Issue 
A&A
Volume 592, August 2016



Article Number  A73  
Number of page(s)  6  
Section  The Sun  
DOI  https://doi.org/10.1051/00046361/201527145  
Published online  28 July 2016 
The influence of helical background fields on current helicity and electromotive force of magnetoconvection
LeibnizInstitut für Astrophysik Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany
email: gruediger@aip.de; mkueker@aip.de
Received: 8 August 2015
Accepted: 29 April 2016
Motivated by the empirical finding that the known hemispheric rules for the current helicity at the solar surface are not strict, we demonstrate the excitation of smallscale current helicity by the influence of largescale helical magnetic background fields on nonrotating magnetoconvection. This is shown within a quasilinear analytic theory of driven turbulence and by nonlinear simulations of magnetoconvection that the resulting smallscale current helicity has the same sign as the largescale current helicity, while the ratio of both pseudoscalars is of the order of the magnetic Reynolds number of the convection. The same models do not provide finite values of the smallscale kinetic helicity. On the other hand, a turbulenceinduced electromotive force is produced including the diamagnetic pumping term, as well as the eddy diffusivity but, however, no α effect. It has thus been argued that the relations for the simultaneous existence of smallscale current helicity and α effect do not hold for the model of nonrotating magnetoconvection under consideration. Calculations for various values of the magnetic Prandtl number demonstrate that, for the considered diffusivities, the current helicity increases for growing magnetic Reynolds number, which is not true for the velocity of the diamagnetic pumping, which is in agreement with the results of the quasilinear analytical approximation.
Key words: magnetohydrodynamics (MHD) / magnetic fields / convection / Sun: activity
© ESO, 2016
1. Introduction
An increasing number of observations concerns the smallscale current helicity: (1)at the solar surface, all showing that it is negative (positive) in the northern (southern) hemisphere (Hale 1927; Seehafer 1990; Rust & Kumar 1994; Abramenko et al. 1996: Bao & Zhang 1998; Pevtsov 2001; Kleeorin et al. 2003; Zhang et al. 2010, 2012). Here the notation b denotes the fluctuating parts of the total magnetic field in the form . It became clear that the scalar quantity (1) shows a strict equatorial antisymmetry with signs which do not change from cycle to cycle. We note that for the linear α^{2} dynamo, as well as the simple αΩ dynamos, the largescale helicity, similar to (1), also shows equatorial antisymmetry in accordance with (Steenbeck & Krause 1969). The fact that for flux transport αΩ dynamos the relation is much more complicated (positive correlation only during the cycle minima) indicates that a direct relation does not necessarily exist. It is nevertheless important that all the mentioned scalars, such as helicities and α effect are pseudoscalars, which may be related to each other.
There are many theoretical studies where both the current helicity and the α effect are derived as consequences of the existence of the pseudoscalar g·Ω in rotating convection zones with g as the (radial) direction of stratification. Yet it is shown in this paper that the current helicity can also be produced, even without rotation, if the convection is influenced by a magnetic background field that is helical. Then the question is whether the same constellation would also lead to a turbulenceinduced electromotive force via an α effect as suggested by the relation (2)of Keinigs (1983). This is based on the existence of homogeneous and stationary turbulence with finite kinetic helicity (Seehafer 1996), where these conditions are obviously not fulfilled if one of the magnetic field components is inhomogeneous. Pouquet & Patterson (1978) presented the relation (3)which also means that even turbulent fluids with vanishing kinetic helicity, but finite smallscale current helicity, should possess an α effect but with an opposite sign as in Eq. (2).
Studies by Yousef et al. (2003), Blackman & Subramanian (2013) and Bhat et al. (2014) are concerned with the dissipation of helical and nonhelical largescale background fields under the influence of a nonhelical turbulent forcing. In these papers, it is shown that the kinetic helicity is dominated by the current helicity, which is confirmed by our quasilinear calculations for forced turbulence and the nonlinear simulations of magnetoconvection under the influence of a largescale helical field. In contradiction to the relation (3), both the quasilinear approximation and nonlinear simulations provide reasonable values for the current helicity, but they do not lead to a finite α effect.
