Insights into Chromospheric Large-Scale Flows using Nobeyama 17 GHz Radio Observations I. The Differential Rotation Profile

TL;DR

This study uses 17 GHz radio observations over two solar cycles to analyze the differential rotation profile of the upper chromosphere, revealing faster rotation than the photosphere and supporting height-dependent rotational dynamics.

Contribution

It introduces a tracer-independent, automated image correlation method applied to radio data to characterize chromospheric rotation, providing new insights into solar atmospheric dynamics.

Findings

Upper chromosphere rotates faster than the photosphere at all latitudes.

The latitudinal rotation profile of the chromosphere is relatively flatter.

A weak anti-correlation exists between equatorial rotation rate and solar activity.

Abstract

Although the differential rotation rate on the solar surface has long been studied using optical and extreme ultraviolet (EUV) observations, associating these measurements to specific atmospheric heights remains challenging due to the temperature-dependent emission of tracers observed in EUV wavelengths. Radio observations, being primarily influenced by coherent plasma processes and/or thermal bremsstrahlung, offer a more height-stable diagnostic and thus provide an independent means to test and validate rotational trends observed at other EUV wavelengths. We aim to characterize the differential rotation profile of the upper chromosphere using cleaned solar full-disc 17 GHz radio imaging from the Nobeyama Radioheliograph (NoRH), spanning a little over two solar cycles (1992 - 2020). A tracer-independent method based on automated image correlation was employed on daily full-disc 17 GHz radio maps. Our results suggest that the upper chromosphere rotates significantly faster than the photosphere at all latitudes, with a relatively flatter latitudinal profile. A very weak anti-correlation between the equatorial rotation rate and solar activity is also observed. Our findings reaffirm the potential of radio observations to probe the dynamics of the solar chromosphere with reduced height ambiguity. The overlap of the equatorial rotation rate found in this study with that for $304$ {\AA} in the EUV regime lends additional support to the view that the equatorial rotation rates increase with height above the photosphere. Future coordinated studies at wavelengths with better-constrained height formation will be crucial for further understanding the complex dynamics of the solar atmosphere.