Origin, Evolution, and Signatures of Cosmological Magnetic Fields, Nordita, June 2015 Evolution of magnetic fields in large scale anisotropic MHD flows.

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Presentation transcript:

Origin, Evolution, and Signatures of Cosmological Magnetic Fields, Nordita, June 2015 Evolution of magnetic fields in large scale anisotropic MHD flows Alexander Tevzadze Tbilisi State University, Georgia Abastumani Astrophys. Observatory, Georgia In collaboration with: T. Kahniashvili (CMU), A. Brandenburg (Nordita) E. Uchava (TSU, Georgia), S. Poedts, B. Shergelashvili (KULeuven, Belgium)

Outline Dilute plasmas; Anisotropic MHD description; – CGL MHD – Braginskii MHD – 16 momentum closure MHD Linear stability (16-mom. MHD) Nonlinear fluctuations in decaying anisotropic MHD; Summary A.T. “Evolution of magnetic fields in large scale anisotropic MHD flows” NORDITA 24 June

Dilute Plasmas Magnetized extragalactic plasmas is dilute collision freq. is much lower then Larmor freq. /  <<1 (dilute, collisionless, weakly collisional, collision poor) Exact description: kinetic theory Particle distribution function; micro physics + fluid effects; micro instabilities; fluid instabilities; (highly complex formalism) Can the MHD be used to describe such “fluids”? Collision freq. is much higher then fluid frequencies /  >>1 A.T. “Evolution of magnetic fields in large scale anisotropic MHD flows” NORDITA 24 June

MHD of Dilute Plasmas If we insist on fluid description of dilute plasmas, pressure can not be isotropic. Anisotropic MHD models (one fluid, one component) Anisotropic MHD should be able to resolve micro physics (micro instabilities) within simple one fluid (component) formalism. Anisotropic MHD Lab: the solar wind; Can we be still successful with “naive” MHD at large scales? A.T. “Evolution of magnetic fields in large scale anisotropic MHD flows” NORDITA 24 June

Anisotropic MHD models Isotropic one fluid MHD Isotropic one fluid MHD Equation of State: CGL (Chew Goldberger Low) MHD CGL (Chew Goldberger Low) MHD “double adiabatic” state (P ||, P ┴ ): Neglecting heat fluxes (high freq. processes) MHD waves + micro physics (Mirror and Fire-hose instabilities) A.T. “Evolution of magnetic fields in large scale anisotropic MHD flows” NORDITA 24 June

Anisotropic MHD models Anisotropic viscosity MHD (Braginskii MHD) Anisotropic viscosity MHD (Braginskii MHD) (Braginskii 1965, Hollweg 1985)  – viscosity parameter Local (viscous) properties of anisotropic plasmas A.T. “Evolution of magnetic fields in large scale anisotropic MHD flows” NORDITA 24 June

Anisotropic MHD models MHD model with heat fluxes: 16 momentum closure model (Oraevski et al. 1968, Ramos 2003, Dzhalilov et al. 2010) A.T. “Evolution of magnetic fields in large scale anisotropic MHD flows” NORDITA 24 June

16 Momentum MHD Linear spectrum: MHD classical; Fire-hose and Mirror instabilities; Effects of heat fluxes (entropy modes); Discrepancies between CGL-MHD and Kinetic theory are removed. (Mirror mode instability crit., Incompressible and compressible fire-hose instabilities, entropy modes); Dzhalilov, Kuznetsov, Staude 2008, 2010 Somov, Dzhalilov, Staude A.T. “Evolution of magnetic fields in large scale anisotropic MHD flows” NORDITA 24 June

16 Momentum MHD: Linear Analysis A.T. “Evolution of magnetic fields in large scale anisotropic MHD flows” NORDITA 24 June

16 Momentum MHD: Linear Analysis Anisotropic MHD shear flow in uniform magnetic field: V=(Sy, 0, 0), B=(B, 0, 0) Strong magnetic field -Heat flux instability (  cr = 0.85) -Shear flow overstability; (Uchava et al. 2014) Weak magnetic field Incompressible linear perturbations; linear thermo-kinetic invariant; (Uchava et al. (in prep.)) A.T. “Evolution of magnetic fields in large scale anisotropic MHD flows” NORDITA 24 June

Nonlinear Anisotropic MHD state Linear theory 16 momentum MHD: Long way to go … (especially at equipartition); Development of linear micro instabilities? Velocity shear overstability: smoothens velocity field Heat flux instability: limits maximal possible  Mirror and Fire-hose family: mimic collision effects? (Santos-Lima et al. 2014: CGL-MHD) Anisotropic MHDs saturates to classical MHD? - At large scales - Small scales ? MHD dynamo (micro phys. can be important) A.T. “Evolution of magnetic fields in large scale anisotropic MHD flows” NORDITA 24 June

Large Scale Magnetic Fluctuations A.T. “Evolution of magnetic fields in large scale anisotropic MHD flows” NORDITA 24 June

Large Scale Magnetic Fluctuations Assumptions: Turbulence fluctuations: incompressible; Constant anisotropy parameters: , . Fluctuation frequency: Fluctuating scale: integral scale of turbulence; Effective magnetic field: CGL MHD: Braginskii MHD: A.T. “Evolution of magnetic fields in large scale anisotropic MHD flows” NORDITA 24 June

Magnetic Fluctuations in Expanding Universe Helical MHD turbulence: Non-helical MHD turbulence: 16-m. anisotrop. MHD EOS: Kinetic fluctuations: A.T. “Evolution of magnetic fields in large scale anisotropic MHD flows” NORDITA 24 June

Summary 16 momentum MHD can be used to describe effects of anisotropy in dilute plasmas at large scales; MHD turbulence decay (helical, or not) predicts higher magnetic field energy then by anisotropic MHD state with constant  and . Possible outcomes -Anisotropy and/or heat flux effects grow: -Anisotropy effects change turbulence spectral shape; A.T. “Evolution of magnetic fields in large scale anisotropic MHD flows” NORDITA 24 June