Evolution of solar magnetic tubes and its manifestation in Stokes parameters

TL;DR

This paper models the formation, evolution, and decay of small-scale solar magnetic tubes, analyzing their signatures in Stokes profiles to understand magnetic element dynamics on the Sun.

Contribution

It introduces a two-dimensional nonstationary magnetogranulation model to simulate magnetic tube evolution and their spectral signatures in the Fe I infrared line.

Findings

Convective collapse causes redshifts and Zeeman splitting in Stokes profiles.

Magnetic dissipation results in blueshifts and decreased magnetic field strength.

Detectable signatures of magnetic element evolution require high-resolution observations.

Abstract

Basic scenarios and mechanisms for the formation and decay of small-scale magnetic elements and their manifestation in synthesized Stokes profiles of the Fe I 15648.5 A infrared line are considered in the context of two-dimensional modeling of nonstationary magnetogranulation on the Sun. The stage of convective collapse is characterized by large redshifts in the V profiles accompanied by complete Zeeman splitting of the I profiles. This is due to intense downward flows of material, which facilitates the concentration of longitudinal field with an amplitude of about several kG in the tube. The dissipation of strong magnetic structures is characterized by blueshifts in the Stokes profiles, which result from upward fluxes that decrease the magnetic field in the tube. Typical signatures during key stages in the evolution of compact magnetic elements should be detectable via observations with sufficiently high spatial and temporal resolution.