Plasma Turbulence and Kinetic Instabilities at Ion Scales in the Expanding Solar Wind

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F15%3A00452203" target="_blank" >RIV/67985815:_____/15:00452203 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/68378289:_____/15:00451773

Výsledek na webu

<a href="http://dx.doi.org/10.1088/2041-8205/811/2/L32" target="_blank" >http://dx.doi.org/10.1088/2041-8205/811/2/L32</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1088/2041-8205/811/2/L32" target="_blank" >10.1088/2041-8205/811/2/L32</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Plasma Turbulence and Kinetic Instabilities at Ion Scales in the Expanding Solar Wind

Popis výsledku v původním jazyce

The relationship between a decaying strong turbulence and kinetic instabilities in a slowly expanding plasma is investigated using two-dimensional (2D) hybrid expanding box simulations. We impose an initial ambient magnetic field perpendicular to the simulation box, and we start with a spectrum of large-scale, linearly polarized, random-phase Alfvenic fluctuations that have energy equipartition between kinetic and magnetic fluctuations and vanishing correlation between the two fields. A turbulent cascade rapidly develops; magnetic field fluctuations exhibit a power-law spectrum at large scales and a steeper spectrum at ion scales. The turbulent cascade leads to an overall anisotropic proton heating, protons are heated in the perpendicular direction, and, initially, also in the parallel direction. The imposed expansion leads to generation of a large parallel proton temperature anisotropy which is at later stages partly reduced by turbulence. The turbulent heating is not sufficient to ov

Název v anglickém jazyce

Plasma Turbulence and Kinetic Instabilities at Ion Scales in the Expanding Solar Wind

Popis výsledku anglicky

The relationship between a decaying strong turbulence and kinetic instabilities in a slowly expanding plasma is investigated using two-dimensional (2D) hybrid expanding box simulations. We impose an initial ambient magnetic field perpendicular to the simulation box, and we start with a spectrum of large-scale, linearly polarized, random-phase Alfvenic fluctuations that have energy equipartition between kinetic and magnetic fluctuations and vanishing correlation between the two fields. A turbulent cascade rapidly develops; magnetic field fluctuations exhibit a power-law spectrum at large scales and a steeper spectrum at ion scales. The turbulent cascade leads to an overall anisotropic proton heating, protons are heated in the perpendicular direction, and, initially, also in the parallel direction. The imposed expansion leads to generation of a large parallel proton temperature anisotropy which is at later stages partly reduced by turbulence. The turbulent heating is not sufficient to ov

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

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Projekt

<a href="/cs/project/GA15-10057S" target="_blank" >GA15-10057S: Ionty ve slunečním větru: korelace, omezení a kausalita</a><br>

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2015

Kód důvěrnosti údajů

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

Název periodika

Astrophysical Journal Letters

ISSN

2041-8205

e-ISSN

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Svazek periodika

812

Číslo periodika v rámci svazku

2

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

6

Strana od-do

"L32/1"-"L32/6"

Kód UT WoS článku

000364478600018

EID výsledku v databázi Scopus

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