Complex Type III‐like radio emissions observed from 1 to 14 MHz

Reiner, M. J.; Kaiser, M. L.

doi:10.1029/1998gl900317

Cited by 42 publications

(21 citation statements)

References 8 publications

(11 reference statements)

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“…STEREO/WAVES observations will also provide a new understanding of the complex type III-like bursts (formerly called SA events) that are nearly always associated with major flare events involving CMEs (Cane et al 1981;Reiner et al 2000). Reiner and Kaiser (1999) pointed out the unusual fine-structure characteristics of these complex type III-like emissions below about 10 MHz, such as shown in Figs. 1 and 2.…”

Section: Remote Sensing Of Type II (Cme-associated) and Type Iii (Flamentioning

confidence: 96%

S/WAVES: The Radio and Plasma Wave Investigation on the STEREO Mission

Bougeret¹,

Goetz²,

Kaiser³

et al. 2008

Space Sci Rev

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346

226

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This paper introduces and describes the radio and plasma wave investigation on the STEREO Mission: STEREO/WAVES or S/WAVES. The S/WAVES instrument includes a suite of state-of-the-art experiments that provide comprehensive measurements of the three components of the fluctuating electric field from a fraction of a hertz up to 16 MHz, plus a single frequency channel near 30 MHz. The instrument has a direction finding or goniopolarimetry capability to perform 3D localization and tracking of radio emissions associated with streams of energetic electrons and shock waves associated with Coronal Mass Ejections (CMEs). The scientific objectives include: (i) remote observation and measurement of radio waves excited by energetic particles throughout the 3D heliosphere that are associated with the CMEs and with solar flare phenomena, and (ii) in-situ measurement of the properties of CMEs and interplanetary shocks, such as their electron density and temperature and the associated plasma waves near 1 Astronomical Unit (AU). Two companion papers provide details on specific aspects of the S/WAVES instrument, namely the electric antenna system (Bale et al., Space Sci. Rev., 2007) and the direction finding technique (Cecconi et al., Space Sci. Rev., 2007).

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Section: Remote Sensing Of Type II (Cme-associated) and Type Iii (Flamentioning

confidence: 96%

S/WAVES: The Radio and Plasma Wave Investigation on the STEREO Mission

Bougeret¹,

Goetz²,

Kaiser³

et al. 2008

Space Sci Rev

Self Cite

346

226

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“…The third criterion is a semi-quantitative method of including the complexity typical for the CDAW events, which is consistent with previous discussions regarding multiple components [Mac-Dowall et al, 1987] and complex type III-like radio bursts [Reiner et al, 2000]. Reiner and Kaiser [1999] note that the unusual features of the ''complex type III-like bursts'' may include bursty emissions above $7 MHz, typically without measurable frequency drift, distinct diminution of the radio emission near 7 MHz, coalescence in fast frequency drifting features below $7 MHz, short duration, and narrow-band features with slow or no frequency drift. We identify a simple type III profile as one like that shown in Figure 1c, a multiple burst profile as the combination of several simple profiles that can be separated visually (Figure 1d), a group as multiple bursts that occur sufficiently close in time that they are appear to be merged together into one longer duration event (Figure 1e, $16:10-16:20), and a complex event (Figures 1a and 1f) as one where the appearance cannot be explained as a simple combination of several simple fast-drift profiles.…”

Section: Observationsmentioning

confidence: 99%

Long‐duration hectometric type III radio bursts and their association with solar energetic particle (SEP) events

MacDowall

Lara

Manoharan

et al. 2003

Geophysical Research Letters

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It has recently been suggested by Cane et al. [2002] that a class of type III solar radio bursts, called type III‐l, is reliably associated with intense solar energetic particle (SEP) events. They proposed that the causative electrons for these bursts are accelerated in regions of reconnecting magnetic field in the wakes of coronal mass ejections (CMEs). In this paper, we examine the durations, intensities, and other characteristics of such radio bursts in the hectometric frequency range and compare them to several groups of control events. We conclude that simple criteria, based on hectometric data alone, can identify the majority (∼80%) of type III‐l radio bursts, which are associated with >20 MeV SEP proton events, while excluding almost 100% of the control events. Detailed study of these type III‐l bursts may play a significant role in a better understanding of the acceleration of SEPs and of the magnetic field evolution in the vicinity of CMEs.

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“…For example, the generation of auroral roar is similar to that of terrestrial continuum radiation, which is generated via mode conversion of upper hybrid waves at the plasmapause, and possibly continuum radiations at other planets as well. Solar type III radiation results from mode conversion of Langmuir waves in the solar wind, and recent observations of structured type III emission [Reiner et al,23,24] indicate the significance of frequency structure in the causative Langmuir waves.…”

Section: Introductionmentioning

confidence: 97%

Phase Correlation of Electrons and Langmuir Waves

Kletzing

Muschietti²

Geospace Electromagnetic Waves and Radiation

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Abstract. Multiple spacecraft observations have confirmed the ubiquitous nature of Langmuir waves in the presence of auroral electrons. The electrons show variations consistent with bunching at or near the plasma frequency. Linear analysis of the interaction of a finite Gaussian packet of Langmuir waves shows that there are two components to the perturbation to the electron distribution function, one in-phase (or 180• out-of-phase) with respect to the wave electric field called the resistive component and one which is 90• (or 270• ) out-of-phase with respect to the electric field. For small wave packets, the resistive perturbation dominates. For longer wave packets, a non-linear analysis is appropriate which suggests that the electrons become trapped and the reactive phase dominates. Rocket observations have measured both components. The UI observations differ from those of the UC Berkeley observations in that a purely reactive phase bunching was observed as compared to a predominantly resistive perturbation. The resistive phase results of the UC Berkeley group were interpreted as arising from a short wave packet. The UI observations of the reactive phase can be explained by either a long, coherent train of Langmuir waves or that the narrower velocity response of the UI detectors made it possible to capture only one side of the reactive component of the perturbed distribution function for a short wave packet in the linear regime. Future wave-particle correlator experiments should be able to resolve these questions by providing more examples with better velocity space coverage.

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Complex Type III‐like radio emissions observed from 1 to 14 MHz

Cited by 42 publications

References 8 publications

S/WAVES: The Radio and Plasma Wave Investigation on the STEREO Mission

S/WAVES: The Radio and Plasma Wave Investigation on the STEREO Mission

Long‐duration hectometric type III radio bursts and their association with solar energetic particle (SEP) events

Phase Correlation of Electrons and Langmuir Waves

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