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Modeling of the solar flare chromosphere and sub-THz radiation with FLARIX and RADYN

Published online by Cambridge University Press:  23 December 2024

Galina G. Motorina Open the ORCID record for Galina G. Motorina [Opens in a new window] ,
Yuriy T. Tsap Open the ORCID record for Yuriy T. Tsap [Opens in a new window] ,
Jana Kašparová ,
Victoria V. Smirnova Open the ORCID record for Victoria V. Smirnova [Opens in a new window] ,
Alexander S. Morgachev  and
Miroslav Bárta
Galina G. Motorina*
Affiliation:
Central Astronomical Observatory at Pulkovo of Russian Academy of Sciences, St. Petersburg, 196140, Russia Space Research Institute of Russian Academy of Sciences, Moscow, 117997, Russia Astronomical Institute of the Czech Academy of Sciences, 251 65 Ondřejov, Czech Republic,
Yuriy T. Tsap
Affiliation:
Crimen Astrophysical Observatory, Nauchny, 298409
Jana Kašparová
Affiliation:
Astronomical Institute of the Czech Academy of Sciences, 251 65 Ondřejov, Czech Republic,
Victoria V. Smirnova
Affiliation:
Crimen Astrophysical Observatory, Nauchny, 298409
Alexander S. Morgachev
Affiliation:
Central Astronomical Observatory at Pulkovo of Russian Academy of Sciences, St. Petersburg, 196140, Russia
Miroslav Bárta
Affiliation:
Astronomical Institute of the Czech Academy of Sciences, 251 65 Ondřejov, Czech Republic,
*
email: [email protected]
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Abstract

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The origin of the sub-terahertz (sub-THz) component of radio emission from solar flares, which is characterized by the increase flux with frequency in the 100-400 GHz range, is considered. On the basis of equations of 1D non-LTE radiation hydrodynamics we simulated the altitude distribution of the plasma density and temperature inside the flare loop caused by the interaction of non-stationary beam of accelerated electrons in the form of a triangular pulse with the chromospheric plasma. The FLARIX numerical code was used to calculate the dynamics of the flare plasma parameters at different heights which are compared with the RADYN numerical code. We found that the characteristic heights of the formation of sub-THz emission vary over a wide range with time for both codes. The main contribution to the sub-THz emission comes from the chromospheric and transition region plasma with temperatures of 104–105K.

Keywords

Sun: Flares - Sun: X-raysEUVRadio emissionsub-THz emission
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 19 , Symposium S365: Dynamics of Solar and Stellar Convection Zones and Atmospheres , December 2023 , pp. 420 - 425
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

Footnotes

†

Most of the presented contribution was finished before February 2022

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