Exploring the variation in the dynamic rotation profile of the hotter solar atmosphere using mutliwavelength data

TL;DR

This study analyzes 13 years of multiwavelength solar data to unify the understanding of the solar atmosphere's rotational profile, revealing variations with height and magnetic structure influences.

Contribution

It provides a comprehensive, multi-thermal analysis of the solar atmosphere's rotation, reconciling previous contradictory results using extensive observational data.

Findings

The solar atmosphere rotates up to 4.18% faster at the equator than the photosphere.

The differential rotation is less pronounced in the higher atmospheric layers.

Magnetic field structures influence the rotational profile, as suggested by comparisons with helioseismology data.

Abstract

The global rotational profile of the solar atmosphere and its variation at different layers, although crucial for a comprehensive understanding of the dynamics of the solar magnetic field, has been a subject to contradictory results throughout the past century. In this study, we thereby unify the results for different parts of the multi-thermal Solar atmosphere by utilizing 13 years of data in 7 wavelength channels of the Atmospheric Imaging Assembly (AIA) atop the Solar Dynamic Observatory (SDO). Using the method of image correlation, we find that the solar atmosphere exhibits a rotational profile that is up to 4.18% and 1.92% faster at the equator and comparatively less differential than that of the photosphere, as derived from Doppler measurements and sunspots, respectively and exhibits variation at different respective heights. Additionally, we find results suggestive of the role played by the rooting of different magnetic field structures on a comparison with helioseismology data.