2. The current helicity
To find the current helicity that is due to the interaction of a prescribed stochastic velocity u(x,t) and a large scale magnetic field it is sufficient to solve the induction equation (4)where the fluctuating magnetic field may be written as . The influence of field gradients on the mean current helicity (1) at linear order is governed by (5)where the prescribed inhomogeneous mean magnetic field has been introduced in the form with the notation and with B_{jj} = 0. It follows , which here may form the only pseudoscalar in the system.
To solve Eq. (5), we use the inhomogeneous Fourier modes (6)This is a standard procedure that yields (7)(Rüdiger 1975) from which the smallscale current helicity (8)can easily be formed. A homogeneous and isotropic turbulence field with the spectral tensor (9)may be postulated where the positive spectrum E gives the intensity of the fluctuations. After several manipulations, the final expression can be derived from (8) and (9) (10)which describes the induction by turbulence in a background field with helical geometry. As is necessary, the effect vanishes in the vacuum (η → ∞). In the highconductivity limit (η ≪ u_{rms}ℓ_{corr}), the integral in (10) only exists after multiplication with η so that (11)linearly scales with the magnetic Reynolds number Rm = u_{rms}ℓ_{corr}/η. Within the lowconductivity limit, as the opposite approximation, the smallscale current helicity scales with Rm^{2}, as does the normalized magnetic energy in the theory of Bräuer & Krause (1974).
With (11) the relation (3) would lead to (12)for the α effect in the highconductivity limit and for weak magnetic fields (Blackman & Brandenburg 2002; Brandenburg & Subramanian 2005).
With our approximations (quasilinear equations, forced turbulence, no rotation) the ratio of the two helicities corresponds to the ratio of both the magnetic energies. Equation (11) requires the same sign for the smallscale and the largescale current helicities. With (2), one finds which contradicts the above mentioned observations, which in the simple α^{2} dynamos . The only solution to this dilemma is that nonrotating convection under the influence of helical largescale fields may produce smallscale current helicity but it does not generate an α effect.
If calculated under the same analytical assumptions as the current helicity (1), the kinetic helicity ⟨ u·curl u ⟩ provides zero. Blackman & Subramanian (2013) find that during the turbulenceinduced decay of helical largescale fields the kinetic helicity remains unchanged. In the quasilinear approximation, the helicity expression, which is due to the background fields, also vanishes. magnetohydrodynamic (MHD) turbulence under the influence of a helical largescale field is thus suspected of generating finite values of current helicity but no kinetic helicity. The question is whether on this basis, and after the relations (2) and/or (3), nonlinear simulations of convection in a stratified plasma also generate current helicity but both the kinetic helicity and the α effect disappear.
In a previous paper we simulated magnetoconvection under the influence of a uniform vertical magnetic field to produce finite values of cross helicity (Rüdiger et al. 2012, Paper I hereafter). In this paper the helical magnetic background field (13)with uniform values of and has been applied as an initial field to probe the possible production of both smallscale kinetic and current helicity. In the computational layer, the vertical coordinate z runs from 0 to 2H, while the convection zone is located in [H,2H]. The value of the initial electric current is , hence the initial value of the largescale current helicity is .
The numerical value of developes during the simulation as the code also implicitly solves the meanfield equations (including the advection term discussed below). Also under the influence of the boundary conditions for the magnetic field, the helicity becomes depthdependent but its (positive) sign is always preserved. Averaged over the horizontal plane, the linear dependence of on the product is also numerically reproduced for the evolved largescale current helicity. In the bulk of the convection box the numerical values of the maxima of the latter are 70 for and 150 for .
