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Title: MODELING OF GYROSYNCHROTRON RADIO EMISSION PULSATIONS PRODUCED BY MAGNETOHYDRODYNAMIC LOOP OSCILLATIONS IN SOLAR FLARES

Abstract

A quantitative study of the observable radio signatures of the sausage, kink, and torsional magnetohydrodynamic (MHD) oscillation modes in flaring coronal loops is performed. Considering first non-zero order effect of these various MHD oscillation modes on the radio source parameters such as magnetic field, line of sight, plasma density and temperature, electron distribution function, and the source dimensions, we compute time-dependent radio emission (spectra and light curves). The radio light curves (of both flux density and degree of polarization) at all considered radio frequencies are then quantified in both time domain (via computation of the full modulation amplitude as a function of frequency) and in Fourier domain (oscillation spectra, phases, and partial modulation amplitude) to form the signatures specific to a particular oscillation mode and/or source parameter regime. We found that the parameter regime and the involved MHD mode can indeed be distinguished using the quantitative measures derived in the modeling. We apply the developed approach to analyze radio burst recorded by Owens Valley Solar Array and report possible detection of the sausage mode oscillation in one (partly occulted) flare and kink or torsional oscillations in another flare.

Authors:
;  [1]
  1. Center For Solar-Terrestrial Research, New Jersey Institute of Technology, Newark, NJ 07102 (United States)
Publication Date:
OSTI Identifier:
22016085
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 748; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; DISTRIBUTION FUNCTIONS; EMISSION SPECTRA; FLUX DENSITY; FREQUENCY DEPENDENCE; GAMMA RADIATION; MAGNETIC FIELDS; MAGNETOHYDRODYNAMICS; OSCILLATION MODES; PLASMA DENSITY; PULSATIONS; RADIOWAVE RADIATION; SIMULATION; SOLAR CORONA; SOLAR FLARES; SOLAR RADIATION; SUN; TIME DEPENDENCE; X RADIATION

Citation Formats

Mossessian, George, and Fleishman, Gregory D. MODELING OF GYROSYNCHROTRON RADIO EMISSION PULSATIONS PRODUCED BY MAGNETOHYDRODYNAMIC LOOP OSCILLATIONS IN SOLAR FLARES. United States: N. p., 2012. Web. doi:10.1088/0004-637X/748/2/140.
Mossessian, George, & Fleishman, Gregory D. MODELING OF GYROSYNCHROTRON RADIO EMISSION PULSATIONS PRODUCED BY MAGNETOHYDRODYNAMIC LOOP OSCILLATIONS IN SOLAR FLARES. United States. https://doi.org/10.1088/0004-637X/748/2/140
Mossessian, George, and Fleishman, Gregory D. 2012. "MODELING OF GYROSYNCHROTRON RADIO EMISSION PULSATIONS PRODUCED BY MAGNETOHYDRODYNAMIC LOOP OSCILLATIONS IN SOLAR FLARES". United States. https://doi.org/10.1088/0004-637X/748/2/140.
@article{osti_22016085,
title = {MODELING OF GYROSYNCHROTRON RADIO EMISSION PULSATIONS PRODUCED BY MAGNETOHYDRODYNAMIC LOOP OSCILLATIONS IN SOLAR FLARES},
author = {Mossessian, George and Fleishman, Gregory D},
abstractNote = {A quantitative study of the observable radio signatures of the sausage, kink, and torsional magnetohydrodynamic (MHD) oscillation modes in flaring coronal loops is performed. Considering first non-zero order effect of these various MHD oscillation modes on the radio source parameters such as magnetic field, line of sight, plasma density and temperature, electron distribution function, and the source dimensions, we compute time-dependent radio emission (spectra and light curves). The radio light curves (of both flux density and degree of polarization) at all considered radio frequencies are then quantified in both time domain (via computation of the full modulation amplitude as a function of frequency) and in Fourier domain (oscillation spectra, phases, and partial modulation amplitude) to form the signatures specific to a particular oscillation mode and/or source parameter regime. We found that the parameter regime and the involved MHD mode can indeed be distinguished using the quantitative measures derived in the modeling. We apply the developed approach to analyze radio burst recorded by Owens Valley Solar Array and report possible detection of the sausage mode oscillation in one (partly occulted) flare and kink or torsional oscillations in another flare.},
doi = {10.1088/0004-637X/748/2/140},
url = {https://www.osti.gov/biblio/22016085}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 748,
place = {United States},
year = {Sun Apr 01 00:00:00 EDT 2012},
month = {Sun Apr 01 00:00:00 EDT 2012}
}