in the quiet Sun and active regions. Such measurements could provide critical information to advance our understanding of the Sun's magnetism and the magnetic coupling of the whole solar atmosphere.