Fig. 1
Snapshots of temperature (red lines) and density (blue lines) during the run for , . The values at the outer surface of the convective domain are fixed to unity. Here, as in all following images, the abscissae give z/H for the vertical coordinate varying from z = 0 to z = 2H with the convection domain reaching from z = H to z = 2H. 

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The compressible MHD equations have been solved with the nirvana code (Ziegler 2004) in a Cartesian box with gravitation along the negative zaxis. The box is periodic in the horizontal directions and all meanfield quantities are averaged over the horizontal plane. For the Prandtl number and the magnetic Prandtl number, a common value is fixed at 0.1. As in Paper I, the velocities are used in units of c_{ac}/ 100 where c_{ac} is the speed of sound at the top of the convection box (see Fig. 1). Correspondingly, the magnetic fields are given in units of with μ_{0} = 4π. We again assume an ideal, fully ionized gas heated from below and kept at a fixed temperature at the top of the simulation box. As in Paper I, the dimensionless Rayleigh number is fixed at 10^{7}. Periodic boundary conditions apply at the horizontal boundaries. The upper and lower boundary are perfect conductors so that for the total magnetic fields (14)which is similar to the stressfree conditions of the velocity, du_{x}/ dz = du_{y}/ dz = u_{z} = 0. At the inner boundary the heatflux is fixed. In Paper I, we find that for very weak magnetic fields the rmsvalue of the convection velocity in the used units is about 8 (see also the left panel of Fig. 2 below). This means that with the dimensionless η = 0.06 the global magnetic Reynolds number slightly exceeds 100, which is larger by definition than the local magnetic Reynolds number Rm = u_{rms}ℓ_{corr}/η introduced above.
We start to compute the intensities of the magnetoconvection and (Fig. 2). The velocity at the top of the convective box results in ≲10% of the surface value of the sound speed, which for the Sun is about 10 km s^{1}. The given time averages and vertical averages in z = [ 1,2 ] of all snapshots are taken as the characteristic values of the quantities. The differences of the velocity dispersion to those given in Paper I, where much weaker vertical fields have been applied, are very small. The magnetic quenching of the velocity fields does exist, but it is weak. However, the ratio is strongly affected by the mean magnetic field. While its value is about 30 for the vertical field , in Paper I the helical field only allows q values of order unity. We note also that , so that, with density values taken from Fig. 1, the convection is not magneticdominated. Contrary to that, we demonstrate that, nevertheless, the current helicity strongly dominates the kinetic helicity.
Fig. 2
Turbulenceintensities (left) and (right) for , . The numbers in the graphs are the volume averages of the coefficients over the whole convective domain. The averages over all blueline snapshots here and in all the plots below are indicated by solid red lines. 

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For the same model, the correlation coefficients, (15)for the kinetic helicity and the current helicity, have been computed (Fig. 3). The numerical values differ greatly. While the fluctuations of b and curl b are well correlated, this is not the case for the flow field.
Fig. 3
As in Fig. 2, but for the correlation coefficients c_{kin} (left) and c_{curr} (right). The numbers below the graphs are the volume averages of the coefficients over the whole convective domain. The average of all snapshots in both cases is below unity. 

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A systematic behavior of the zprofile also does not exist. In accordance with the analytic quasilinear calculations, magnetoconvection that is subject to helical background fields does not generate smallscale kinetic helicity, but it generates smallscale current helicity.
Fig. 4
Smallscale current helicity ⟨ b·curl b ⟩ the result of the largescale current helicity for , (left) and , (right). The numbers in the plots indicate the averages of all given snapshots in z = [ 1,2 ]. The stratified layer is convectively unstable on the righthand side of the vertical dashed line. 

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The behavior of the magnetoconvection complies with the above analytical result of the incapability of largescale helical fields to produce smallscale kinetic helicity from nonhelical turbulence, and this corresponds with the results of Blackman & Subramanian (2013) and Bhat et al. (2014), who find the helicities as magneticdominated in their simulations of decaying helical background fields under the influence of nonhelically driven turbulence.
