<i>Solar Radio Astronomy</i>

Kundu, M. R.; Hagger, H. J.

doi:10.1063/1.3034108

Cited by 136 publications

(221 citation statements)

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“…There are two mechanisms can contribute to the radio emission from non-flaring coronal plasma which are a thermal bremsstrahlung (free-free) and thermal gyroemission [108,109]. Thermal bremsstrahlung is the minimum possible radio intensity emitted by the plasma.…”

Section: Volume 35mentioning

confidence: 99%

“…A power law electron energy distribution with exponent −3 to −5 is found satisfactory to account for the time profile of the radio burst. In general, bursts are considered to be a significant characteristic of solar activity because they are generally attributed to a sudden acceleration of particles from the Sun [108,122]. The first observations and radio burst classification in decimetric region was done by (Young, Spencer, Moreton, & and Roberts, 1961).…”

Section: Solar Radio Burstmentioning

confidence: 99%

“…Literature about radio bursts is rather extended and appeared [2,29,105,108,123]. One of the main reason detecting solar burst is because this is the important tool for specifying magnetic, thermal and density structures at the time.…”

Section: Solar Radio Burstmentioning

confidence: 99%

“…The initial statistical studies of solar bursts were inadequate to single-frequency observations, [108,[129][130][131][132] using data recorded during Solar Cycle 20. Some of the first statistical studies of this kind analyzed by [133,134] using radio data recorded at up to five frequencies.…”

Section: Volume 35mentioning

confidence: 99%

“…This determines that the SRBT II cannot appear at any altitude. It has been known for decades that about 50 % of SRBT II are preceded by a group of SRBT III by several minutes [108]. Recently, it has been shown that the overall frequency envelope of the precursor type III bursts drifts at a rate close to that of the associated type II bursts [213].…”

Section: Combination Of Srbt II and Srbt Iiimentioning

confidence: 99%

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Probability of Solar Flares Turn out to Form a Coronal Mass Ejections Events due to the Characterization of Solar Radio Burst Type II and III

Hamidi

2014

ILCPA

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The solar flare and Coronal Mass Ejections (CMEs) are well known as one of the most massive eruptions which potentially create major disturbances in the interplanetary medium and initiate severe magnetic storms when they collide with the Earth's magnetosphere. However, how far the solar flare can contribute to the formation of the CMEs is still not easy to be understood. These phenomena are associated with II and III burst it also divided by sub-type of burst depending on the physical characteristics and different mechanisms. In this work, we used a Compound Astronomical Low-cost Low-frequency Instrument for Spectroscopy in Transportable Observatories (CALLISTO) system. The aim of the present study is to reveal dynamical properties of solar burst type II and III due to several mechanisms. Most of the cases of both solar radio bursts can be found in the range less that 400 MHz. Based on solar flare monitoring within 24 hours, the CMEs that has the potential to explode will dominantly be a class of M1 solar flare. Overall, the tendencies of SRBT III burst form the solar radio burst type III at 187 MHz to 449 MHz. Based on solar observations, it is evident that the explosive, short time-scale energy release during flares and the long term, gradual energy release expressed by CMEs can be reasonably understood only if both processes are taken as common and probably not independent signatures of a destabilization of pre-existing coronal magnetic field structures. The configurations of several active regions can be sourced regions of CMEs formation. The study of the formation, acceleration and propagation of CMEs requires advanced and powerful observational tools in different spectral ranges as many 'stages' as possible between the photosphere of the Sun and magnetosphere of the Sun and magnetosphere of the Earth. In conclusion, this range is a current regime of solar radio bursts during CMEs events.

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Section: Volume 35mentioning

confidence: 99%

Section: Solar Radio Burstmentioning

confidence: 99%

Section: Solar Radio Burstmentioning

confidence: 99%

Section: Volume 35mentioning

confidence: 99%

Section: Combination Of Srbt II and Srbt Iiimentioning

confidence: 99%

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Probability of Solar Flares Turn out to Form a Coronal Mass Ejections Events due to the Characterization of Solar Radio Burst Type II and III

Hamidi

2014

ILCPA

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A self‐consistent mechanism for electron cyclotron maser emission and its application to type III solar radio bursts

Chen

Zhao

et al. 2017

JGR Space Physics

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Type III solar radio bursts (SRBs) produced by fast electron beams (FEBs) traveling along solar magnetic fields are the best known and the most important kind of SRBs because of their clearest association with FEBs as well as most frequent observations during solar activities. However, the physics of their emitting mechanism has been a controversial issue. Based on the electron cyclotron maser (ECM) instability driven directly by a magnetized FEB, whose physics is fairly well known from the Earth's auroral kilometric radiation, this paper proposes a self‐consistent mechanism for type III SRBs, in which the Alfvén wave (AW) produced by the current instability of the beam‐return current system associated with the FEB, called the self‐generated AW, plays an important and crucial role. Taking into account the return‐current effect of the FEB, the growth rate and the saturation intensity of the self‐generated AW are estimated. Then the effects of the self‐generated AW on the ECM emission via the ECM instability driven by the magnetized FEB are further investigated. The results show that the self‐generated AW can significantly influence and change the physical properties of the ECM emission. In particular, this novel ECM emission mechanism can effectively overcome the main difficulties of the conventional ECM emission mechanism in application to type III SRBs and may potentially provide a self‐consistent physics scenario for type III SRBs.

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Are short‐time variations of the solar S‐component emission identical with microwave bursts?

et al. 1997

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Extended time series (time resolution about 2-3 min) of spatially resolved observations (2 17 arcsec) in one dimension of solar S-component sources obtained at the Siberian Solar Radio Telescope (SSRT) at 5.2 cm wavelength allow the detection of evolutional features of the growth and decay of active regions in the solar corona. Characteristic slow flux variations with timescales of about 1-2 hours occurring during the decay phase of the radio emission in the low corona above plages and sunspots are compared with recently detected step-like flux increases on timescales of about 10-20 min followed by quasi-constant periods appearing in the initial phase of the development of active regions. Superimposed on this basic behaviour, also fluctuations at shorter timescales (or even periodic oscillations) have been observed. As it is well known from emission-model calculations, the variations of the S-component radiation can be due to variations of the magnetic field and/or changes of the energy of the radiating particles, which is basically the same emission mechanism as for microwave bursts. Since the "S-component" is originally defined by its long timescale behaviour derived from whole-Sun flux density measurements, the presently detected small-timescale features in S-component sources require either a revised definition of S-component emission or must be considered as "burst-like" .

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Solar Radio Astronomy

Cited by 136 publications

References 0 publications

Probability of Solar Flares Turn out to Form a Coronal Mass Ejections Events due to the Characterization of Solar Radio Burst Type II and III

Probability of Solar Flares Turn out to Form a Coronal Mass Ejections Events due to the Characterization of Solar Radio Burst Type II and III

A self‐consistent mechanism for electron cyclotron maser emission and its application to type III solar radio bursts

Are short‐time variations of the solar S‐component emission identical with microwave bursts?

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