Issue 
A&A
Volume 495, Number 1, February III 2009



Page(s)  1  8  
Section  Astrophysical processes  
DOI  https://doi.org/10.1051/00046361:200810359  
Published online  11 December 2008 
Alpha effect and diffusivity in helical turbulence with shear
D. Mitra^{1}  P. J. Käpylä^{2}  R. Tavakol^{1}  A. Brandenburg^{3}
1  Astronomy unit, School of Mathematical Sciences, Queen Mary University of London,
Mile End Road, London E1 4NS, UK
2 
Observatory, Tähtitorninmäki (PO Box 14), 00014
University of Helsinki, Finland
3 
NORDITA, Roslagstullsbacken 23, 10691 Stockholm, Sweden
Received 10 June 2008 / Accepted 28 November 2008
Abstract
Aims. We study the dependence of turbulent transport coefficients, such as the components of the tensor (
)
and the turbulent magnetic diffusivity tensor (), on shear and magnetic Reynolds number in the presence of helical forcing.
Methods. We use threedimensional direct numerical simulations with periodic boundary conditions and measure the turbulent transport coefficients using the kinematic test field method. In all cases the magnetic Prandtl number is taken as unity.
Results. We find that with increasing shear the diagonal components of
quench, whereas those of
increase. The antisymmetric parts of both tensors increase with increasing shear. We also propose a simple expression for the turbulent pumping velocity (or effect). This pumping velocity is proportional to the kinetic helicity of the turbulence and the vorticity of the mean flow. For negative helicity, i.e. for a positive trace of
,
it points in the direction of the mean vorticity, i.e. perpendicular to the plane of the shear flow. Our simulations support this expression for low shear and magnetic Reynolds number. The transport coefficients depend on the wavenumber of the mean flow in a Lorentzian fashion, just as for nonshearing turbulence.
Key words: magnetohydrodynamics (MHD)  hydrodynamics  turbulence  magnetic fields
1 Introduction
Understanding the origin of nonuniform largescale magnetic fields in stars, galaxies, and accretion discs continues to pose important challenges. Such fields are commonly thought to be the result of dynamo action that converts the kinetic energy of turbulent motions and largescale shear into magnetic energy. The usual framework for studying such dynamo actions is mean field electrodynamics (e.g. Krause & Rädler 1980). Over the years, however, the applicability of this framework has been questioned (Piddington 1981; Vainshtein & Cattaneo 1992). In particular, an important debate in this connection revolves around the role played by magnetic helicity (Gruzinov & Diamond 1994). Magnetic helicity is conserved for ideal (nondissipative) magnetohydrodynamics (MHD) and also in the limit of large magnetic Reynolds numbers. This conservation places severe constraints on the growth of the mean magnetic field and may regulate the quenching of the effect as the magnetic Reynolds number ( ) increases (Brandenburg & Subramanian 2005). Under certain circumstances (no magnetic helicity fluxes), quenching becomes more severe with proportional to . It has been suggested that this can be alleviated by expelling magnetic helicity through open boundaries (Kleeorin et al. 2000; Blackman & Field 2000), possibly mediated by shear (Subramanian & Brandenburg 2004; Vishniac & Cho 2001; Brandenburg & Sandin 2004). Furthermore, shear itself is an important ingredient in MHD dynamos in solar and stellar settings as, for example, in the solar tachocline. Hence, it is important to understand how shear affects the turbulent transport coefficients, in particular the components of the and tensors.Several studies have recently looked at various aspects of this problem (see, e.g., Rüdiger & Kitchatinov 2006; Rogachevskii & Kleeorin 2003,2004; Brandenburg 2005; Leprovost & Kim 2008; Rädler & Stepanov 2006;Brandenburg et al. 2008a). These works employ different tools and make different assumptions and are often applicable to limited regions of the parameter space. As a consequence, care must be taken in comparing these results. For example, using semianalytical tools, which treat the nonlinear Lorentz force feedback perturbatively, Leprovost & Kim (2008) have found that shear can reduce in helically forced turbulence. This is analogous to the ``rotational quenching'' of turbulent transport coefficients with increasing Coriolis or inverse Rossby numbers (Kitchatinov et al. 1994; Pipin et al. 1996). There are also other related cases in which the presence of shear enhances the growth rate of the dynamo. For example; using direct numerical simulations of the MHD equations in the presence of shear and nonhelical forcing, Yousef et al. (2008a,b) have found largescale dynamos whose growth rate increases linearly with shear. Such scaling has also been found for shear dynamos where the effect is due to stratified convection with shear (Käpylä et al. 2008a). Furthermore, using the kinematic test field method (described below), Brandenburg et al. (2008a) have studied the dynamo coefficients in the presence of shear, but in the absence of helicity, and they find that Gaussian fluctuations of about zero are strong enough to drive an incoherent shear dynamo (Vishniac & Brandenburg 1997; Proctor 2007). The significance of the incoherent effect has also been stressed by Hughes & Proctor (2009), although their system may have also had a net effect. They dismissed this on the grounds that for an imposed uniform magnetic field is very small. However, this result disagrees with recent calculations of using the test field method (Käpylä et al. 2008b).
