Evolution of the Solar Flare Energetic Electrons in the Inhomogeneous Inner Heliosphere

Reid, Hamish; Kontar, Eduard P.

doi:10.1007/s11207-012-0013-x

Cited by 34 publications

(44 citation statements)

References 35 publications

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“…As in Reid & Kontar (2013), the electron transport assumes radial expansion of the beam due to expansion of magnetic field in the corona (described by the second term on the RHS of Eq. (1)).…”

Section: Electron-langmuir Wave Interactionsmentioning

confidence: 99%

“…(1) (Reid & Kontar 2013). The cross-sectional area of the electron beam therefore expands, and the electron density correspondingly decreases.…”

Section: Electron-langmuir Wave Interactionsmentioning

confidence: 99%

“…The background plasma is assumed to be isothermal at 1.5 MK, and the electron and ion temperatures are set everywhere equal. The plasma density profile is defined as in Reid & Kontar (2013), based on the model of Parker (1958) with normalisation as in Mann et al (1999), as the solution of…”

Section: Initial Conditionsmentioning

confidence: 99%

“…In this paper we present type III burst simulations based on the description of electron propagation and Langmuir wave evolution in inhomogeneous plasma of Reid & Kontar (2013). We add an angle-averaged model for plasma radio emission, described in Ratcliffe & Kontar (2014), in order to simulate the type III burst generation process from electrons to radio waves.…”

Section: Introductionmentioning

confidence: 99%

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Large-scale simulations of solar type III radio bursts: flux density, drift rate, duration, and bandwidth

Ratcliffe

Kontar

Reid

2014

A&A

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Non-thermal electrons accelerated in the solar corona can produce intense coherent radio emission, known as solar type III radio bursts. This intense radio emission is often observed from hundreds of MHz in the corona down to the tens of kHz range in interplanetary space. It involves a chain of physical processes from the generation of Langmuir waves to non-linear processes of wave-wave interaction. We develop a self-consistent model to calculate radio emission from a non-thermal electron population over a large frequency range, including the effects of electron transport, Langmuir wave-electron interaction, the evolution of Langmuir waves due to non-linear wave-wave interactions, Langmuir wave conversion into electromagnetic emission, and finally escape of the electromagnetic waves. For the first time we simulate escaping radio emission over a broad frequency range from 500 MHz down to a few MHz and infer key properties of the radio emission observed: the onset (starting) frequency, identification as fundamental or harmonic emission, peak flux density, instantaneous frequency bandwidth, and timescales for rise and decay. By comparing these large-scale simulations with the observations, we can identify the processes governing the major type III solar radio burst characteristics.

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Section: Electron-langmuir Wave Interactionsmentioning

confidence: 99%

“…(1) (Reid & Kontar 2013). The cross-sectional area of the electron beam therefore expands, and the electron density correspondingly decreases.…”

Section: Electron-langmuir Wave Interactionsmentioning

confidence: 99%

Section: Initial Conditionsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Large-scale simulations of solar type III radio bursts: flux density, drift rate, duration, and bandwidth

Ratcliffe

Kontar

Reid

2014

A&A

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“…They are categorized into five main types according to their spectral appearances: Type I, Type II, Type III, Type IV, and Type V radio bursts. Most of them are closely related to solar eruptions such as coronal mass ejections (CMEs) and solar flares (McLean, 1985;Cho et al, 2011;Reid and Kontar, 2013;Chen et al, 2014;Feng et al, 2015). Of the five types of solar radio bursts, a Type IV radio burst is the broadband continuum emission in metric wavelength that usually lasts for a relatively long time (> 10 minutes) (Pick, 1963).…”

Section: Introductionmentioning

confidence: 99%

A Solar Stationary Type IV Radio Burst and Its Radiation Mechanism

et al. 2018

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A stationary Type IV (IVs) radio burst was observed on September 24, 2011. Observations from the Nançay RadioHeliograph (NRH) show that the brightness temperature (T B ) of this burst is extremely high, over 10 11 K at 150 MHz and over 10 8 K in general. The degree of circular polarization (q) is between −60% ∼ −100%, which means that it is highly left-handed circularly polarized. The flux-frequency spectrum follows a power-law distribution, and the spectral index is considered to be roughly −3 ∼ −4 throughout the IVs. Radio sources of this event are located in the wake of the coronal mass ejection and are spatially dispersed. They line up to present a formation in which lower-frequency sources are higher. Based on these observations, it is suggested that the IVs was generated through electron cyclotron maser emission.

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Bimodal fluxes of near‐relativistic electrons during the onset of solar particle events

2013

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[1] We report for several solar energetic particle events (SEPs) intensity and anisotropy measurements of energetic electrons in the energy range 27 to 500 keV as observed with the Wind and ACE spacecraft in June 2000. The observations onboard Wind show bimodal pitch angle distributions (PADs), whereas ACE shows PADs with one peak, as usually observed for impulsive injection of electrons at the Sun. During the time of observation Wind was located upstream of the Earth's bow shock, in the dawn-noon sector, at distances of 40 to 70 R E from the Earth, and magnetically well connected to the quasi-parallel bow shock, whereas ACE, located at the libration point L1, was not connected to the bow shock. The electron intensity-time profiles and energy spectra show that the backstreaming electrons observed at Wind are not of magnetospheric origin. The observations rather suggest that the bimodal electron PADs are due to reflection or scattering at an obstacle located at a distance of less than 150 R E in the antisunward direction, compatible with the bow shock or magnetosheath of the magnetosphere of the Earth. For a modeling of the observations, we have performed transport simulations which include the effects of pitch angle diffusion, adiabatic focusing, and reflection at a boundary close to the point of observation. The results of the simulations demonstrate that the bimodal PADs are compatible with the reflection of electrons at a nearby boundary, at distances of 70 R E . This finding is supported by the orbital configuration and the magnetic field direction: Whereas ACE is not connected, Wind is well connected to the magnetosphere of the Earth.

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Evolution of the Solar Flare Energetic Electrons in the Inhomogeneous Inner Heliosphere

Cited by 34 publications

References 35 publications

Large-scale simulations of solar type III radio bursts: flux density, drift rate, duration, and bandwidth

Large-scale simulations of solar type III radio bursts: flux density, drift rate, duration, and bandwidth

A Solar Stationary Type IV Radio Burst and Its Radiation Mechanism

Bimodal fluxes of near‐relativistic electrons during the onset of solar particle events

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