Radio Measurements of the Magnetic Field in the Solar Chromosphere and the Corona

摘要: The structure of the upper solar atmosphere, on all observable scales, is intimately governed by magnetic field. same holds for a variety phenomena that constitute activity, from tiny transient brightening to huge Coronal Mass Ejections. Due inherent difficulties in measuring field effects atoms (Zeeman and Hanle effects) corona, radio methods sensitive electrons are primary importance obtaining quantitative information about its In this review we explore these point out their advantages limitations. After brief presentation magneto-ionic theory wave propagation cold, collisionless plasmas, discuss how affects emission produced incoherent mechanisms (free-free, gyroresonance gyrosynchrotron processes) give examples measurements filed parameters quiet sun, active regions CMEs. We proceed discussing inversion sense circular polarization can be used measure above regions. Subsequently pass coherent present results fiber bursts, zebra patterns type II burst emission. close with discussion variation field, deduced measurement, low corona up  10 radii some thoughts future work.