Stokes Profile Asymmetries in Solar Active Regions

摘要

Asymmetries in Stokes polarization spectral line profiles can be attributed to the existence of gradients in the velocity (and magnetic field) over the line-forming region. Models that solve the Stokes radiative transfer equations have incorporated both line-of-sight gradients and gradients perpendicular to the line of sight over the resolution element to produce the observed asymmetries. There have been only a few systematic studies of how these Stokes profile asymmetries vary across spatial structures and as a function of the amplitude of the velocity and magnetic fields, and very little statistical information is available.