In this paper we use threedimensional direct numerical simulations of the kinematic test field equations with helical forcing in order to study the dependence of turbulent transport coefficients on shear and magnetic Reynolds number. In Sect. 2 we give a brief account of our model. Section 3 contains our results and finally we conclude in Sect. 4.
2 The model
We use the test field method (Schrinner et al. 2005,2007) to calculate the turbulent transport coefficients. This method and its modification in the presence of largescale shear are described in Brandenburg et al. (2008a). Here we just point out the essence of the method and elaborate only on those aspects where our treatment differs from their paper.
In the presence of largescale shear, the equations of magnetohydrodynamics
are treated in the following way. Writing the velocity as the
sum
,
where the largescale shear
velocity
with a constant shear S,
and assuming an isothermal equation of state characterised by the sound
speed ,
the momentum equation becomes
Here is the viscous force, is the traceless rate of strain tensor (not to be confused with the shear parameter S), is the kinematic viscosity, is the fluid density, is the isothermal sound speed and
(2) 
As our external forcing we employ helical, whiteintime, random forcing described in Brandenburg (2001). In this paper we consider the purely kinematic problem, so there is no feedback in Eq. (1) due to the Lorentz force. In addition to the momentum equation, we have the continuity equation
and the uncurled induction equation in the Weyl gauge,
Here the magnetic field is , the current density is , and and are the vacuum permeability and the molecular magnetic diffusivity, respectively. In the mean field approach to MHD one usually decomposes the magnetic field (or magnetic vector potential) and velocity into mean (indicated by an overbar) and fluctuating parts respectively
The equations satisfied by the mean and fluctuating parts of the magnetic vector potential are given by
and
where and is the mean turbulent electromotive force. Specification of this second order quantity in terms of the mean field constitutes a closure problem. A common procedure is to expand in terms of the mean field and its derivatives,
where and are the tensorial turbulent transport coefficients, and quantifies additional contributions that arise even in the absence of a mean field, owing to smallscale dynamo action, for example. Here and throughout, summation is assumed over repeated indices. In the test field method we take the mean magnetic field to be a given ``test field'' , and calculate these tensors by measuring by solving Eq. (7) simultaneously with Eqs. (1) and (3), while using Eq. (5) to find . In order to find all the components of the and tensors, and not just projections relevant to the actual fields, one has to use an orthogonal set of test fields and solve Eq. (7) for each of them.
In our simulations we employ averages over x and
y directions to define our mean fields, which are therefore functions
of z and t only. Thus, all other components
of
except
and
vanish, and the
and
tensors can be written as rank two tensors
with
and
for i,j=(1,2)(Brandenburg et al. 2008a). Now consider, as an example, the following two test fields,
which we use to compute the two corresponding mean electromotive forces and . The relevant components of the and tensors are then given by
(11) 
The rest of the 2+2 components of the and tensors can be similarly determined by using the test fields,
In what follows we denote a test field by , where p=c,s and q=1,2. A particular smallscale magnetic vector potential that develops in response to the is denoted by and the corresponding smallscale magnetic field is given by . Note that at large values of there will also be smallscale dynamo action that will lead to spurious timedependencies of . However, since neither the test fields nor or depend on time, i.e.
such time dependence must be entirely due to and can be eliminated by time averaging.
Figure 1: Rootmeansquare velocity normalized by the speed of sound as: a) a function of for different values of : respectively and b) a function of the shear parameter for different value of : (), (), and (). 

