Mapping the magnetic field in the solar corona through magnetoseismology

Zihao Yang, Hui Tian, Steven Tomczyk, Richard Morton, Xianyong Bai, Tanmoy Samanta, Yajie Chen

Research output: Contribution to journalArticlepeer-review

4 Citations (Scopus)

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.
Original languageEnglish
Pages (from-to)2357-2368
Number of pages12
JournalScience China Technological Sciences
Volume63
Issue number11
Early online date28 Aug 2020
DOIs
Publication statusPublished - 1 Nov 2020

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