Time delays in the nonthermal radiation of solar flares according to observations of the CORONAS-F satellite

In 2001–2003, the X-ray and microwave observations of ten solar flares of M- and X-classes were carried out by the CORONAS-F orbital station, the RSTN Sun service, and Nobeyama radio polarimeters. Based on these observations, a correlation analysis of time profiles of nonthermal radiation was perfor...

Full description

Saved in:
Bibliographic Details
Published in:Cosmic research 2016-07, Vol.54 (4), p.285-289
Main Authors: Tsap, Yu. T., Stepanov, A. V., Kashapova, L. K., Myagkova, I. N., Bogomolov, A. V., Kopylova, Yu. G., Goldvarg, T. B.
Format: Article
Language:English
Subjects:
Arches
Astronomy
Astrophysics and Astroparticles
Astrophysics and Cosmology
Corona
Correlation analysis
Energetic particles
Flares
Indication
Magnetic mirrors
Microwave radiation
Microwaves
Nonthermal radiation
Orbitals
Physics
Physics and Astronomy
Pitch (inclination)
Polarimeters
Radiation
Satellite observation
Solar corona
Solar flares
Space Exploration and Astronautics
Space Sciences (including Extraterrestrial Physics
Time delay
X-rays
Citations: Items that this one cites
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary:In 2001–2003, the X-ray and microwave observations of ten solar flares of M- and X-classes were carried out by the CORONAS-F orbital station, the RSTN Sun service, and Nobeyama radio polarimeters. Based on these observations, a correlation analysis of time profiles of nonthermal radiation was performed. On average, hard X-ray radiation outstrips the microwave radiation in 9 events, i.e., time delays are positive. The appearance of negative delays is associated with effective scattering of accelerated electrons in pitch angles, where the length of the free path of a particle is less than the half-length of a flare loop. The additional indications are obtained in favor of the need to account for the effect of magnetic mirrors on the dynamics of energetic particles in the coronal arches.
ISSN:0010-9525
1608-3075
DOI:10.1134/S0010952516040067