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In the following we shall, to begin with, use k=k_{1}, the wavenumber corresponding to the box size, to study the dependence of and on shear and magnetic Reynolds number. We shall discuss the dependence of the and tensors on k in Sect. 3.3. Note that the usual approach of using uniform applied fields for calculating (e.g., Courvoisier et al. 2006) corresponds to a special case of the test field method for k=0. However, dynamos generate largescale fields with nonzero k, so it is important to relax this restriction. It is then also important to calculate . The test field method allows the simultaneous calculation of all the components of the and tensors for arbitrary values of k.
The test field method has recently been criticised by Cattaneo & Hughes (2008) on the grounds that the test fields are arbitrary predetermined mean fields. They argue that the resulting turbulent transport coefficients will only be approximations to the true values unless the test fields are close to the actual mean fields  a criticism equally applicable to other methods using arbitrary uniform fields. This concern has been addressed by Tilgner & Brandenburg (2008), who argue that Eq. (7) can instead be applied to any mean field. This statement has been numerically verified in three cases that we describe below.
Firstly, the test field method correctly reproduces a vanishing growth rate in saturated nonlinear cases (Brandenburg et al. 2008b). Secondly, in the timedependent case, the test field method correctly reproduces also a nonvanishing growth rate, but in that case it is no longer permissible to express in terms of a multiplication of turbulent transport coefficients with the mean field and its spatial derivatives. One must therefore write Eq. (8) as a convolution in time (Hubbard & Brandenburg 2008). Finally, the success of the test field method becomes particularly clear when it is applied to a passive vector field that obeys a separate induction equation with a velocity field from a saturated dynamo (Tilgner & Brandenburg 2008). This question was originally posed by Cattaneo & Tobias (2008). In particular for the Roberts flow with a mean field of Beltrami type, e.g. one that is proportional to , the tensor is anisotropic and has an additional component proportional to that tends to quench the components of the isotropic part of . The fastest growing passive vector field is then proportional to . This result has been confirmed both numerically and using weakly nonlinear theory (Tilgner & Brandenburg 2008).
In the following we ignore the complications involving timedependent
mean fields and restrict ourselves
to transport coefficients that apply strictly speaking only to the
timeindependent or marginally excited case.
For our numerical simulations we use the
PENCIL CODE^{},
where the test field algorithm has already been implemented.
All our numerical simulations are performed in a periodic cubic box.
The forcing scale is chosen to have the wavenumber
.
This gives enough scale separation for a largescale field to develop
(Haugen et al. 2004), and is still not too big to reduce the resulting
Reynolds numbers too much.
We use units such that
and arrange the forcing amplitude
so that the Mach number is around 0.1.
For the magnetic Prandtl number we choose
,
where lies
in the range
to
(in units of
).
We choose the shear S such that the parameter
(14) 
takes values in the range 0.02 to 0.9, where is the rootmeansquare velocity. All the runs are started with uniform density, , , and . Depending upon the parameters of a particular run we use up to 256^{3} grid points. For each test field we calculate the time averages of the and tensors over time intervals over which is statistically stationary. In runs with higher magnetic Reynolds numbers,
(15) 
we obtain an exponential growth of smallscale magnetic field (see below). We interpret this as being associated with the term. This often gives rise to large fluctuations in all components of the and tensors at late times. In such cases we confine our calculations of the time averages to time intervals over which does not exceed by more than a factor of about 20. Up until this point, the components of the and tensors show only their intrinsic fluctuations, but at later times these will be swamped by additional contributions from the smallscale dynamo that grows exponentially in time. If necessary, we repeat our calculations over several independent realizations by resetting at regular time intervals.
3 Results
Our principal aim in this paper is to study the effects of varying shear () and magnetic Reynolds number ( ) on the components of the and tensors. In the subsection below we summarize our results concerning the different components of these tensors.
3.1 Diagonal components of the transport tensors
The isotropic parts of the
and tensors are respectively characterised as
where denotes an average taken over z and t. We normalize these quantities by and which are their respective expressions obtained using the First Order Smoothing Approximation (FOSA) for , which has previously been confirmed with the test field method in simulations of helical turbulence without shear (Sur et al. 2008).
Since enters the normalization of and , it is useful to first look at how it changes as a function of (Fig. 1a) and (Fig. 1b). As can be seen, increases as a function of for small and then reaches a plateau for high . On the other hand, is almost a constant as a function of shear except for high , where we observe excitation of the vorticity dynamo discussed further in Sect. 3.4.
In Fig. 2 we show as a function of shear for three different values of the magnetic Reynolds number and 72. Figure 2b shows the corresponding results for . We note that for small shear the turbulent transport coefficients are close to their values for zero shear. As increases, decreases and increases up to four times . As can be seen there is a clear reduction (quenching) of with increasing shear in all these cases. In order to examine the possible convergence of the results with we plot and as functions of for three different values of the shear parameter , see Fig. 3. For small we observe an increase in both and with . A similar initial increase of and was also seen in earlier simulations of helical turbulence without shear (Sur et al. 2008) and in nonhelical shear flow turbulence (Brandenburg et al. 2008a). For higher values of and , both and show large variations. In these kinematic simulations, however, we expect them to tend to constant values asymptotically at high (Sur et al. 2008).
Figure 2: Turbulent transport coefficients a) and b) as functions of shear parameter for different values of : (), (), and (). 

