Millimeter and X-Ray Emission from the 5 July 2012 Solar Flare

The 5 July 2012 solar flare SOL2012-07-05T11:44 (11:39 – 11:49 UT) with an increasing millimeter spectrum between 93 and 140 GHz is considered. We use space and ground-based observations in X-ray, extreme ultraviolet, microwave, and millimeter wave ranges obtained with the Reuven Ramaty High-Energy...

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Bibliographic Details
Published in:Solar physics 2018-03, Vol.293 (3), p.1-15, Article 50
Main Authors: Tsap, Y. T., Smirnova, V. V., Motorina, G. G., Morgachev, A. S., Kuznetsov, S. A., Nagnibeda, V. G., Ryzhov, V. S.
Format: Article
Language:English
Subjects:
Antennas
Astrophysics and Astroparticles
Atmospheric Sciences
Chromosphere
Electrons
Emission measurements
Energy
GOES satellites
Ground-based observation
Magnetic fields
Mathematical models
Millimeter waves
Observatories
Physics
Physics and Astronomy
Radio telescopes
Satellite observation
Solar activity
Solar corona
Solar energy
Solar flares
Solar observatories
Solar physics
Space Exploration and Astronautics
Space Sciences (including Extraterrestrial Physics
Telescopes
Thermal analysis
X ray spectra
X-ray emissions
X-rays
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Summary:The 5 July 2012 solar flare SOL2012-07-05T11:44 (11:39 – 11:49 UT) with an increasing millimeter spectrum between 93 and 140 GHz is considered. We use space and ground-based observations in X-ray, extreme ultraviolet, microwave, and millimeter wave ranges obtained with the Reuven Ramaty High-Energy Solar Spectroscopic Imager , Solar Dynamics Observatory (SDO), Geostationary Operational Environmental Satellite , Radio Solar Telescope Network , and Bauman Moscow State Technical University millimeter radio telescope RT-7.5. The main parameters of thermal and accelerated electrons were determined through X-ray spectral fitting assuming the homogeneous thermal source and thick-target model. From the data of the Atmospheric Imaging Assembly /SDO and differential-emission-measure calculations it is shown that the thermal coronal plasma gives a negligible contribution to the millimeter flare emission. Model calculations suggest that the observed increase of millimeter spectral flux with frequency is determined by gyrosynchrotron emission of high-energy ( ≳ 300  keV) electrons in the chromosphere. The consequences of the results are discussed in the light of the flare-energy-release mechanisms.
ISSN:0038-0938
1573-093X
DOI:10.1007/s11207-018-1269-6