Plasma fluctuations at the flanks of the Earth's magnetosheath  at ion kinetic scales

Rakhmanova, L. S.; Рязанцева, М. О.; Zastenker, G. N.

doi:10.5194/angeo-34-1011-2016

Cited by 17 publications

(20 citation statements)

References 33 publications

(42 reference statements)

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“…Rakhmanova et al. (2016) showed that the polar angle fluctuation spectra are typically steeper than the spectra of the ion flux value fluctuations. This is also the case in the present study.…”

Section: Magnetosheath Crossingmentioning

confidence: 99%

“…Alexandrova et al. 2013; Bruno & Carbone 2013) and at the flank MSH (Alexandrova 2008; Rakhmanova, Riazantseva & Zastenker 2016; Riazantseva et al. 2016).…”

Section: Introductionmentioning

confidence: 99%

“…Recently, studies of the turbulent cascade at these scales were performed in the MSH based on systematic ion flux measurements (Rakhmanova et al. 2016; Riazantseva et al. 2016).…”

Section: Introductionmentioning

confidence: 99%

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High-frequency plasma fluctuations in the middle magnetosheath and near its boundaries: Spektr-R observations

et al. 2017

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We present a case study of the flank magnetosheath crossing by the Spektr-R satellite. High time resolution measurements of the ion flux value and its direction provided by the BMSW (Fast Solar Wind Monitor) instrument are examined at different distances from the magnetosheath boundaries – the bow shock and the magnetopause. The magnetosheath behind the quasi-perpendicular bow shock is analysed. The time resolution of these data – 31 ms – is sufficient for observing the frequency spectra of plasma fluctuations both at the magnetohydrodynamics (MHD) and ion kinetic scales. Generally, MHD scales are characterised by Kolmogorov-like spectra ${\sim}f^{-5/3}$ while spectra at kinetic scales are steeper with a break existing between the two scales. We examine evolution of spectral parameters such as power density and slopes, and the break frequency together with the evolution of properties of the probability distribution function. We find out that (i) power spectral densities of the two quantities change differently toward the magnetosheath (MSH) boundaries, (ii) the spectra slopes do not change significantly across the magnetosheath, (iii) the break frequency of the spectrum changes toward the magnetopause. In the middle MSH the spectra are affected by instabilities supposed to be ion cyclotron instabilities. We demonstrate that the plasma is low intermittent in the middle MSH and highly intermittent near its boundaries in the absence of large-scale variations.

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Section: Magnetosheath Crossingmentioning

confidence: 99%

“…Alexandrova et al. 2013; Bruno & Carbone 2013) and at the flank MSH (Alexandrova 2008; Rakhmanova, Riazantseva & Zastenker 2016; Riazantseva et al. 2016).…”

Section: Introductionmentioning

confidence: 99%

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High-frequency plasma fluctuations in the middle magnetosheath and near its boundaries: Spektr-R observations

et al. 2017

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“…Kinetic‐scale plasma fluctuations have been explored systematically since 2011 with the help of the BMSW (Fast Solar Wind Monitor, Šafránková, Němeček, Přech, Zastenker, Cěrmák, et al, ; Zastenker et al, ) instrument on board Spektr‐R spacecraft. Parameters of plasma turbulence based on BMSW measurements were considered in the SW (Chen et al, ; Riazantseva et al, , , ; Šafránková, Němeček, Přech, & Zastenker, ; Šafránková et al, , ) as well as in the flank MSH (Rakhmanova et al, ; Rakhmanova, Riazantseva, Zastenker & Yermolaev, ; Riazantseva et al, , ). The BMSW data set covers 6 years of continuous plasma measurements in the SW and MSH that allow for statistical study of plasma fluctuations for various ambient conditions and upstream SW parameters.…”

Section: Introductionmentioning

confidence: 99%

Kinetic‐Scale Ion Flux Fluctuations Behind the Quasi‐Parallel and Quasi‐Perpendicular Bow Shock

et al. 2018

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Properties of kinetic‐scale plasma turbulence are examined observationally with the help of Spektr‐R measurements in the Earth's magnetosheath. The statistics covers 6 years of ion flux measurements during years 2011–2017 and includes a few dozens of the magnetosheath crossings with total duration of 250 hr. Several types of Fourier spectra are distinguished in the magnetosheath according to a spectral shape at the scales of transition from magnetohydrodynamic to kinetic regimes. Spectral indices and occurrence rate of different spectral shapes are examined at different locations with respect to the magnetosheath boundaries—the magnetopause and the bow shock. Magnetosheath plasma behind the quasi‐parallel and quasi‐perpendicular bow shock is explored separately. Clear dynamics of spectral shapes across the magnetosheath is shown: spectra with broad bump at the transition frequencies occur more frequently in the vicinity of the bow shock, while spectra with plateau at the same frequencies are usually observed closer to the magnetopause. Spectral indices such as spectral slope at the kinetic scales and break frequency are shown to be weakly affected by the boundaries behind the quasi‐perpendicular bow shock. The steepest spectra are observed close to the quasi‐parallel bow shock.

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“…2013 b , 2015, 2016; Riazantseva et al. 2015, 2016; Rakhmanova, Riazantseva & Zastenker 2016; Rakhmanova et al. 2017) allows us to expand our knowledge on processes in the dissipation range and in the transition region.…”

Section: Introductionmentioning

confidence: 99%

Variety of shapes of solar wind ion flux spectra: Spektr-R measurements

et al. 2017

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The paper is devoted to the shapes of the solar wind ion flux fluctuation spectrum at the transition between the inertial and the kinetic range using in situ high-resolution measurements of the Russian mission Spektr-R. We analyse the variability of the transition region and select five typical types of spectral shapes: (i) spectra with two slopes and one break, (ii) spectra characterized by a nonlinear steepening in the kinetic range, (iii) spectra with flattening in the vicinity of the break, (iv) spectra with a bump in the vicinity of the break and (v) spectra without any steepening in the kinetic range. The most popular is the well-known type (i) observed in approximately half of the cases. The second most popular type of spectra is type (iii) occurring in approximately one third of the cases. The other three types are observed less often: type (ii) – in approximately 6 %; type (iv) in 3 % and type (v) in 6 % of cases. An analysis of typical plasma conditions for different types of spectra revealed that the last two type of spectra (iv) and (v) are generally observed in a very slow solar wind with a low proton density, (i) and (iii) are observed in the solar wind with rather typical conditions and (ii) is usually observed in high-speed streams. The effect of nonlinear steepening of the spectra in the kinetic range increases with the solar wind speed. We present also the analysis of statistical properties of the observed events and compare them with the predictions of several statistical turbulence models. We show that intermittency is always observed in the solar wind flow despite the presence of one or another shape of spectra. The log-Poisson model with a dominant contribution of filament-like structures shows the best parameterization of the experimentally observed scaling.

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Plasma fluctuations at the flanks of the Earth's magnetosheath at ion kinetic scales

Cited by 17 publications

References 33 publications

High-frequency plasma fluctuations in the middle magnetosheath and near its boundaries: Spektr-R observations

High-frequency plasma fluctuations in the middle magnetosheath and near its boundaries: Spektr-R observations

Kinetic‐Scale Ion Flux Fluctuations Behind the Quasi‐Parallel and Quasi‐Perpendicular Bow Shock

Variety of shapes of solar wind ion flux spectra: Spektr-R measurements

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