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CMSO 2005 cattaneo@flash.uchicago.edu Mean field dynamos: analytical and numerical results Fausto Cattaneo Center for Magnetic-Self Organization and Department of Mathematics University of Chicago

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CMSO 2005 Historical considerations 1919 Dynamo action introduced (Larmor) 30s – 50sAnti-dynamo theorems (Cowling; Zeldovich) 50s - 60s Averaging is introduced Formulation of Mean Field Electrodynamics (Parker 1955; Braginskii 1964; Steenbeck, Krause & Radler 1966) 90s – now Large scale computing. MHD equations can be solved directly »Check validity of assumptions »Explore other types of dynamos Universal mechanism for generation of large-scale fields from turbulence lacking reflectional symmetry

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CMSO 2005 Mean Field Theory Evolution equations for the Mean field (homogeneous, isotropic case) Transport coefficients determined by velocity and R m – mean inductionrequires lack of reflectional symmetry (helicity) –β turbulent diffusivity Many assumption needed –Linear relation between and –Separations of scales FOS (quasi-linear) approximation –Short correlation time – Assumed that fluctuations not self-excited

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CMSO 2005 Troubles In order for MFT to work: fluctuations must be controlled by smoothing procedure (averages) system must be strongly irreversible When R m << 1 irreversibility provided by diffusion When R m >> 1, problems arise: development of long memory loss of irreversibility unbounded growth of fluctuations

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CMSO 2005 Examples Exactly solvable kinematic model (Boldyrev & FC) –lots of assumptions –can be treated analytically Nonlinear rotating convection (Hughes & FC) –fewer assumptions –solved numerically ______________________________________________________________ Shear-buoyancy driven dynamo (Brummell, Cline & FC) –Intrinsically nonlinear dynamo –Not described by MFT

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CMSO 2005 Solvable models Model for random passive advection (Kazentsev 1968; Kraichnan 1968) Velocity: zero mean, homogeneous, isotropic, incompressible, Gaussian and delta-correlated in time Exact evolution equation for magnetic field correlator Input: velocity correlator Ouput: magnetic correlator

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CMSO 2005 Solvable models Exact evolution equation –Non-helical case (C= 0): Kazantsev 1968 –Helical case: Vainshtein & Kichatinov 1986; Kim & Hughes 1997 –Spectral version: Kulsrud & Anderson 1992; Berger& Rosner 1995 –Symmetric form: Boldyrev, Cattaneo & Rosner 2005 Operator in square brackets is self-adjoint

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CMSO 2005 Solvable models Dynamo growth rate from MFT: In this model MFT is exact; with Dynamo growth rate of mean field: Dynamo growth rate of fluctuations: Large scale asymptotics of corresponding eigenfunction

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CMSO 2005 Solvable models Conclusion: For a fixed time t, large enough spatial scales exist such that averages of the fluctuations are negligible. –on these scales the evolution of the average field is described by MFT However For any spatial scale x, contributions from mean field to the correlator at those scales quickly becomes subdominant Fluctuations eventually take over on any scale

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CMSO 2005 Convectively driven dynamos with rotation Cattaneo & Hughes g hot cold B0B0 Energy densities time kinetic magnetic x 4

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CMSO 2005 Rotating convection Turbulent convection with near-unit Rossby number System has strong small-scale fluctuations No evidence for mean field generation Non rotatingRotating Cattaneo & Hughes Energy: hor. averageEnergy ratioMagnetic fieldVelocity

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CMSO 2005 What is going on? System has helicity, yet no mean field Consider two possibilities: –Nonlinear saturation of turbulent -effect (Cattaneo & Vainshtein 1991; Kulsrud & Anderson 1992; Gruzinov & Diamond 1994) – -effect is collisional and not turbulent

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CMSO 2005 Averages and -effect emf: volume average emf: volume average and cumulative time average Introduce (external) uniform mean field. Compute below dynamo threshold. Calculate average emf. Extremely slow convergence. Cattaneo & Hughes time

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CMSO 2005 Convectively driven dynamos The α-effect here is inversely proportional to Pm (i.e. proportional to η). It is therefore not turbulent but collisional Convergence requires huge sample size. –Divergence with decreasing η? Small-scale dynamo is turbulent but -effects is not!! Press this if running out of time

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CMSO 2005 Something completely different B y + Interaction between localized velocity shear and weak background poloidal field generates intense toroidal magnetic structures Magnetic buoyancy leads to complex spatio-temporal beahviour Cline, Brummell & Cattaneo

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CMSO 2005 Shear driven dynamo B y - B y + Slight modification of shear profile leads to sustained dynamo action System exhibits cyclic behaviour, reversals, even episodes of reduced activity

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CMSO 2005 Conclusion In turbulent dynamos behaviour dominated by fluctuations Averages not well defined for realistic sample sizes In realistic cases large-scale field generation possibly driven by non-universal mechanisms –Shear –Large scale motions –Boundary effects

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CMSO 2005 The end

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Turbulent Dynamo Stanislav Boldyrev (Wisconsin-Madison) Fausto Cattaneo (Chicago) Center for Magnetic Self-Organization in Laboratory and Astrophysical.

Turbulent Dynamo Stanislav Boldyrev (Wisconsin-Madison) Fausto Cattaneo (Chicago) Center for Magnetic Self-Organization in Laboratory and Astrophysical.

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