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Title: AN IMAGING STUDY OF A COMPLEX SOLAR CORONAL RADIO ERUPTION

Abstract

Solar coronal radio bursts are enhanced radio emission excited by energetic electrons accelerated during solar eruptions. Studying these bursts is important for investigating the origin and physical mechanism of energetic particles and further diagnosing coronal parameters. Earlier studies suffered from a lack of simultaneous high-quality imaging data of the radio burst and the eruptive structure in the inner corona. Here we present a study on a complex solar radio eruption consisting of a type II burst and three reversely drifting type III bursts, using simultaneous EUV and radio imaging data. It is found that the type II burst is closely associated with a propagating and evolving CME-driven EUV shock structure, originated initially at the northern shock flank and later transferred to the top part of the shock. This source transfer is coincident with the presence of shock decay and enhancing signatures observed at the corresponding side of the EUV front. The electron energy accelerated by the shock at the flank is estimated to be ∼0.3 c by examining the imaging data of the fast-drifting herringbone structure of the type II burst. The reverse-drifting type III sources are found to be within the ejecta and correlated with a likely reconnection eventmore » therein. The implications for further observational studies and relevant space weather forecasting techniques are discussed.« less

Authors:
; ; ; ;  [1]
  1. Shandong Provincial Key Laboratory of Optical Astronomy and Solar-Terrestrial Environment, and Institute of Space Sciences, Shandong University, Weihai, Shandong 264209 (China)
Publication Date:
OSTI Identifier:
22654251
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astrophysical Journal Letters; Journal Volume: 827; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; COSMIC RADIO SOURCES; DECAY; EMISSION; EXTREME ULTRAVIOLET RADIATION; FORECASTING; MASS; PARTICLES; SOLAR CORONA; SOLAR RADIO BURSTS; SPACE; SUN; TAIL ELECTRONS

Citation Formats

Feng, S. W., Chen, Y., Song, H. Q., Wang, B., and Kong, X. L., E-mail: yaochen@sdu.edu.cn. AN IMAGING STUDY OF A COMPLEX SOLAR CORONAL RADIO ERUPTION. United States: N. p., 2016. Web. doi:10.3847/2041-8205/827/1/L9.
Feng, S. W., Chen, Y., Song, H. Q., Wang, B., & Kong, X. L., E-mail: yaochen@sdu.edu.cn. AN IMAGING STUDY OF A COMPLEX SOLAR CORONAL RADIO ERUPTION. United States. doi:10.3847/2041-8205/827/1/L9.
Feng, S. W., Chen, Y., Song, H. Q., Wang, B., and Kong, X. L., E-mail: yaochen@sdu.edu.cn. Wed . "AN IMAGING STUDY OF A COMPLEX SOLAR CORONAL RADIO ERUPTION". United States. doi:10.3847/2041-8205/827/1/L9.
@article{osti_22654251,
title = {AN IMAGING STUDY OF A COMPLEX SOLAR CORONAL RADIO ERUPTION},
author = {Feng, S. W. and Chen, Y. and Song, H. Q. and Wang, B. and Kong, X. L., E-mail: yaochen@sdu.edu.cn},
abstractNote = {Solar coronal radio bursts are enhanced radio emission excited by energetic electrons accelerated during solar eruptions. Studying these bursts is important for investigating the origin and physical mechanism of energetic particles and further diagnosing coronal parameters. Earlier studies suffered from a lack of simultaneous high-quality imaging data of the radio burst and the eruptive structure in the inner corona. Here we present a study on a complex solar radio eruption consisting of a type II burst and three reversely drifting type III bursts, using simultaneous EUV and radio imaging data. It is found that the type II burst is closely associated with a propagating and evolving CME-driven EUV shock structure, originated initially at the northern shock flank and later transferred to the top part of the shock. This source transfer is coincident with the presence of shock decay and enhancing signatures observed at the corresponding side of the EUV front. The electron energy accelerated by the shock at the flank is estimated to be ∼0.3 c by examining the imaging data of the fast-drifting herringbone structure of the type II burst. The reverse-drifting type III sources are found to be within the ejecta and correlated with a likely reconnection event therein. The implications for further observational studies and relevant space weather forecasting techniques are discussed.},
doi = {10.3847/2041-8205/827/1/L9},
journal = {Astrophysical Journal Letters},
number = 1,
volume = 827,
place = {United States},
year = {Wed Aug 10 00:00:00 EDT 2016},
month = {Wed Aug 10 00:00:00 EDT 2016}
}