The dynamo-generated magnetic field will, in general, produce a Lorentz force that will tend to oppose the driving fluid motions. This is a basic physical effect that should be included in any dynamo model. It is not at all trivial to do so, however, since in a turbulent environment both the fluctuating and mean components of the magnetic field can affect both the large-scale flow components, as well as the small-scale turbulent flow providing the Reynolds stresses powering the large-scale flows. One can thus distinguish a number of (related) amplitude-limiting mechanisms:

- Lorentz force associated with the mean magnetic field directly affecting large-scale flow (sometimes called the “Malkus-Proctor effect”, after the groudbreaking numerical investigations of Malkus and Proctor (1975)).
- Large-scale magnetic field indirectly affecting large-scale flow via effects on small-scale turbulence and associated Reynolds stresses (sometimes called “-quenching”, see, e.g., Kitchatinov and Rüdiger, 1993).
- Maxwell stresses of small-scale magnetic field directly or indirectly affecting large-scale flow.

The -quenching formulae introduced in Section 4.2.1 is a particularly simple - some would say simplistic -
way to model the backreaction of the magnetic field on the turbulent fluid motions producing the
-effect^{11}.
In the context of solar cycle models, one could also expect the Lorentz force to reduce the amplitude of differential
rotation until the effective dynamo number falls back to its critical value, at which point the dynamo again
saturates^{12}.
The third class of quenching mechanism listed above has not yet been investigated in detail, but numerical
simulations of MHD turbulence indicate that the effects of the small-scale turbulent magnetic field on the
-effect can be profound (see Pouquet et al., 1976; Durney et al., 1993).
Introducing magnetic backreaction on differential rotation is a tricky business, because one must then
also, in principle, provide a model for the Reynolds stresses powering the large-scale flows in the solar
convective envelope (see, e.g., Kitchatinov and Rüdiger, 1993), as well as a procedure for computing
magnetic backreaction on these. This rapidly leads into the unyielding realm of MHD turbulence,
although algebraic “-quenching” formulae akin to -quenching have been proposed based on
specific turbulence models (see, e.g., Kitchatinov et al., 1994). Alternately, one can add an ad
hoc source term to the right hand side of Equation (2), designed in such a way that in the
absence of the magnetic field, the desired solar-like large-scale flow is obtained. As a variation on
this theme, one can simply divide the large-scale flow into two components, the first ()
corresponding to some prescribed, steady profile, and the second () to a time-dependent flow field
driven by the Lorentz force (see, e.g., Tobias, 1997; Moss and Brooke, 2000; Thelen, 2000b):

The majority of studies published thus far and using this approach have only considered the nonlinear magnetic backreaction on differential rotation. This has been shown to lead to a variety of behaviors, including amplitude and parity modulation, periodic or aperiodic, as well as intermittency (more on the latter in Section 5.6). Knobloch et al. (1998) have argued that amplitude modulation in such models can be divided into two main classes. Type-I modulation corresponds to a nonlinear interaction between modes of different parity, with the Lorenz force-mediated flow variations controlling the transition from one mode to another. Type-II modulation refers to an exchange of energy between a single dynamo mode (of some fixed parity) with the flow field. This leads to quasiperiodic modulation of the basic cycle, with the modulation period controlled by the magnetic Prandtl number. Both types of modulation can co-exists in a given dynamo model, leading to a rich overall dynamical behavior.

Figure 20 shows two butterfly diagrams produced by the nonlinear mean-field interface model of Tobias (1997) (see also Beer et al., 1998). The model is defined on a Cartesian slab with a reference differential rotation varying only with depth, and includes backreaction on the differential rotation according to the procedure described above. The model exhibits strong, quasi-periodic modulation of the basic cycle, leading to epochs of strongly reduced amplitude. Note how the dynamo can emerge from such epochs with strong hemispheric asymmetries (top panel), or with a different parity (bottom panel).

The differential rotation can also be suppressed indirectly by magnetic backreaction on the small-scale turbulent flows that produce the Reynolds stresses driving the large-scale mean flow. Inclusion of this so-called “-quenching” in mean-field dynamo models, alone or in conjunction with other amplitude-limiting nonlinearities, has also been shown to lead to a variety of periodic and aperiodic amplitude modulations, provided the magnetic Prandtl number is small (see Küker et al., 1999; Pipin, 1999). This type of models stand or fall with the turbulence model they use to compute the various mean-field coefficients, and it is not yet clear which aspects of the results are truly generic to -quenching.

To date, dynamical backreaction on large-scale flows has only been studied in dynamo models based on mean-field electrodynamics. Equivalent studies must be carried out in the other classes of solar cycle models discussed in Section 4. In particular, it is essential to estimate the effect of the Lorentz force on meridional circulation in models based on the Babcock-Leighton mechanism and/or hydrodynamical instabilities in the tachocline, since in these models the circulation is the primary determinant of the cycle period and enforces equatorward propagation in the butterfly diagram. Even though meridional circulation in the convective envelope is a “weak” flow, in the sense of being much slower than differential rotation, it arises from a small imbalance between forces that are in themselves quite large; the importance of magnetically-mediated backreaction on meridional circulation is likely to be a complex affair.

A number of authors have attempted to bypass the shortcomings of -quenching by introducing into dynamo models an additional, physically-inspired partial differential equation for the -coefficient itself (e.g., Kleeorin et al., 1995; Blackman and Brandenburg, 2002, and references therein). The basic physical idea is that magnetic helicity must be conserved in the high- regime, so that production of helicity in the mean field implies a corresponding production of helicity of opposite sign at the scales of the fluctuating components of the flow and field, which ends up acting in such a way as to reduce the -effect. Most investigations published to date have made used of severely truncated models, and/or models in one spatial dimensions (see, e.g., Weiss et al., 1984; Schmalz and Stix, 1991; Jenning and Weiss, 1991; Roald and Thomas, 1997; Covas et al., 1997; Blackman and Brandenburg, 2002), so that the model results can only be compared to solar data in some general qualitative sense. Rich dynamical behavior definitely arises in such models, including multiperiodicity, amplitude modulation, and chaos.

Covas et al. (1998) have incorporated dynamical -quenching into a two-dimensional spherical axisymmetric mean-field dynamo model, and compared the resulting behavior to that produced by classical algebraic -quenching. These authors found, perhaps not surprisingly, both quantitative and qualitative differences between solutions computed using dynamical rather than algebraic -quenching, with the nonlinear behavior in the former case depending sensitively on model parameters, so it is not clear which class of models can be considered “more realistic”.

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