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Figure 3: a) and b) as functions of , for different values of : , and respectively. Horizontal dashed lines at and are added to facilitate comparison. 

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In an earlier study of shear flow turbulence with nonhelical forcing by
Brandenburg et al. (2008a), the diagonal components of
were
found to be the same.
Obviously, in the absence of helicity
all the components of
are zero.
It turns out that in the presence of helicity the two diagonal components
of
are still the same, but those of
are now
nonzero and not equal to each other.
This is best shown by considering the quantities
The results are shown in Fig. 4. Note that especially for large values of the values of are predominantly negative. Since both and are negative, this means that is larger than , although the relative difference is only of the order of at most 5 per cent.
Figure 4: Normalized a) and b) , as defined in Eq. (17), as functions of for constant value of the shear parameter : , and respectively. Horizontal dashed lines are added to facilitate comparison. 

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Figure 5: Normalized offdiagonal components of the and tensors as functions of the shear parameter for different values of : (), (), and (). Horizontal dashed lines are added to facilitate comparison. 

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Figure 6: Normalized offdiagonal components of the and tensors as functions of for constant values of : . Horizontal dashed lines are added to facilitate comparison. 

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3.2 Offdiagonal components
We now consider the offdiagonal components of
and .
The results are depicted in Figs. 5 and 6.
Of particular interest among these is the component ,
whose dependence on
and
is shown
in Figs. 5d and 6d, respectively.
This component can indicate the possible presence of a
shearcurrent dynamo that may operate when
(Rogachevskii & Kleeorin 2003,2004). Here
is the total
(sum of turbulent and microscopic) magnetic diffusivity.
In our case we have S < 0,
which implies that the necessary condition for the shearcurrent dynamo
to operate is
.
As can be seen from Fig. 6d,
for the range of
values considered here
is positive for
small shear but becomes negative for strong shear and certain values of
.
Earlier work of Brandenburg et al. (2008a) without helicity did indicate a similar
sign change, although only for larger
.
However, the error bars were so large that
this result could not be regarded as significant.
For the run with the strongest shear (
)
and for
we now find
to be more clearly negative, but for smaller
and larger values of
the results are again, at least within
error bars, compatible with zero.
Also, of course, the present results apply to the case with helicity
and are therefore not really comparable with those of Brandenburg et al. (2008a),
where the helicity is zero.
The antisymmetric contributions to the
and
tensors
are characterised by the vectors
(18) 
Since our averages depend only on z, the z components of these tensors are irrelevant and therefore only the z components of the and vectors are of interest. We denote those simply by and , with
A time series of both quantities is shown in Fig. 7 for positive and negative signs of the kinetic helicity. The results show that, in our case with S<0, is positive (negative) for positive (negative) kinetic helicity, whilst has always the same sign.
Figure 7: Normalized time series of turbulent transport coefficients, a) , b) , c) and d) , from two runs with exactly the same parameters ( , ), but different signs of helicity for the external force. Continuous and broken lines denote results from runs with positive and negative helicities, respectively. 

