A solar flare driven by thermal conduction observed in mid-infrared^⋆

¹ Centro de Rádio Astronomia e Astrofísica Mackenzie, Escola de Engenharia, Universidade Presbiteriana Mackenzie, Prédio 45 T, cobertura, R. da Consolação, 896–7o andar–Consolação, São Paulo, Brazil
e-mail: guigue@craam.mackenzie.br
² Instituto de Astronomía y Física del Espacio, CONICET-UBA, Ciudad Universitaria, Buenos Aires, Argentina
³ Facultad de Ciencias Exactas y Naturales, Universidad de Buenos Aires, 1428 Buenos Aires, Argentina
⁴ Facultad de Ciencias Exactas, Físicas y Naturales, Universidad Nacional de San Juan, Av. José Ignacio de la Roza Oeste 590, J5402DCS San Juan, Argentina
⁵ SUPA School of Physics and Astronomy, University of Glasgow, Glasgow G128QQ, UK
⁶ Center for Solar-Terrestrial Research, New Jersey Institute of Technology, Newark, NJ 07102, USA
⁷ Observatorio Astronómico Félix Aguilar (OAFA), Universidad Nacional de San Juan (UNSJ), San Juan J5413FHL, Argentina
⁸ LESIA, Observatoire de Paris, Université PSL, CNRS, Sorbonne Université, Université de Paris, 5 place Jules Janssen, 92195 Meudon, France
⁹ Laboratoire Cogitamus, 75005 Paris, France

Received: 5 August 2021
Accepted: 13 October 2021

Abstract

Context. The mid-infrared (mid-IR) range has been mostly unexplored for the investigation of solar flares. It is only recently that new mid-IR flare observations have begun opening a new window into the response and evolution of the solar chromosphere. These new observations have been mostly performed by the AR30T and BR30T telescopes that are operating in Argentina and Brazil, respectively.

Aims. We present the analysis of SOL2019-05-15T19:24, a GOES class C2.0 solar flare observed at 30 THz (10 μm) by the ground-based telescope AR30T. Our aim is to characterize the evolution of the flaring atmosphere and the energy transport mechanism in the context of mid-IR emission.

Methods. We performed a multi-wavelength analysis of the event by complementing the mid-IR data with diverse ground- and space-based data from the Solar Dynamics Observatory (SDO), the H-α Solar Telescope for Argentina, and the Expanded Owens Valley Solar Array (EOVSA). Our study includes the analysis of the magnetic field evolution of the flaring region and of the development of the flare.

Results. The mid-IR images from AR30T show two bright and compact flare sources that are spatially associated with the flare kernels observed in ultraviolet (UV) by SDO. We confirm that the temporal association between mid-IR and UV fluxes previously reported for strong flares is also observed for this small flare. The EOVSA microwave data revealed flare spectra consistent with thermal free-free emission, which lead us to dismiss the existence of a significant number of non-thermal electrons. We thus consider thermal conduction as the primary mechanism responsible for energy transport. Our estimates for the thermal conduction energy and total radiated energy fall within the same order of magnitude, reinforcing our conclusions.