A publicly available multi-observatory data set of an enhanced network patch from the Photosphere to Corona

TL;DR

This paper presents a comprehensive, publicly available multi-observatory dataset capturing chromospheric and coronal activity, enabling improved understanding of energy transfer and connectivity in the solar atmosphere.

Contribution

It introduces a new multi-wavelength, multi-instrument dataset of the solar atmosphere, including calibration, co-alignment, and initial analysis, focusing on a bipolar magnetic region near disk center.

Findings

Strong spatial correlation between Hydrogen-alpha spectral width and ALMA temperature data.

Observation of numerous transient brightenings across multiple wavelengths.

Identification of a 20-minute transient brightening with temperature evolution from cool to hot.

Abstract

New instruments sensitive to chromospheric radiation at X-ray, UV, Visible, IR, and sub-mm wavelengths have become available that significantly enhance our ability to understand the bi-directional flow of energy through the chromosphere. We describe the calibration, co-alignment, initial results, and public release of a new data set combining a large number of these instruments to obtain multi-wavelength photospheric, chromospheric, and coronal observations capable of improving our understanding of the connectivity between the photosphere and the corona via transient brightenings and wave signatures. The observations center on a bipolar region of enhanced network magnetic flux near disk center on SOL2017-03-17T14:00-17:00. The comprehensive data set provides one of the most complete views of chromospheric activity related to small scale brightenings in the corona and chromosphere to date. Our initial analysis shows strong spatial correspondence between the areas of broadest width of the Hydrogen-$\alpha$ spectral line and the hottest temperatures observed in ALMA Band 3 radio data, with a linear coefficient of $6.12\times 10^{-5}$\AA{}/K. The correspondence persists for the duration of co-temporal observations ($\approx 60$ minutes). Numerous transient brightenings were observed in multiple data series. We highlight a single, well observed transient brightening along a set of thin filamentary features with a duration of 20 minutes. The timing of the peak intensity transitions from the cooler (ALMA, 7000 K) to hotter (XRT, 3 MK) data series.