A Preliminary Study of the Dynamic Spectra of Solar Radio Bursts in the Frequency Range 500-950 Mc/s.

Young, Charles W.; Spencer, Chance L.; Moreton, G. E.; Roberts, Jane

doi:10.1086/147019

Cited by 114 publications

(80 citation statements)

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“…Oscillations and quasi-periodic pulsations (QPPs) in radio emission from solar flares have been observed for half a century (Young et al 1961). Pulsation phenomena can be formally categorized by the wavelength of the emission and by the frequency/period of the QPPs.…”

Section: Introductionmentioning

confidence: 99%

“…For example, at meter and decimeter wavelengths, rapid QPPs occur with periods of tens to hundreds of milliseconds. Typically, these QPPs have rapidly varying amplitudes, variable periods, and narrow bandwidths δf/f 1 (e.g., Young et al 1961;Zlobec et al 1987;Stepanov & Yurovsky 1990;Kurths et al 1991;Yurovsky 1991;Fleishman et al 1994;Aschwanden et al 1995;Fleishman et al 2002aFleishman et al , 2002bMagdalenić et al 2002;Benz et al 2005;Mészárosová et al 2005;Chen & Yan 2007;Benz et al 2011;Chen et al 2011). Longer-period QPPs, with periods τ 10 s, are observed in microwaves; such QPPs are often accompanied by QPPs in hard X-rays (HXRs; e.g., Parks & Winckler 1969;Janssens et al 1973;Zaitsev & Stepanov 1982a;Kane et al 1983;Nakajima et al 1983;Asai et al 2001;Grechnev et al 2003;Nakariakov et al 2003;Stepanov et al 2004;Melnikov et al 2005;Fleishman et al 2008).…”

Section: Introductionmentioning

confidence: 99%

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Modeling of Gyrosynchrotron Radio Emission Pulsations Produced by Magnetohydrodynamic Loop Oscillations in Solar Flares

Mossessian

Fleishman

2012

ApJ

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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.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Modeling of Gyrosynchrotron Radio Emission Pulsations Produced by Magnetohydrodynamic Loop Oscillations in Solar Flares

Mossessian

Fleishman

2012

ApJ

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“…Some type III burst will only exist at high frequencies above 100MHz [6]. These solar type III radio emissions is dominant a few days before solar flare and Coronal Mass Ejections explosion [7,8,9].…”

Section: Introductionmentioning

confidence: 99%

Preliminary Analysis on the Solar Burst Type III and the Effect of the Magnetic Reconnection

Husien

Hamidi

Shariff

et al. 2015

ILCPA

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ABSTRACT. From the data from a BLEIN Callisto site, we aim to provide a comprehensive description of the synopsis formation and dynamics of a a single solar burst type III and magnetic reconnection effect. The data above is the solar radio burst type iii occurred on 10th September 2005 between 05:44 UT till 06:00 UT.This eruption has started since 5:55 UT with a formation of type III solar burst. The wave emission process of solar radio burst type III from magnetic reconnection region in a solar flare were investigated by using a two-dimensional, that are electromagnetic and relativistic particle-in-cell code. The solar radio burst type III initially impose into two plasma populations : background dense plasma and hot electrons that can be generated by the magnetic reconnection process in a solar flare. The conversion of the energy stored in the magnetic field by a process called the magnetic reconnection released the energy in the solar flares and related phenomena. By the launching the e-CALLISTO network, its prove the existence of the magnetic reconnection on the surface of the sun in radio region.

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“…In the case of BBP, the frequency drift can be as high as (≈-250 MHz s −1 ) [7]. This type of burst is dominant a few days before solar flare and Coronal Mass Ejections explosion [8,9,10].…”

Section: Introductionmentioning

confidence: 99%

The Evolution of Unstable 'Beta-Gamma' Magnetic Fields of Active Region AR 2222

Hamidi

Sabri

Shariff

et al. 2015

ILCPA

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This event allows us to investigate how plasma-magnetic field interactions in the solar corona can produce suprathermal electron populations over periods from tens of minutes to several hours, and the interactions of wave-particle and wave-wave lead to characteristic fine structures of the emission. An intense and broad solar radio burst type IV was recorded by CALLISTO spectrometer from 240-360 MHz. Using data from a the KRIM observatory, we aim to provide a comprehensive description of the synopsis formation and dynamics of a a single solar burst type IV event due to active region AR2222. For five minutes, the event exhibited strong pulsations on various time scales and "broad patterns" with a formation of a group type III solar burst. AR 2222 remained the most active region, producing a number of minor C-Class solar flares. The speed of the solar wind also exceeds 370.8 km/second with 10.2 g/cm 3 density of proton in the solar corona. The radio flux also shows 171 SFU. Besides, there are 3 active regions, AR2217, AR2219 and AR2222 potentially pose a threat for Mclass solar flares. Active region AR2222 have unstable 'beta-gamma' magnetic fields that harbor energy for M-class flares. As a conclusion, we believed that Sun's activities more active in order to achieve solar maximum cycle at the end of 2014.

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A Preliminary Study of the Dynamic Spectra of Solar Radio Bursts in the Frequency Range 500-950 Mc/s.

Cited by 114 publications

References 0 publications

Modeling of Gyrosynchrotron Radio Emission Pulsations Produced by Magnetohydrodynamic Loop Oscillations in Solar Flares

Modeling of Gyrosynchrotron Radio Emission Pulsations Produced by Magnetohydrodynamic Loop Oscillations in Solar Flares

Preliminary Analysis on the Solar Burst Type III and the Effect of the Magnetic Reconnection

The Evolution of Unstable 'Beta-Gamma' Magnetic Fields of Active Region AR 2222

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