TY - GEN

T1 - Evolution of magnetic fields in the IGM: kinetic MHD turbulence

AU - de Lima, Reinaldo S.

AU - de Gouveia Dal Pino, E. M.

AU - Lazarian, A.

AU - Falceta-Goncalves, D.

PY - 2009

Y1 - 2009

N2 - In this work, we present 3D MHD simulations of non-helical, forced turbulence, with an anisotropic thermal pressure with respect to the orientation of the local magnetic field. Such anisotropy arises when the plasma, is weakly collisional, i.e., when the Larmor frequency is much greater than the ion-ion collision frequency. In this Kinetic MHD regime (KMHD), there are instabilities that give rise to fast; growing magnetic fluctuations in the smallest scales. The plasma that; fills the intergalactic and intracluster media has small density (n similar to 10(-3) cm(-3)), hence the effects of these instabilities could be important in the turbulent amplification of the magnetic fields there. In order to study the KMHD) turbulence, we have performed 3D numerical simulations employing a godunov-MHD) code (e.g., Kowal, Lazarian & Beresnyak 2007; Falceta-Goncalves, Lazarian & Kowal 2008). The power spectrum of the velocity and magnetic fields were calculated for two cases: when there is a pre-existing mean magnetic field, and when there is only an initial weak magnetic field.

AB - In this work, we present 3D MHD simulations of non-helical, forced turbulence, with an anisotropic thermal pressure with respect to the orientation of the local magnetic field. Such anisotropy arises when the plasma, is weakly collisional, i.e., when the Larmor frequency is much greater than the ion-ion collision frequency. In this Kinetic MHD regime (KMHD), there are instabilities that give rise to fast; growing magnetic fluctuations in the smallest scales. The plasma that; fills the intergalactic and intracluster media has small density (n similar to 10(-3) cm(-3)), hence the effects of these instabilities could be important in the turbulent amplification of the magnetic fields there. In order to study the KMHD) turbulence, we have performed 3D numerical simulations employing a godunov-MHD) code (e.g., Kowal, Lazarian & Beresnyak 2007; Falceta-Goncalves, Lazarian & Kowal 2008). The power spectrum of the velocity and magnetic fields were calculated for two cases: when there is a pre-existing mean magnetic field, and when there is only an initial weak magnetic field.

KW - Magnetic fields

KW - plasmas

KW - intergalactic medium

U2 - 10.1017/S1743921309031342

DO - 10.1017/S1743921309031342

M3 - Conference contribution

SN - 978-0-521-88990-2

T3 - IAU Symposium Proceedings Series

SP - 563

EP - 564

BT - COSMIC MAGNETIC FIELDS: FROM PLANETS, TO STARS AND GALAXIES

A2 - Strassmeier, KG

A2 - Kosovichev, AG

A2 - Beckman, JE

PB - Cambridge University Press

CY - CAMBRIDGE

T2 - 259th Symposium of the International-Astronomical-Union

Y2 - 3 November 2008 through 7 November 2008

ER -