348 research outputs found
Suppression of the large-scale Lorentz force by turbulence
The components of the total stress tensor (Reynolds stress plus Maxwell
stress) are computed within the quasilinear approximation for a driven
turbulence influenced by a large-scale magnetic background field. The
conducting fluid has an arbitrary magnetic Prandtl number and the turbulence
without the background field is assumed as homogeneous and isotropic with a
free Strouhal number St. The total large-scale magnetic tension is always
reduced by the turbulence with the possibility of a `catastrophic quenching'
for large magnetic Reynolds number Rm so that even its sign is reversed. The
total magnetic pressure is enhanced by turbulence with short correlation time
(`white noise') but it is reduced by turbulence with long correlation time.
Also in this case the sign of the total pressure may reverse but only for
special turbulences with sufficiently large St> 1.
The turbulence-induced terms of the stress tensor are suppressed by strong
magnetic fields. For the tension term this quenching grows with the square of
the Hartmann number of the magnetic field. For microscopic (i.e. small)
diffusivity values the magnetic tension term becomes thus highly quenched even
for field amplitudes much smaller than their equipartition value. In the
opposite case of large-eddy simulations the magnetic quenching is only mild but
then also the turbulence-induced Maxwell tensor components for weak fields
remain rather small.Comment: 7 pages, 5 figures, submitted to Astron. Nach
The negative magnetic pressure effect in stratified turbulence
While the rising flux tube paradigm is an elegant theory, its basic
assumptions, thin flux tubes at the bottom of the convection zone with field
strengths two orders of magnitude above equipartition, remain numerically
unverified at best. As such, in recent years the idea of a formation of
sunspots near the top of the convection zone has generated some interest. The
presence of turbulence can strongly enhance diffusive transport mechanisms,
leading to an effective transport coefficient formalism in the mean-field
formulation. The question is what happens to these coefficients when the
turbulence becomes anisotropic due to a strong large-scale mean magnetic field.
It has been noted in the past that this anisotropy can also lead to highly
non-diffusive behaviour. In the present work we investigate the formation of
large-scale magnetic structures as a result of a negative contribution of
turbulence to the large-scale effective magnetic pressure in the presence of
stratification. In direct numerical simulations of forced turbulence in a
stratified box, we verify the existence of this effect. This phenomenon can
cause formation of large-scale magnetic structures even from initially uniform
large-scale magnetic field.Comment: 5 pages, 2 figures, submitted conference proceedings IAU symposium
273 "Physics of Sun and Star Spots
Magnetic Helicity Evolution During the Solar Activity Cycle: Observations and Dynamo Theory
We study a simple model for the solar dynamo in the framework of the Parker
migratory dynamo, with a nonlinear dynamo saturation mechanism based on
magnetic helicity conservation arguments. We find a parameter range in which
the model demonstrates a cyclic behaviour with properties similar to that of
Parker dynamo with the simplest form of algebraic alpha-quenching. We compare
the nonlinear current helicity evolution in this model with data for the
current helicity evolution obtained during 10 years of observations at the
Huairou Solar Station of China. On one hand, our simulated data demonstrate
behaviour comparable with the observed phenomenology, provided that a suitable
set of governing dynamo parameters is chosen. On the other hand, the
observational data are shown to be rich enough to reject some other sets of
governing parameters. We conclude that, in spite of the very preliminary state
of the observations and the crude nature of the model, the idea of using
observational data to constrain our ideas concerning magnetic field generation
in the framework of the solar dynamo appears promising.Comment: 10 pages, 3 Postscript figures, uses aa.cl
The dynamics of Wolf numbers based on nonlinear dynamo with magnetic helicity: comparisons with observations
We investigate the dynamics of solar activity using a nonlinear
one-dimensional dynamo model and a phenomenological equation for the evolution
of Wolf numbers. This system of equations is solved numerically. We take into
account the algebraic and dynamic nonlinearities of the alpha effect. The
dynamic nonlinearity is related to the evolution of a small-scale magnetic
helicity, and it leads to a complicated behavior of solar activity. The
evolution equation for the Wolf number is based on a mechanism of formation of
magnetic spots as a result of the negative effective magnetic pressure
instability (NEMPI). This phenomenon was predicted 25 years ago and has been
investigated intensively in recent years through direct numerical simulations
and mean-field simulations. The evolution equation for the Wolf number includes
the production and decay of sunspots. Comparison between the results of
numerical simulations and observational data of Wolf numbers shows a 70 %
correlation over all intervals of observation (about 270 years). We determine
the dependence of the maximum value of the Wolf number versus the period of the
cycle and the asymmetry of the solar cycles versus the amplitude of the cycle.
These dependencies are in good agreement with observations.Comment: 9 pages, 13 figures, final revised paper for MNRA
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