Spectrum of kinetic plasma turbulence at 0.3-0.9 astronomical units from the Sun

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F21%3A00547579" target="_blank" >RIV/67985815:_____/21:00547579 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/68378289:_____/21:00543392

Výsledek na webu

<a href="https://doi.org/10.1103/PhysRevE.103.063202" target="_blank" >https://doi.org/10.1103/PhysRevE.103.063202</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1103/PhysRevE.103.063202" target="_blank" >10.1103/PhysRevE.103.063202</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Spectrum of kinetic plasma turbulence at 0.3-0.9 astronomical units from the Sun

Popis výsledku v původním jazyce

We investigate spectral properties of turbulence in the solar wind that is a weakly collisional astrophysical plasma, accessible to in situ observations. Using the Helios search coil magnetometer measurements in the fast solar wind, in the inner heliosphere, we focus on properties of the turbulent magnetic fluctuations at scales smaller than the ion characteristic scales, the so-called kinetic plasma turbulence. At such small scales, we show that magnetic power spectra between 0.3 and 0.9 AU from the Sun have a generic shape similar to f(-8/3) exp (-f/f(d)), where the dissipation frequency f(d) is correlated with the Doppler shifted frequency f(rho e) of the electron Larmor radius. This behavior is statistically significant: all the observed kinetic spectra are well described by this model, with f(d) = f(rho e)/1.8. Our results indicate that the electron gyroradius plays the role of the dissipation scale and marks the end of the electromagnetic cascade in the solar wind.

Název v anglickém jazyce

Spectrum of kinetic plasma turbulence at 0.3-0.9 astronomical units from the Sun

Popis výsledku anglicky

We investigate spectral properties of turbulence in the solar wind that is a weakly collisional astrophysical plasma, accessible to in situ observations. Using the Helios search coil magnetometer measurements in the fast solar wind, in the inner heliosphere, we focus on properties of the turbulent magnetic fluctuations at scales smaller than the ion characteristic scales, the so-called kinetic plasma turbulence. At such small scales, we show that magnetic power spectra between 0.3 and 0.9 AU from the Sun have a generic shape similar to f(-8/3) exp (-f/f(d)), where the dissipation frequency f(d) is correlated with the Doppler shifted frequency f(rho e) of the electron Larmor radius. This behavior is statistically significant: all the observed kinetic spectra are well described by this model, with f(d) = f(rho e)/1.8. Our results indicate that the electron gyroradius plays the role of the dissipation scale and marks the end of the electromagnetic cascade in the solar wind.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

<a href="/cs/project/GA18-08861S" target="_blank" >GA18-08861S: Plazmová turbulence na iontových škálách ve slunečním větru</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2021

Kód důvěrnosti údajů

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

Název periodika

Physical Review E

ISSN

2470-0045

e-ISSN

2470-0053

Svazek periodika

103

Číslo periodika v rámci svazku

6

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

9

Strana od-do

063202

Kód UT WoS článku

000657177000007

EID výsledku v databázi Scopus

2-s2.0-85108077108