Magnetic Reconnection as a Driver for a Sub-ion-scale Cascade in Plasma Turbulence

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F17%3A00484359" target="_blank" >RIV/67985815:_____/17:00484359 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.3847/2041-8213/aa93fb" target="_blank" >http://dx.doi.org/10.3847/2041-8213/aa93fb</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.3847/2041-8213/aa93fb" target="_blank" >10.3847/2041-8213/aa93fb</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Magnetic Reconnection as a Driver for a Sub-ion-scale Cascade in Plasma Turbulence

Popis výsledku v původním jazyce

A new path for the generation of a sub-ion-scale cascade in collisionless space and astrophysical plasma turbulence, triggered by magnetic reconnection, is uncovered by means of high-resolution two-dimensional hybridkinetic simulations employing two complementary approaches, Lagrangian and Eulerian, and different driving mechanisms. The simulation results provide clear numerical evidence that the development of power-law energy spectra below the so-called ion break occurs as soon as the first magnetic reconnection events take place, regardless of the actual state of the turbulent cascade at MHD scales. In both simulations, the reconnection-mediated small-scale energy spectrum of parallel magnetic fluctuations exhibits a very stable spectral slope of similar to-2.8, whether or not a large-scale turbulent cascade has already fully developed. Once a quasi-stationary turbulent state is achieved, the spectrum of the total magnetic fluctuations settles toward a spectral index of -5/3 in the MHD range and of similar to-3 at sub-ion scales.

Název v anglickém jazyce

Magnetic Reconnection as a Driver for a Sub-ion-scale Cascade in Plasma Turbulence

Popis výsledku anglicky

A new path for the generation of a sub-ion-scale cascade in collisionless space and astrophysical plasma turbulence, triggered by magnetic reconnection, is uncovered by means of high-resolution two-dimensional hybridkinetic simulations employing two complementary approaches, Lagrangian and Eulerian, and different driving mechanisms. The simulation results provide clear numerical evidence that the development of power-law energy spectra below the so-called ion break occurs as soon as the first magnetic reconnection events take place, regardless of the actual state of the turbulent cascade at MHD scales. In both simulations, the reconnection-mediated small-scale energy spectrum of parallel magnetic fluctuations exhibits a very stable spectral slope of similar to-2.8, whether or not a large-scale turbulent cascade has already fully developed. Once a quasi-stationary turbulent state is achieved, the spectrum of the total magnetic fluctuations settles toward a spectral index of -5/3 in the MHD range and of similar to-3 at sub-ion scales.

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

Návaznosti

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

Rok uplatnění

2017

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

—

Svazek periodika

850

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

6

Strana od-do

"L16/1"-"L16/6"

Kód UT WoS článku

000415860700002

EID výsledku v databázi Scopus

2-s2.0-85035363904