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Some idea about the functional forms of
and
can be
obtained from symmetry considerations.
The vectors
and
enter the electromotive force
thus
(20) 
so we see that must be a polar vector and must be an axial vector. Using the shear flow , the only axial vector that can be constructed is the mean vorticity, , so we expect to have a component that is proportional to . Likewise, since is a polar vector which points in the direction of , the two must be related via a pseudoscalar. In the present case the only pseudoscalar available is the kinetic helicity, . Based on these symmetry arguments we write
where we have introduced two nondimensional quantities, and which could be either positive or negative, and is a correlation time that we approximate here by
(22) 
In the present case, itself is a negative multiple of . We therefore expect to have a component proportional to , multiplied by the correlation time . By similar arguments we expect to have a component proportional to , multiplied by . Based on these arguments we can also write
with new nondimensional quantities, and , that we expect to be of order unity. Our simulations confirm this reasoning and show that both coefficients are of order unity with positive and negative (e.g., and for the run shown in Fig. 8) for runs with small and ; see Figs. 8 and 9, respectively. The sign in Eq. (23) has been chosen a posteriori from our simulations. For high shear and Reynolds number this simple reasoning is no longer accurate and, at least in one case (Fig. 9a), even becomes negative. For lower values of we find an almost constant negative of the order of (or less). This result is fairly independent of . The moduli of and increase with increasing shear parameter, and for larger values of both quantities may approach an asymptotic value. For small we observe a roughly linear increase of with shear (see inset of Fig 8a), further verifying Eq. (21).
The coefficient can be interpreted as turbulent pumping, i.e. advection of the magnetic field by means other than the mean velocity field. In strongly stratified convection, turbulent pumping has been seen to be directed from higher to lower turbulence intensity (Käpylä et al. 2006; Tobias et al. 1998; Ossendrijver et al. 2002; Tobias et al. 2001), which is usually in the downward direction. Thus, turbulent pumping is likely to play an important role in convection zones of stars where it can overcome the buoyancy of the magnetic field. In the present case where the turbulence is homogeneous, however, stratification does not play a role and the pumping is just due to the combined action of shear and helical turbulence.
Figure 8: Normalized a) and b) as functions of for (), (), and (). Horizontal dashed lines are added to facilitate comparison. The inset shows versus for . 

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Figure 9: Normalized a) and b) as functions of for constant values of the shear parameter : . Horizontal dashed lines are added to facilitate comparison. 

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3.3 Scaledependence
So far we have confined the calculations of the and tensors to test fields whose characteristic length scale is the largest scale in the domain, i.e., test fields of the form or with k=k_{1}, where and L is the box size of our simulations. We have also done similar calculations for other values of k, which correspond to test fields with different characteristic length scales. In Fig. 10 we show the dependence of and on k for . The decrease can be modelled by a Lorentzian peaked at k=0 (Fig. 10). This result is not surprising, because Lorentzian fits have been obtained earlier also in the absence of shear (Brandenburg et al. 2008c).Figure 10: a) and b) as a function of the wavenumber k of the largescale magnetic field for . The solid lines show the Lorentzian fits of width 1.4 . 

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Figure 11: Panel a) shows the rootmeansquare values of the velocity for one of our runs (with and ) which exhibits a vorticity dynamo. The inset shows the timeseries for . Panel b) shows a pronounced pattern in U_{y} on the periphery of the box at the end of the same run. Similar structures are also found in the x component of the velocity. 

