Waves in Interplanetary Shocks: A Wind/WAVES Study

Wilson, L. B.; Cattell, C. A.; Kellogg, P. J.; Goetz, K.; Kersten, K.; Hanson, L. E.; Macgregor, Riley P; Kasper, J. C.

doi:10.1103/physrevlett.99.041101

Cited by 86 publications

(155 citation statements)

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“…Previous studies focusing on electric field observations of some of the higher-frequency modes observed amplitudes exceeding ∼200 mV/m [e.g., Breneman et al, 2013;Hull et al, 2006;Mozer and Sundkvist, 2013;Wilson et al, 2007. Recent Vlasov simulations using realistic mass ratios [e.g., Petkaki et al, 2006;Petkaki and Freeman, 2008;Lui, 2006, 2007] show that the effective collision frequencies, wave-particle interactions, previously estimated from quasi-linear theory are ∼2-3 orders of magnitude too small.…”

Section: Introductionmentioning

confidence: 99%

“…Therefore, we will focus on the relevance of wave-particle interactions as an energy dissipation mechanism in low-to-mid Mach number shocks. Thus, our work will focus on high-frequency electrostatic waves, specifically the ECDI waves, IAWs, and trains of ESWs because of the following: (1) previous observations [e.g., Wilson et al, 2007] found the highest probability of occurrence of large-amplitude IAWs in the shock ramp; (2) several studies have documented very large amplitude electrostatic fluctuations in collisionless shock ramps [e.g., Bale et al, 1998Bale et al, , 2002Breneman et al, 2013;Hull et al, 2006;Mozer and Sundkvist, 2013;Wilson et al, 2007; and (3) theory predicts [e.g., Sagdeev, 1966;Coroniti, 1970;Tidman and Krall, 1971;Wu et al, 1984;Treumann, 2009] that high-frequency electrostatic waves can be the dominant form of energy dissipation for these shocks.…”

Section: Introductionmentioning

confidence: 99%

“…In addition, previous studies of collisionless shocks have found any combination of the following electromagnetic and electrostatic fluctuations: (1) magnetosonic whistler waves [e.g., Hull et al, 2012;Sundkvist et al, 2012;Wilson et al, 2009Wilson et al, , 2012, (2) high-frequency electromagnetic whistler mode waves [e.g., Hull et al, 2012;Wilson et al, 2013a], (3) trains of electrostatic solitary waves (ESWs) or electron phase space holes [e.g., Bale et al, 1998Bale et al, , 2002, (4) ion-acoustic waves (IAWs) [e.g., Fuselier and Gurnett, 1984;Balikhin et al, 2005;Wilson et al, 2007], and/or (5) the electron cyclotron drift instability (ECDI) [Breneman et al, 2013;. Note that the ECDI is an instability, not a wave.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

et al. 2014

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“…Waveform data from Polar [Hull et al, 2006] and Cluster [Giagkiozis et al, 2011] have also been used to identify large amplitude ( 80 mV/m) ion acoustic waves at the bow shock transition region. An important observation from these and other waveform analyses [Wilson et al, 2007[Wilson et al, , 2010 is that these waves can be large amplitude and bursty. The combined influence of significant numbers of large amplitude waves can potentially provide an important contribution to overall energy dissipation at the bow shock.…”

Section: Introductionmentioning

confidence: 99%

STEREO and Wind observations of intense cyclotron harmonic waves at the Earth's bow shock and inside the magnetosheath

et al. 2013

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[1] We present the first observations of electron cyclotron harmonic waves at the Earth's bow shock from STEREO and Wind burst waveform captures. These waves are observed at magnetic field gradients at a variety of shock geometries ranging from quasi-parallel to nearly perpendicular along with whistler mode waves, ion acoustic waves, and electrostatic solitary waves. Large amplitude cyclotron harmonic waveforms are also observed in the magnetosheath in association with magnetic field gradients convected past the bow shock. Amplitudes of the cyclotron harmonic waves range from a few tens to more than 500 mV/m peak-peak. A comparison between the short (15 m) and long (100 m) Wind spin plane antennas shows a similar response at low harmonics and a stronger response on the short antenna at higher harmonics. This indicates that wavelengths are not significantly larger than 100 m, consistent with the electron cyclotron radius. Waveforms are broadband and polarizations are distinctively comma-shaped with significant power both perpendicular and parallel to the magnetic field. Harmonics tend to be more prominent in the perpendicular directions. These observations indicate that the waves consist of a combination of perpendicular Bernstein waves and field-aligned waves without harmonics. A likely source is the electron cyclotron drift instability which is a coupling between Bernstein and ion acoustic waves. These waves are the most common type of high-frequency wave seen by STEREO during bow shock crossings and magnetosheath traversals and our observations suggest that they are an important component of the high-frequency turbulent spectrum in these regions.

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“…Ion Acoustic Waves are also often (but not always) reported in connection to interplanetary shocks (Kurth et al, 1979;Hess et al, 1998;Wilson et al, 2007). The IAW activity is strongly increased at the shock time passage but is also noticeable several hours upstream and downstream of a shock.…”

Section: Ion Acoustic Wavesmentioning

confidence: 99%

Plasma waves above the ion cyclotron frequency in the solar wind: a review on observations

Briand

2009

Nonlin. Processes Geophys.

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Waves in Interplanetary Shocks: A Wind/WAVES Study

Cited by 86 publications

References 31 publications

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

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

STEREO and Wind observations of intense cyclotron harmonic waves at the Earth's bow shock and inside the magnetosheath

Plasma waves above the ion cyclotron frequency in the solar wind: a review on observations

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