Morphology and dynamics of photospheric and chromospheric magnetic fields

TL;DR

This study investigates the morphology and dynamics of magnetic and non-magnetic regions in the solar fluctosphere using joint observations, revealing stable magnetic flux elements and similarities to numerical simulations.

Contribution

It provides new observational insights into the structure and behavior of magnetic fields in the solar fluctosphere, linking observations with simulations.

Findings

Non-magnetic regions show intensity structures similar to simulations.

Magnetic flux elements in the network are stable.

Challenges exist in deriving magnetic field vectors from observations.

Abstract

We use joint observations obtained with the Hinode space observatory and the Interferometric Bidimensional Spectrometer (IBIS) installed at the DST of the NSO/SP to investigate the morphology and dynamics of (a) non-magnetic and (b) magnetic regions in the fluctosphere. In inter-network regions with no significant magnetic flux contributions above the detection limit of IBIS, we find intensity structures with similar characteristics as those seen in numerical simulations by Wedemeyer-B\"ohm (2008). The magnetic flux elements in the network are stable and seem to resemble the spatially extended counterparts to the underlying photospheric magnetic elements. We will explain some of the difficulties in deriving the magnetic field vector from observations of the fluctosphere.