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3.4 Effects from the vorticity dynamo
In the runs with relatively high values of shear and Reynolds number, the rootmeansquare velocity, , which initially reaches a steady state, shows an exponential growth at late times, as can be seen in Fig. 11a. Similar behaviour is seen for turbulent transport coefficients, which also show large fluctuations for later times. Large fluctuations of the turbulent transport coefficients at later times are also seen by Sur et al. (2008), but those fluctuations are more irregular and have a different origin. They are interpreted as being due to the development of a smallscale dynamo at late times and are not due to the more systematic increase in the rms velocity, which in turn is associated with the shear. However, we emphasize that even before becomes dominated by this type of dynamo action, the temporal and spatial fluctuations of and are of the order of and , respectively. This is true even for large values of ; see Brandenburg et al. (2008a), who have argued that these fluctuations also contribute to largescale dynamo action via the incoherent effect (Vishniac & Brandenburg 1997; Proctor 2007). For example, the timeseries of shown in the inset of Fig. 11 has a plateau even beyond the range over which is steady.The vertical spikes in the inset of Fig. 11 come from resetting to zero in regular time intervals; see the end of Sect. 2. Note, however, that the mean values and also the upper envelope trace the evolution of reasonably well, including the increased rise after t=300. The late time behaviour is accompanied by the formation of largescale vortical structures, as seen in Fig. 11b, which is a signature of the vorticity dynamo proposed by Elperin et al. (2003), see also Yousef et al. (2008a,b). A detailed numerical study of the vorticity dynamo has been performed by Käpylä et al. (2008).
The presence of the vorticity dynamo and the resulting systematic variation in as well as the turbulent transport coefficients for late times limit the lengths of time over which average values of the components of the and tensors can be calculated. In the above case this interval lies between the two arrows in Fig. 11a. This limits the range of and that we have probed and explains the larger error bars shown for example in Fig. 6, and why they cannot be reduced by simply running our simulations for longer times. This problem would be avoided in the presence of magnetic fields, because then the resulting Lorentz force would quench the vorticity dynamo (Käpylä & Brandenburg 2008). This is however beyond the scope of this paper.
4 Conclusions
We have studied the effects of varying shear and magnetic Reynolds number on the turbulent transport coefficients in the presence of helicity in the kinematic limit. We have shown that for fixed , is reduced (quenched) with increasing shear. Despite the differences in the assumptions made, this quenching is qualitatively similar to the recent results obtained by Leprovost & Kim (2008). To the best of our knowledge this is the first numerical study to show quenching of as a function of shear in helical turbulence. We find that increases with increasing shear in the range of values that we have considered here. A similar behaviour for was also seen in Brandenburg et al. (2008a) where the forcing was nonhelical.
We also compute the offdiagonal components of the and tensors. The antisymmetric part of corresponds to a turbulent pumping velocity in the direction perpendicular to the plane of the shear flow. It shows a roughly linear increase with shear for small magnetic Reynolds number. We propose simple expressions for and in Eq. (21) which show reasonable agreement with our numerical results for small and . Our expression shows that for negative helicity, points in the direction of the vorticity of the mean flow. Regarding the component we find indications that, at least in one or two cases, this component changes sign and becomes negative. This could be of significance in connection with the shearcurrent effect.
We also find that all the turbulent transport coefficients depend on the wavenumber of the mean flow in a Lorentzian fashion, just as in the case of nonshearing turbulence (Brandenburg et al. 2008c). This means that the kinematic values of and for k=k_{1} are close to the values obtained for . This is not the case for certain nonturbulent flows such as the GallowayProctor flow (Rädler & Brandenburg 2009; Courvoisier 2008). In an earlier paper, Courvoisier et al. (2006) considered only the limiting case k=0 for this flow.
Several aspects of the present investigations could be of astrophysical relevance. Turbulence in celestial bodies is helical and exhibits an effect. In addition, shear (S) can be an important ingredient in that the efficiency of largescale dynamo action is determined by the product of and S. However, as S increases, itself becomes quenched when Sbecomes comparable with the inverse turnover time, i.e. . Furthermore, the turbulent diffusivity becomes enhanced, suppressing the dynamo even further. Finally, it is found that the combined action of helicity and shear gives rise to a pumping velocity of mean magnetic field perpendicular to the plane of the shear flow. The existence of such a pumping velocity has not been emphasized before. On the other hand, it is well known that (or rather ) dynamos can have travelling wave solutions (Brandenburg et al. 2001). When the product of and S is positive, these waves travel in the positive z direction, which agrees with the direction of pumping. In the nearsurface shear layer of the Sun this pumping would therefore support the equatorward migration in that layer.
It is important to understand the quenching of turbulent transport coefficients in the presence of shear beyond the kinematic approximation. In that case one needs to include the induction equation (in addition to the test field equations) and incorporate the resulting Lorentz force in the momentum equation (Brandenburg et al. 2008b). This would also help in alleviating problems of strong latetime fluctuations arising from the vorticity dynamo, because the vorticity dynamo tends to be suppressed by magnetic fields of equipartition strengths (Käpylä & Brandenburg 2008). Similarly, given their potential importance in allowing the escape of magnetic helicity, the effects of open boundary conditions also needs to be considered. These questions are under study and will be reported elsewhere.
Acknowledgements
The authors acknowledge the hospitality of Nordita during the programme ``Turbulence and Dynamos''. A.B. and P.J.K. thank Astronomy Unit, Queen Mary University of London, for hospitality. Computational resources were granted by CSC (Espoo, Finland), UKMHD, and QMUL HPC facilities purchased under the SRIF initiative. This work was supported by the the Leverhulme Trust (DM, RT), the Academy of Finland grant No. 121431 (PJK), and the Swedish Research Council (AB).
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Footnotes
All Figures
Figure 1: Rootmeansquare velocity normalized by the speed of sound as: a) a function of for different values of : respectively and b) a function of the shear parameter for different value of : (), (), and (). 

