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

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F17%3A10371715" target="_blank" >RIV/00216208:11320/17:10371715 - isvavai.cz</a>

Result on the web

<a href="http://dx.doi.org/10.1017/S0022377817000502" target="_blank" >http://dx.doi.org/10.1017/S0022377817000502</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1017/S0022377817000502" target="_blank" >10.1017/S0022377817000502</a>

Result language

angličtina

Original language name

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

Original language description

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.

Czech name

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Czech description

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Type

J_imp - Article in a specialist periodical, which is included in the Web of Science database

CEP classification

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OECD FORD branch

10305 - Fluids and plasma physics (including surface physics)

Project

<a href="/en/project/GA16-04956S" target="_blank" >GA16-04956S: Solar wind as a natural laboratory: structure, turbulence, and shocks.</a><br>

Continuities

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Publication year

2017

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

Journal of Plasma Physics

ISSN

0022-3778

e-ISSN

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Volume of the periodical

83

Issue of the periodical within the volume

4

Country of publishing house

GB - UNITED KINGDOM

Number of pages

24

Pages from-to

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UT code for WoS article

000424148100001

EID of the result in the Scopus database

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