Detailed study of electron plasma waves upstream of the Earth’s bow shock

Etcheto, J.; Faucheux, M.

doi:10.1029/ja089ia08p06631

Cited by 121 publications

(102 citation statements)

References 30 publications

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“…Astrophysical examples include Type II and III solar radio bursts (Lin et al 1981(Lin et al , 1986Dulk et al 1984;Goldman 1983;Robinson et al 1993aRobinson et al ,b, 1994Reid & Ratcliffe 2014), outer heliospheric radio emission (Kurth et al 1984), and in planetary electron foreshocks (Etcheto & Faucheux 1984;Moses et al 1984;Fuselier et al 1985;Lacombe et al 1985). Related processes in laboratory plasmas have also been discussed by, e.g.…”

Section: Introductionmentioning

confidence: 99%

Self-consistent particle-in-cell simulations of fundamental and harmonic plasma radio emission mechanisms

Thurgood

Tsiklauri

2015

A&A

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Aims. The simulation of three-wave interaction based plasma emission, thought to be the underlying mechanism for Type III solar radio bursts, is a challenging task requiring fully-kinetic, multi-dimensional models. This paper aims to resolve a contradiction in past attempts, whereby some studies indicate that no such processes occur. Methods. We self-consistently simulate three-wave based plasma emission through all stages by using 2D, fully kinetic, electromagnetic particle-in-cell simulations of relaxing electron beams using the EPOCH2D code.Results. Here we present the results of two simulations;, which we find to permit and prohibit plasma emission respectively. We show that the possibility of plasma emission is contingent upon the frequency of the initial electrostatic waves generated by the bump-in-tail instability, and that these waves may be prohibited from participating in the necessary three-wave interactions due to frequency conservation requirements. In resolving this apparent contradiction through a comprehensive analysis, in this paper we present the first self-consistent demonstration of fundamental and harmonic plasma emission from a single-beam system via fully kinetic numerical simulation. We caution against simulating astrophysical radio bursts using unrealistically dense beams (a common approach which reduces run time), as the resulting non-Langmuir characteristics of the initial wave modes significantly suppresses emission. Comparison of our results also indicates that, contrary to the suggestions of previous authors, an alternative plasma emission mechanism based on two counter-propagating beams is unnecessary in an astrophysical context. Finally, we also consider the action of the Weibel instability which generates an electromagnetic beam mode. As this provides a stronger contribution to electromagnetic energy than the emission, we stress that evidence of plasma emission in simulations must disentangle the two contributions and not simply interpret changes in total electromagnetic energy as evidence of plasma emission.

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Section: Introductionmentioning

confidence: 99%

Self-consistent particle-in-cell simulations of fundamental and harmonic plasma radio emission mechanisms

Thurgood

Tsiklauri

2015

A&A

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“…The wave spectral features and their spatial dependence are described in detail by Etcheto and Faucheux [1984], Fuselief et al [1985], and Lacombe et al [1985]. Narrowband waves (bandwidths of less than a few percent of fpe ) with frequencies near the local plasma frequency fpe (which is typically about 30 kHz, though it varies depending on the solar wind plasma density) are gen- Electromagnetic waves with frequencies of fpeand 2fpehave been observed in regions close to the bow shock and are associated with electrostatic oscillations [Scarf et al, 1970;Dunckel, 1974;Gurnett, 1975 Gary [1985], who showed that when a beam has a sufficiently large density and/or a sufficiently small temperature the Langmuir mode is stable and that a beam mode can be unstable with wave growth occurring at frequencies above the ion plasma frequency.…”

Section: Fitzenreiter Et Al [1990] Developed a 3-d Analyticalmentioning

confidence: 99%

Plasma waves in the Earth's electron foreshock: 1. Time‐of‐flight electron distributions in a generalized Lorentzian plasma and dispersion solutions

Yin¹,

Ashour‐Abdalla²,

Bosqued³

et al. 1998

J. Geophys. Res.

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Abstract. The correlated studies discussed here used high-quality and frequent in situ measurements provided by the Wind spacecraft to investigate the properties of the foreshock plasma (measured by Wind/3DPlasma) and the enhanced plasma waves (detected by Wind/WAVES). A time-of-flight electron distribution model was developed in a generalized Lorentzian plasma using experimental data. The Wind/3DP results show that typical foreshock electron distributions are well approximated by this model, although discernible "bumps" in distributions that may be unstable are not often observed or resolved by the 3DP instrument. We used unstable distributions described by the model to initialize our study. In addition to verifying the interdependence of dispersion, cutoff velocity and beam density that was previously found in a Maxwellian beam-plasma system, our dispersion solutions demonstrate how the dispersion topology and wave spectral bandwidths evolve as a consequence of wave modifications of time-of-flight distributions. By identifying sections of distributions that interact with each of the growing and damping branches, we analyzed the role played by nonthermal electrons in the evolution of the instability. Our results complement those from previous investigations and, more importantly, provide information about the linear behavior of the system that will enable the simulation studies discussed in our companion paper [Y in et al., this issue] to examine possible nonlinear interactions and to address the issue of whether nonlinear wave-wave interactions in the foreshock nonthermal plasma are a significant factor in producing the observed electromagnetic emissions.

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“…Using data from ISEE 1, Etcheto and Faucheux (1984) found that the maximum amplitudes of the Langmuir waves were a few millivolts per meter at the edge of the foreshock and only a few tens to a few hundreds of microvolts per meter inside the foreshock. During a time period when the solar wind magnetic field was unusually constant, used ISEE 1 plasma wave data to show that there is a slight offset of the high wave amplitude region from the boundary of the foreshock.…”

Section: Introductionmentioning

confidence: 99%

Statistical behavior of foreshock Langmuir waves observed by the Cluster wideband data plasma wave receiver

Sigsbee

Kletzing²,

Gurnett³

et al. 2004

Ann. Geophys.

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Abstract. We present the statistics of Langmuir wave amplitudes in the Earth's foreshock using Cluster Wideband Data (WBD) Plasma Wave Receiver electric field waveforms from spacecraft 2, 3 and 4 on 26 March 2002. The largest amplitude Langmuir waves were observed by Cluster near the boundary between the foreshock and solar wind, in agreement with earlier studies. The characteristics of the waves were similar for all three spacecraft, suggesting that variations in foreshock structure must occur on scales greater than the 50-100 km spacecraft separations. The electric field amplitude probability distributions constructed using waveforms from the Cluster WBD Plasma Wave Receiver generally followed the log-normal statistics predicted by stochastic growth theory for the event studied. Comparison with WBD receiver data from 17 February 2002, when spacecraft 4 was set in a special manual gain mode, suggests nonoptimal auto-ranging of the instrument may have had some influence on the statistics.

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Detailed study of electron plasma waves upstream of the Earth’s bow shock

Cited by 121 publications

References 30 publications

Self-consistent particle-in-cell simulations of fundamental and harmonic plasma radio emission mechanisms

Self-consistent particle-in-cell simulations of fundamental and harmonic plasma radio emission mechanisms

Plasma waves in the Earth's electron foreshock: 1. Time‐of‐flight electron distributions in a generalized Lorentzian plasma and dispersion solutions

Statistical behavior of foreshock Langmuir waves observed by the Cluster wideband data plasma wave receiver

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