Combining magneto-hydrostatic constraints with Stokes profiles inversions

II. Application to Hinode/SP observations

¹ Leibniz-Institut für Sonnenphysik, Schöneckstr. 6, 79110 Freiburg, Germany
e-mail: orrero@leibniz-kis.de
² Institute for Solar Physics, Department of Astronomy, Stockholm University, AlbaNova University Centre, 10691 Stockholm, Sweden
³ Instituto de Astrofísica de Canarias, Avd. Vía Láctea s/n, 38205 La Laguna, Spain
⁴ Departamento de Astrofísica, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain

Received: 17 November 2020
Accepted: 16 December 2020

Abstract

Context. Inversion techniques applied to the radiative transfer equation for polarized light are capable of inferring the physical parameters in the solar atmosphere (temperature T, magnetic field B, and line-of-sight velocity v_los) from observations of the Stokes vector (i.e., spectropolarimetric observations) in spectral lines. Inferences are usually performed in the (x, y, τ_c) domain, where τ_c refers to the optical-depth scale. Generally, their determination in the (x, y, z) volume is not possible due to the lack of a reliable estimation of the gas pressure, particularly in regions of the solar surface harboring strong magnetic fields.

Aims. We aim to develop a new inversion code capable of reliably inferring the physical parameters in the (x, y, z) domain.

Methods. We combine, in a self-consistent way, an inverse solver for the radiative transfer equation (Firtez-DZ) with a solver for the magneto-hydrostatic equilibrium, which derives realistic values of the gas pressure by taking the magnetic pressure and tension into account.

Results. We test the correct behavior of the newly developed code with spectropolarimetric observations of two sunspots recorded with the spectropolarimeter (SP) instrument on board the Hinode spacecraft, and we show how the physical parameters are inferred in the (x, y, z) domain, with the Wilson depression of the sunspots arising as a natural consequence of the force balance. In particular, our approach significantly improves upon previous determinations that were based on semiempirical models.

Conclusions. Our results open the door for the possibility of calculating reliable electric currents in three dimensions, j(x, y, z), in the solar photosphere. Further consistency checks would include a comparison with other methods that have recently been proposed and which achieve similar goals.