Combining magnetohydrostatic constraints with Stokes profiles inversions

Inversion codes for the polarized radiative transfer equation, when applied to spectropolarimetric observations (i.e., Stokes vector) in spectral lines, can be used to infer the temperature T, line-of-sight velocity v(los), and magnetic field B as a function of the continuum optical-depth tau(c). However, they do not directly provide the gas pressure P-g or density rho.

In order to obtain these latter parameters, inversion codes rely instead on the assumption of hydrostatic equilibrium (HE) in addition to the equation of state (EOS). Unfortunately, the assumption of HE is rather unrealistic across magnetic field lines, causing estimations of P-g and rho to be unreliable. This is because the role of the Lorentz force, among other factors, is neglected.