Open with DEXTER  
In the text 
Figure 2: Turbulent transport coefficients a) and b) as functions of shear parameter for different values of : (), (), and (). 

Open with DEXTER  
In the text 
Figure 3: a) and b) as functions of , for different values of : , and respectively. Horizontal dashed lines at and are added to facilitate comparison. 

Open with DEXTER  
In the text 
Figure 4: Normalized a) and b) , as defined in Eq. (17), as functions of for constant value of the shear parameter : , and respectively. Horizontal dashed lines are added to facilitate comparison. 

Open with DEXTER  
In the text 
Figure 5: Normalized offdiagonal components of the and tensors as functions of the shear parameter for different values of : (), (), and (). Horizontal dashed lines are added to facilitate comparison. 

Open with DEXTER  
In the text 
Figure 6: Normalized offdiagonal components of the and tensors as functions of for constant values of : . Horizontal dashed lines are added to facilitate comparison. 

Open with DEXTER  
In the text 
Figure 7: Normalized time series of turbulent transport coefficients, a) , b) , c) and d) , from two runs with exactly the same parameters ( , ), but different signs of helicity for the external force. Continuous and broken lines denote results from runs with positive and negative helicities, respectively. 

Open with DEXTER  
In the text 
Figure 8: Normalized a) and b) as functions of for (), (), and (). Horizontal dashed lines are added to facilitate comparison. The inset shows versus for . 

Open with DEXTER  
In the text 
Figure 9: Normalized a) and b) as functions of for constant values of the shear parameter : . Horizontal dashed lines are added to facilitate comparison. 

Open with DEXTER  
In the text 
Figure 10: a) and b) as a function of the wavenumber k of the largescale magnetic field for . The solid lines show the Lorentzian fits of width 1.4 . 

Open with DEXTER  
In the text 
Figure 11: Panel a) shows the rootmeansquare values of the velocity for one of our runs (with and ) which exhibits a vorticity dynamo. The inset shows the timeseries for . Panel b) shows a pronounced pattern in U_{y} on the periphery of the box at the end of the same run. Similar structures are also found in the x component of the velocity. 

Open with DEXTER  
In the text 
Copyright ESO 2009
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