Theory and Simulation of the Beam Cyclotron Instability

Lampe, Mártin; Manheimer, Wallace M.; McBride, J. B.; Orens, Joseph H.; Papadopoulos, K.; Shanny, R.; Sudan, R. N.

doi:10.1063/1.1693961

Cited by 125 publications

(63 citation statements)

References 12 publications

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“…In spite of the consensus that saturation of the beam-cyclotron instability via resonance broadening occurs at a low level of electric field turbulence (Lampe et al, 1972;Biskamp, 1973 and Lemons and Gary, 19781, it is riot clear that this will be true for solar wind parameters. The cr cal amplitude of the turbulent fields when resonance broadening becomes important was found by Lampe et al [1972] to be E = 960(NTe(ae/we)'(1/kaa))112 (mV/m), with T measured in eV.…”

Section: Forward and Reverse Shocksmentioning

confidence: 97%

“…As in Figure 8, V SW=450 km s -1 , N=7 cm -3 , B=5 y, and -e /T i -3. The results are shown in a relationship derived by Lampe et al [1972] for the case T »T i . Although the ratio ym /w is rather small, ranging from 5x10 -3 -5x10 -2 , ym is 5-6 times greater than found for the MTSI (cf.…”

Section: Forward and Reverse Shocksmentioning

confidence: 99%

“…The dispersion relation for A • )}=0 and kL e >1 has been derived by Lampe et al [1972], and is given by where a e =V a/w e is the electron Debye length, and % is assumed parallel to ji. The neglect of electromagnetic effects in (3.4) is well ,justified for the parameter range of interest [Lampe et al, 19721.…”

Section: Forward and Reverse Shocksmentioning

confidence: 99%

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Microscale instabilities in stream interaction regions

Eviatar¹,

Goldstein²

1980

J. Geophys. Res.

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A theoretical investigation of the microstructure of solar wind stream interaction regions is presented. We discuss the role of several electrostatic kinetic instabilities which may be important within the stream interface and the compression region. Inside of 1 AU the interface is likely to be stable against the electrostatic streaming instabilities considered. Between 1 and 2 AU we argue that the interface will excite the magnetized ion‐ion instability. The compression region is also found to be unstable beyond 1 AU, where the modified two‐stream instability, beam‐cyclotron instability, and ion‐acoustic instability will be important in determining the structure of the compressive pulses as they evolve into forward and reverse shocks. We conclude that the modified two‐stream instability and beam‐cyclotron instability predominately play a role in heating the electrons to the threshold for the ion‐acoustic instability. Various electrostatic plasma waves, ranging in frequency from the lower‐hybrid to harmonics of the electron cyclotron frequency, would be produced by these instabilities. Their signature should also be seen by high time resolution measurements of the temperature of the various plasma species.

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Section: Forward and Reverse Shocksmentioning

confidence: 97%

Section: Forward and Reverse Shocksmentioning

confidence: 99%

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Microscale instabilities in stream interaction regions

Eviatar¹,

Goldstein²

1980

J. Geophys. Res.

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“…ECDI-driven waves are important for shock physics because they are capable of resonantly interacting with the bulk of the ion distribution and preferentially heating the electrons perpendicular to B o [Forslund et al, 1970[Forslund et al, , 1972Lampe et al, 1972]. More recent work has shown that the ECDI can produce a suprathermal tail on the ion distribution and can strongly heat the electrons [Muschietti and Lembège, 2013].…”

Section: A1 Themis Examplesmentioning

confidence: 99%

“…The typical growth rates for the observed modes are k : ≤ lh (or ≤20-200 rad/s) [e.g., Lampe et al, 1972;Forslund et al, 1972;Muschietti and Lembège, 2013] for the ECDI, ∼ 10 −2 pi (or ∼30-90 rad/s) [e.g., Dum et al, 1980;Akimoto and Winske, 1985;Petkaki et al, 2006] for IAWs, ≤ 10 −1 Ω ce (or ∼88-880 rad/s) [e.g., Dum et al, 1980;Moreira, 1983;Baumjohann et al, 1999] for the high-frequency whistler mode waves, and ≤ 10 −1 pe [e.g., Omura et al, 1996] for ESWs. Therefore, when the wave amplitudes are large B ≫ k for the ESWs and ⋙ k for the ECDI, IAWs, and high-frequency whistler mode waves.…”

