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Title: AN ERUPTIVE HOT-CHANNEL STRUCTURE OBSERVED AT METRIC WAVELENGTH AS A MOVING TYPE-IV SOLAR RADIO BURST

Abstract

Hot-channel (HC) structure, observed in the high-temperature passbands of the Atmospheric Imaging Assembly/ Solar Dynamic Observatory , is regarded as one candidate of coronal flux rope that is an essential element of solar eruptions. Here, we present the first radio imaging study of an HC structure in the metric wavelength. The associated radio emission manifests as a moving type-IV (t-IVm) burst. We show that the radio sources co-move outward with the HC, indicating that the t-IV emitting energetic electrons are efficiently trapped within the structure. The t-IV sources at different frequencies present no considerable spatial dispersion during the early stage of the event, while the sources spread gradually along the eruptive HC structure at later stage with significant spatial dispersion. The t-IV bursts are characterized by a relatively high brightness temperature (∼10{sup 7}–10{sup 9} K), a moderate polarization, and a spectral shape that evolves considerably with time. This study demonstrates the possibility of imaging the eruptive HC structure at the metric wavelength and provides strong constraints on the t-IV emission mechanism, which, if understood, can be used to diagnose the essential parameters of the eruptive structure.

Authors:
; ; ; ; ; ;  [1];  [2]
  1. Institute of Space Sciences, Shandong University, Weihai, Shandong 264209 (China)
  2. College of Science, China University of Petroleum, Qingdao 266580 (China)
Publication Date:
OSTI Identifier:
22654207
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal Letters
Additional Journal Information:
Journal Volume: 830; Journal Issue: 1; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 2041-8205
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BRIGHTNESS; DISPERSIONS; EMISSION; HOT CHANNEL; LIMITING VALUES; MASS; METRICS; POLARIZATION; SOLAR RADIO BURSTS; SUN; TAIL ELECTRONS; TRAPPING; WAVELENGTHS

Citation Formats

Vasanth, V., Chen, Yao, Feng, Shiwei, Du, Guohui, Song, Hongqiang, Kong, Xiangliang, Wang, Bing, and Ma, Suli. AN ERUPTIVE HOT-CHANNEL STRUCTURE OBSERVED AT METRIC WAVELENGTH AS A MOVING TYPE-IV SOLAR RADIO BURST. United States: N. p., 2016. Web. doi:10.3847/2041-8205/830/1/L2.
Vasanth, V., Chen, Yao, Feng, Shiwei, Du, Guohui, Song, Hongqiang, Kong, Xiangliang, Wang, Bing, & Ma, Suli. AN ERUPTIVE HOT-CHANNEL STRUCTURE OBSERVED AT METRIC WAVELENGTH AS A MOVING TYPE-IV SOLAR RADIO BURST. United States. https://doi.org/10.3847/2041-8205/830/1/L2
Vasanth, V., Chen, Yao, Feng, Shiwei, Du, Guohui, Song, Hongqiang, Kong, Xiangliang, Wang, Bing, and Ma, Suli. 2016. "AN ERUPTIVE HOT-CHANNEL STRUCTURE OBSERVED AT METRIC WAVELENGTH AS A MOVING TYPE-IV SOLAR RADIO BURST". United States. https://doi.org/10.3847/2041-8205/830/1/L2.
@article{osti_22654207,
title = {AN ERUPTIVE HOT-CHANNEL STRUCTURE OBSERVED AT METRIC WAVELENGTH AS A MOVING TYPE-IV SOLAR RADIO BURST},
author = {Vasanth, V. and Chen, Yao and Feng, Shiwei and Du, Guohui and Song, Hongqiang and Kong, Xiangliang and Wang, Bing and Ma, Suli},
abstractNote = {Hot-channel (HC) structure, observed in the high-temperature passbands of the Atmospheric Imaging Assembly/ Solar Dynamic Observatory , is regarded as one candidate of coronal flux rope that is an essential element of solar eruptions. Here, we present the first radio imaging study of an HC structure in the metric wavelength. The associated radio emission manifests as a moving type-IV (t-IVm) burst. We show that the radio sources co-move outward with the HC, indicating that the t-IV emitting energetic electrons are efficiently trapped within the structure. The t-IV sources at different frequencies present no considerable spatial dispersion during the early stage of the event, while the sources spread gradually along the eruptive HC structure at later stage with significant spatial dispersion. The t-IV bursts are characterized by a relatively high brightness temperature (∼10{sup 7}–10{sup 9} K), a moderate polarization, and a spectral shape that evolves considerably with time. This study demonstrates the possibility of imaging the eruptive HC structure at the metric wavelength and provides strong constraints on the t-IV emission mechanism, which, if understood, can be used to diagnose the essential parameters of the eruptive structure.},
doi = {10.3847/2041-8205/830/1/L2},
url = {https://www.osti.gov/biblio/22654207}, journal = {Astrophysical Journal Letters},
issn = {2041-8205},
number = 1,
volume = 830,
place = {United States},
year = {Mon Oct 10 00:00:00 EDT 2016},
month = {Mon Oct 10 00:00:00 EDT 2016}
}