Case study on the identification and classification of small-scale flow patterns in flaring active region

¹ Centre for Mathematical Plasma Astrophysics/Department of Mathematics, Celestijnenlaan 200B, 3001 Leuven, Belgium
² Centre for Computational Helio Studies, Ilia State University, Cholokashvili Ave. 3/5, 0162 Tbilisi, Georgia
e-mail: bidzina.shergelashvili@iliauni.edu.ge
³ Space Research Institute, Austrian Academy of Sciences, Schmiedlstrasse 6, 8042 Graz, Austria
e-mail: bidzina.shergelashvili@oeaw.ac.at
⁴ Evgeni Kharadze Georgian National Astrophysical Observatory, Abastumani, 0301 Adigeni Municipality, Georgia
⁵ Department of Statistics and Actuarial Science, Stellenbosch University, Victoria Street, 7600 Stellenbosch, South Africa
⁶ Institute of Physics, University of Maria Curie-Skłodowska, 20-031 Lublin, Poland
⁷ Lomonosov Moscow State University, Skobeltsyn Institute of Nuclear Physics (MSU SINP) Leninskie Gory, 119992 Moscow, Russia
⁸ Institute of Astronomy, Russian Academy of Sciences, Moscow 119017, Russia

Received: 10 July 2020
Accepted: 13 October 2020

Abstract

Context. We propose a novel methodology to identity flows in the solar atmosphere and classify their velocities as either supersonic, subsonic, or sonic.

Aims. The proposed methodology consists of three parts. First, an algorithm is applied to the Solar Dynamics Observatory (SDO) image data to locate and track flows, resulting in the trajectory of each flow over time. Thereafter, the differential emission measure inversion method is applied to six Atmospheric Imaging Assembly (AIA) channels along the trajectory of each flow in order to estimate its background temperature and sound speed. Finally, we classify each flow as supersonic, subsonic, or sonic by performing simultaneous hypothesis tests on whether the velocity bounds of the flow are larger, smaller, or equal to the background sound speed.

Methods. The proposed methodology was applied to the SDO image data from the 171 Å spectral line for the date 6 March 2012 from 12:22:00 to 12:35:00 and again for the date 9 March 2012 from 03:00:00 to 03:24:00. Eighteen plasma flows were detected, 11 of which were classified as supersonic, 3 as subsonic, and 3 as sonic at a 70% level of significance. Out of all these cases, 2 flows cannot be strictly ascribed to one of the respective categories as they change from the subsonic state to supersonic and vice versa. We labeled them as a subclass of transonic flows.

Results. The proposed methodology provides an automatic and scalable solution to identify small-scale flows and to classify their velocities as either supersonic, subsonic, or sonic. It can be used to characterize the physical properties of the solar atmosphere.

Conclusions. We identified and classified small-scale flow patterns in flaring loops. The results show that the flows can be classified into four classes: sub-, super-, trans-sonic, and sonic. The flows occur in the complex structure of the active region magnetic loops. The detected flows from AIA images can be analyzed in combination with the other high-resolution observational data, such as Hi-C 2.1 data, and be used for the development of theories describing the physical conditions responsible for the formation of flow patterns.