Fast measurements of parameters of the Solar Wind using the BMSW instrument

Zastenker, G. N.; Šafránková, Jana; Němeček, Zdenek; Přech, Lubomír; Cermak, I.; Vaverka, Jakub; Komárek, Arnošt; Voita, J.; Chesalin, L. S.; Karimov, B. T.; Agafonov, Yu. N.; Бородкова, Н. Л.; Gavrilova, E. A.; Gagua, T. I.; Gagua, I. T.; Dalin, Peter; Dyachkov, A.; Koloskova, I. V.; Leibov, A. V.; Semena, N.; Чернов, В. В.; Markov, Y. I.; Ryazanova, E. E.; Ryazanrtseva, M. O.; Shevyrev, N. N.; Chrapchenkov, V. V.; Chugunova, O. M.; Yurasov, A. S.

doi:10.1134/s0010952513020081

Cited by 50 publications

(23 citation statements)

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“…For more detailed description of the instrument see Šafránková, Němeček, Přech, Zastenker, Cěrmák, et al () and Zastenker et al (). The BMSW data quick looks are available at http://aurora.troja.mff.cuni.cz/spektr-r/web-site.…”

Section: Data Setsmentioning

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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Section: Data Setsmentioning

confidence: 99%

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

et al. 2018

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“…Solar wind instrument suite Plasma‐F [ Zelenyi et al , ] is a payload of opportunity onboard Spectr‐R Russian radio astronomy mission [ Andreyanov et al , ] launched on 18 July 2011 on a highly elliptic orbit with apogee almost at a Moon orbit [ Kardashev et al , ]. Plasma‐F includes fast solar wind flow spectrometer [ Zastenker et al , ], energetic particle spectrometer [ Baláž et al , ], and data storage unit. Such an orbit allows prolonged solar wind observations for the most of the calendar year.…”

Section: Instrumentation and Datamentioning

confidence: 99%

Oscillations of energetic ions flux near the Earth's bow shock

et al. 2015

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A new type of variability in the foreshock and magnetosheath is revealed with the recent energetic particle experiments monitor of electrons and protons (MEP) onboard Spectr‐R spacecraft and solid‐state telescope onboard Time History of Events and Macroscale Interactions during Substorms spacecraft, which have high time resolution. Oscillations of energetic ion fluxes are observed in the broad energy range ∼4–400 keV, with periods 10–30 s, often rather monochromatic waveform and accompanied with magnetic oscillations. Such events are not so rare (∼100 cases are found for 2007–2012) but are associated mostly with high‐speed solar wind.

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“…The first results provided by this instrument are published in [23,[34][35][36][37][38]. Such multiscale structure of SW is described in numerous papers (e.g.…”

Section: Introductionmentioning

confidence: 99%

“…The BMSW instrument was specially designed for measuring some SW plasma parameters with very high time resolution (see [33][34][35]). The main axis of the BMSW instrument is permanently directed to the Sun within the limits of 5-10 • deviation.…”

Section: Introductionmentioning

confidence: 99%

Dynamic properties of small-scale solar wind plasma fluctuations

Рязанцева

Budaev

Zelenyǐ

et al. 2015

Phil. Trans. R. Soc. A.

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The paper presents the latest results of the studies of small-scale fluctuations in a turbulent flow of solar wind (SW) using measurements with extremely high temporal resolution (up to 0.03 s) of the bright monitor of SW (BMSW) plasma spectrometer operating on astrophysical SPECTR-R spacecraft at distances up to 350 000 km from the Earth. The spectra of SW ion flux fluctuations in the range of scales between 0.03 and 100 s are systematically analysed. The difference of slopes in low- and high-frequency parts of spectra and the frequency of the break point between these two characteristic slopes was analysed for different conditions in the SW. The statistical properties of the SW ion flux fluctuations were thoroughly analysed on scales less than 10 s. A high level of intermittency is demonstrated. The extended self-similarity of SW ion flux turbulent flow is constantly observed. The approximation of non-Gaussian probability distribution function of ion flux fluctuations by the Tsallis statistics shows the non-extensive character of SW fluctuations. Statistical characteristics of ion flux fluctuations are compared with the predictions of a log-Poisson model. The log-Poisson parametrization of the structure function scaling has shown that well-defined filament-like plasma structures are, as a rule, observed in the turbulent SW flows.

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Fast measurements of parameters of the Solar Wind using the BMSW instrument

Cited by 50 publications

References 4 publications

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

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

Oscillations of energetic ions flux near the Earth's bow shock

Dynamic properties of small-scale solar wind plasma fluctuations

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