Generalized self-similarity of intermittent plasma turbulence in space and laboratory plasmas

Budaev, V.P.; Zelenyǐ, L. M.; Savin, S.

doi:10.1017/s0022377815001099

Cited by 33 publications

(23 citation statements)

References 169 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…Recently, it was also shown to be the case for the ion flux fluctuations, including the kinetic range (Budaev et al. 2015; Riazantseva et al. 2015), but only for spectra with two slopes and one break.…”

Section: Statistical Properties Of Turbulence For Different Shapes Ofmentioning

confidence: 99%

“…Statistical properties of turbulence follow the universal laws despite the various conditions in the plasma in different areas of the near-Earth space and also in laboratory plasma (Budaev et al. 2011; Budaev, Zelenyi & Savin 2015). We will show below that the solar wind ion flux fluctuations for different shapes of spectra have similar statistical properties.…”

Section: Statistical Properties Of Turbulence For Different Shapes Ofmentioning

confidence: 99%

“…It is a rather typical situation for the solar wind turbulent flow (Burlaga 1991; Hnat, Chapman & Rowlands 2005; Budaev et al. 2015). Herewith the extended self-similarity (ESS) can be shown by linear dependence of from (Benzi et al.…”

Section: Statistical Properties Of Turbulence For Different Shapes Ofmentioning

confidence: 99%

“…The analysis of the experimental scaling can help to validate a preferred model of the intermittent turbulence (Budaev et al. 2011, 2015). The description of the observations of intermittent turbulence with the ESS can be implemented to the log-Poisson turbulence models.…”

Section: Statistical Properties Of Turbulence For Different Shapes Ofmentioning

confidence: 99%

See 3 more Smart Citations

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

et al. 2017

View full text Add to dashboard Cite

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.

show abstract

Section: Statistical Properties Of Turbulence For Different Shapes Ofmentioning

confidence: 99%

Section: Statistical Properties Of Turbulence For Different Shapes Ofmentioning

confidence: 99%

Section: Statistical Properties Of Turbulence For Different Shapes Ofmentioning

confidence: 99%

Section: Statistical Properties Of Turbulence For Different Shapes Ofmentioning

confidence: 99%

See 2 more Smart Citations

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

et al. 2017

View full text Add to dashboard Cite

show abstract

“…Для кратеров r ~ 10 мкм в диаметре время термодиффузии оценивается как τ ~ r 2 / ~1 мкс, предполагая коэффициент термодиффузии  ~ 1 cм 2 /с. Время τ ~ 1 мкс существенно меньше, чем типичные временные масштабы 10-100 мкс крупномасштабных флуктуаций плотности плазмы и электрического поля, обусловленные пристеночной плазменной турбулентностью [16,17]. Такие условия обеспечивают неизменность пристеночного плазменного слоя в течение развития одного дугового процесса, что обеспечивает независимость от флуктуаций приповерхностной плазмы токамака эволюции дуги, и есть основания применять для описания этих дуговых процессов выводы известных моделей дуговых явлений [4,5,[8][9][10].…”

Section: обсуждение результатовunclassified

Arcing Effects on Tokamak First Wall Tungsten Components Exposed to Plasma Loads

Budaev¹,

Khimchenko²,

Grashin³

et al. 2019

PAST-TF

View full text Add to dashboard Cite

В статье приведены последние экспериментальные исследования вольфрамовых материалов после экстремальных плазменных нагрузок в токамаке Т-10. Плазменная нагрузка на поверхность вольфрамовых лимитеров приводит к эрозии и формированию неоднородной шероховатой поверхности. Условия в приповерхностной плазме над шероховатой поверхностью благоприятны для формирования дуг и искр, влияющих на перегрев поверхности материала. Влияние униполярных дуг и искр на взаимодействие плазмы с поверхностью может привести к усилению теплообмена плазмы с поверхностью и к охлаждению плазмы. Неамбиполярный поток из-за дуговых эффектов рекомендуется учитывать при оценке эрозии диверторных вольфрамовых пластин в ИТЭР. Ключевые слова: токамак, дивертор, плазменно-тепловые испытания материалов, материалы термоядерного реактора, вольфрам, дуги.

show abstract