Download presentation

Presentation is loading. Please wait.

Published byKaylee Johnson Modified over 3 years ago

1
Turbulent transport of magnetic fields Fausto Cattaneo Center for Magnetic Self-Organization in Laboratory and Astrophysical Plasmas Chicago 2003

2
Motivation/Objective Chicago 2003 Typically: present physical motivation for research (not the case here) Rather: Decide if subject is suitable area of research for center activity Apparently, of some interest to several neighbouring communities –Geophysics –Planetary physics –Dynamo theorists –Generic astrophysics Present some of the issues

3
Turbulent transport Chicago 2003 Important effect of turbulence is greatly to enhance transport over collisional values. Reynolds, Peclet, magnetic Reynolds numbers are ratios of turbulent to collisional diffusivities Magnetic fields affect turbulence, hence its transport properties Can consider transport of –temperature fluctuations –energetic particles-chemical species –angular momentum –magnetic fields

4
Mean-field-electrodynamics Chicago 2003 Two-scale approach. Consider the kinematic problem Introduce averages Mean-field equation

5
Closure of mean-field equations Chicago 2003 Closure requires equations for mean emf Consider evolution of fluctuations Isotropic case α mean induction β eddy diffusion Linearity establishes relationship between mean field and mean emf

6
Transport coefficients Chicago 2003 In kinematic regime α and β should be determined solely by Rm and the statistics of u α is a pseudo-scalar (tensor) requires lack of reflectional symmetry Simple solutions of dynamo equation with In large Rm situation α and β should have turbulent values. i.e. independent of Rm Dynamo sets in at small, rather than large scales

7
Nonlinear effects: 2D diffusion Chicago 2003 In 2D induction equation becomes scalar transport equation With suitable boundary conditions we have In order to maintain turbulent behaviour as Rm gradients of A must diverge Generation of small scale fluctuations increases magnetic field energy Energetic constraint ~ u 2, gives estimate

8
Effect on velocity field Chicago 2003 Assume diffusive behaviour of large scale component of A

9
Back to α Chicago 2003 Possible problems with definition of α as a sensible statistical quantity as Rm Also possible problems with small-scale dynamo action. Look at simple case when B is uniform Assume large scale field is kinematic. Then in turbulent situation With b typically strongly non-Gaussian

10
Nonlinear effects Chicago 2003 Most nonlinear treatments rely on two statements –geometrical –dynamical Assume suitable boundaries Stationary, uniform mean field From EDQNM, say, get dynamical relationship

11
Nonlinear effects Chicago 2003 Combine to get saturation effects (as before)

12
Problems Chicago 2003 Three types of criticisms: Formula is incorrect –Agrees with DNS but only at small (moderate) Rm –The Sun does it stuff therefore it must be wrong Formula is correct but derivation is wrong/suspect –Assumptions about correlation time need justification –Second formula neglects intermittency (possibly strong in 3D) –Second formula just plain wrong Formula is correct but irrelevant (should not be used in physical models) –First formula neglects time dependence –First formula neglect large scale gradients –First formula assumes special boundary conditions (no flux of helicity)

13
Conclusion Chicago 2003 After about a decade controversy continues Is it likely to be settled by theoretical arguments alone? (Probably not) Can Center activity help resolve situation? –Better theories (Yeah right…) –More fancier simulations? (Possibly) –Experiments? (Possibly) What about β? Is it suppressed in 3D? What about non MHD-effects? –Hall effect –ambipolar diffusion

Similar presentations

© 2017 SlidePlayer.com Inc.

All rights reserved.

Ads by Google