Abstract
The study analyzes the millimeter emission of a solar flare on April 2, 2017, observed by the Bauman Moscow State Technical University telescope RT-7.5. Based on the flare atmosphere model proposed by Machado et al. (1980) we inferred the emission contribution function of the source and determined its main characteristics. The results show that the subterahertz emission is formed in a thin, chromospheric layer with a thickness of about 10 km with a plasma temperature of ~105 K. The proposed homogeneous model of the layer makes it possible to explain the observed spectral features. The obtained results suggest the chromospheric source heating with heat fluxes generated in the overlying flare areas.
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