Analysis of the instability growth rate during the jet? background interaction in a magnetic field

Kód výsledku v IS VaVaI

RIV/67985815:_____/13:00392453 - isvavai.cz

Výsledek na webu

http://dx.doi.org/10.1088/1674-4527/13/6/008

DOI - Digital Object Identifier

10.1088/1674-4527/13/6/008

Jazyk výsledku

angličtina

Název v původním jazyce

Analysis of the instability growth rate during the jet? background interaction in a magnetic field

Popis výsledku v původním jazyce

The two-stream instability is common, responsible for many observed phenomena in nature, especially the interaction of jets of various origins with the background plasma (e.g. extragalactic jet interacting with the cosmic background). The dispersion relation that does not consider magnetic fields is described by the wellknown Buneman relation. In 2011, Bohata, Břeň and Kulhánek derived the relation for the two-stream instability without the cold limit, with the general orientation of a magnetic field, and arbitrary stream directions. The maximum value of the imaginary part of the individual dispersion branches omega(k) is of interest from a physical point of view. It represents the instability growth rate which is responsible for the onset of turbulence mode and subsequent reconnection on the scale of the ion radius accompanied by a strong plasma thermalization. The paper presented here is focused on the non-relativistic instability growth rate and its dependence on various input param

Název v anglickém jazyce

Analysis of the instability growth rate during the jet? background interaction in a magnetic field

Popis výsledku anglicky

The two-stream instability is common, responsible for many observed phenomena in nature, especially the interaction of jets of various origins with the background plasma (e.g. extragalactic jet interacting with the cosmic background). The dispersion relation that does not consider magnetic fields is described by the wellknown Buneman relation. In 2011, Bohata, Břeň and Kulhánek derived the relation for the two-stream instability without the cold limit, with the general orientation of a magnetic field, and arbitrary stream directions. The maximum value of the imaginary part of the individual dispersion branches omega(k) is of interest from a physical point of view. It represents the instability growth rate which is responsible for the onset of turbulence mode and subsequent reconnection on the scale of the ion radius accompanied by a strong plasma thermalization. The paper presented here is focused on the non-relativistic instability growth rate and its dependence on various input param

Druh

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

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

—

Projekt

GD205/09/H033: Obecná relativita a její aplikace v astrofyzice a kosmologii

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2013

Kód důvěrnosti údajů

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

Název periodika

Research in Astronomy and Astrophysics

ISSN

1674-4527

e-ISSN

—

Svazek periodika

13

Číslo periodika v rámci svazku

6

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

8

Strana od-do

687-694

Kód UT WoS článku

000319704300008

EID výsledku v databázi Scopus

—