Section: Appendix A: High Frequency Wavesmentioning

confidence: 99%

Quantified energy dissipation rates in the terrestrial bow shock: 2. Waves and dissipation

et al. 2014

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Key Points:• Microscopic wave-particle interactions can regulate macroscopic shock structure • High-frequency large-amplitude waves are ubiquitous in collisionless shocks • Wave-particle interactions are the end result of nearly all dissipation pathways AbstractWe present the first quantified measure of the energy dissipation rates, due to wave-particle interactions, in the transition region of the Earth's collisionless bow shock using data from the Time History of Events and Macroscale Interactions during Substorms spacecraft. Our results show that wave-particle interactions can regulate the global structure and dominate the energy dissipation of collisionless shocks. In every bow shock crossing examined, we observed both low-frequency (<10 Hz) and high-frequency (≳10 Hz) electromagnetic waves throughout the entire transition region and into the magnetosheath. The low-frequency waves were consistent with magnetosonic-whistler waves. The high-frequency waves were combinations of ion-acoustic waves, electron cyclotron drift instability driven waves, electrostatic solitary waves, and whistler mode waves. The high-frequency waves had the following: (1) peak amplitudes exceeding B ∼ 10 nT and E ∼ 300 mV/m, though more typical values were B ∼ 0.1-1.0 nT and E ∼ 10-50 mV/m; (2) Poynting fluxes in excess of 2000 μW m −2 (typical values were ∼ 1-10 μW m −2 ); (3) resistivities > 9000 Ω m; and (4) associated energy dissipation rates > 10 μW m −3 . The dissipation rates due to wave-particle interactions exceeded rates necessary to explain the increase in entropy across the shock ramps for ∼90% of the wave burst durations. For ∼22% of these times, the wave-particle interactions needed to only be ≤ 0.1% efficient to balance the nonlinear wave steepening that produced the shock waves. These results show that wave-particle interactions have the capacity to regulate the global structure and dominate the energy dissipation of collisionless shocks.

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Microturbulence in the electron cyclotron frequency range at perpendicular supercritical shocks

Muschietti

Lembège

2013

JGR Space Physics

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[1] Supercritical perpendicular collisionless shocks are characterized by a fraction of the incoming ions being reflected at the steep front. These reflected ions accumulate and form a foot, where the relative drift of the reflected ion beam versus the electrons can easily excite an electron cyclotron drift instability (ECDI). Here, we analyze the resulting wave emissions by two approaches. First, our linear dispersion analysis shows that several electron Bernstein harmonics can be unstable, their number being proportional to the drift, yet limited by the ion beam temperature. Second, the three local populations (incoming electrons/ions and reflected ions) of the foot region are introduced in full electromagnetic particle-in-cell (PIC) periodic simulations in order to analyze the nonlinear regime of the ECDI. The main results are the following: (1) High gyroharmonics develop over a short time scale less than the lower hybrid period. (2) The spectral power shifts toward lower k modes to accumulate on the first harmonic under the effects of two complementary processes: (i) trapping of the reflected ion beam and (ii) resonance broadening. The latter acts to demagnetize the electrons in the dispersion relation. It initially applies to very high k modes (k e >> 1) and progressively, as time evolves, to lower k modes, invalidating the existence of all gyroharmonics except the first one. (3) In the late stage, a magnetic field component surprisingly develops in the energy spectrum that had so far been electrostatic. (4) The electrons are heated, which represents a source of preheating in the foot region of the shock front.Citation: Muschietti, L., and B. Lembège (2013), Microturbulence in the electron cyclotron frequency range at perpendicular supercritical shocks,

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Theory and Simulation of the Beam Cyclotron Instability

Cited by 125 publications

References 12 publications

Microscale instabilities in stream interaction regions

Microscale instabilities in stream interaction regions

Quantified energy dissipation rates in the terrestrial bow shock: 2. Waves and dissipation

Microturbulence in the electron cyclotron frequency range at perpendicular supercritical shocks

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