After (11), we expect the current helicity numerical values to exceed , which is indeed confirmed by the simulations (Fig. 4). The average number in the right plot is just twice the number in the left plot, demonstrating the linear run of the correlation with the largescale helicity. The relation (11), which linearly connects the smallscale current helicity with the largescale current helicity, can thus be considered as being fulfilled by the numerical simulations. The numerical value between the two helicities and its relation to the magnetic Reynolds number is discussed below in Sect. 3.2.
3. The electromotive force
The same magnetoconvection model is used to calculate the turbulenceinduced electromotive force. As electric currents exist in the convection zone, this will certainly contain tensorial components of magnetic diffusion. The question is whether an electromotive force along the magnetic field also occurs, which must be interpreted as an α effect. Surprisingly, the answer is that no α effect is generated by the convection that is influenced by the helical magnetic background field (13). Since simultaneously current helicity without kinetic helicity exists, Eq. (3) cannot be correct for all possible turbulence fields.
The electromotive force ℰ = ⟨ u × b ⟩ in a turbulent plasma is a polar vector. To express linearly by the axial mean magnetic field vector , then only the formulation(16)is possible if pseudoscalars, such as g·Ω or , are not available. Without global rotation, an α effect in the formulation does not occur in the linear relation (16). The parameter η_{T} describes the turbulenceinduced eddy diffusivity in the fluid, while the vector γ gives a velocity which transports (“pumps”) the largescale magnetic field downward for positive γ_{z}. If, however, terms that are nonlinear in are included in the heuristic expression (16), then the extra terms(17)occur within the secondordercorrelation approximation (Kitchatinov et al. 1994). The first term of the right hand side represents the known magnetic influence on the eddy diffusivity, while the second one forms a magneticinduced pumping effect. There is no term representing an α effect with the largescale current helicity of the background field as (pseudoscalar) coefficient. For nonrotating and nonhelically driven turbulence, the largescale current helicity does not create an α effect in this approximation. Indeed, we do not find an α effect in the numerical simulations below. There is instead the – sometimes ignored – magneticinduced new pumping term, which for positive advects the magnetic field towards the maximum magnetic field. This effect should appear in all numerical models with helical largescale field and nonhelically driven flow (Yousef et al. 2003; Bhat et al. 2014).
Equations (16) and (17) yield(18)The nonlinear terms magnetically affect both the eddy diffusivity and the advection velocity, which are basically reduced if the factor (19)is positive. The possesses the dimension of a time and can be estimated as in the highconductivity limit. One easily finds for important cases. For ν = η, the coefficient is always positive for all spectral functions that do not grow with growing frequency. Moreover, for all Pm, the full expression (19) is positive for E ∝ δ(ω), which represents long correlation times as well as for E ≃ const, i.e.very short correlation times (socalled white noise). If compared with the magneticdiffusion time , the deltalike spectral line represents the lowconductivity limit, while the whitenoise spectrum represents the highconductivity limit. In both limits, the is positive and, therefore, both eddy diffusivity and diamagnetic pumping are magnetically quenched rather than amplified (“antiquenched”).
3.1. Numerical results
Fig. 5
Two horizontal components (top: ℰ_{x}, bottom: ℰ_{y}) of the turbulenceinduced electromotive force for background fields without helicity. Left panels: , (only homogeneous magnetic field in y direction); right panels: , (only homogeneous electric current in y direction). The averages over all snapshots are noted in the plots. 

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The two horizontal components of the electromotive force are calculated for two different cases. In the first simulation, the applied magnetic fields are assumed to be free of helicity, i.e. . The other possibility works with . If the results of both setups are identical, then the global helicity does not contribute to the electromotive force, as suggested by Eq. (17).
Let us first consider the two different helicityfree cases where, in the y direction, either only a field or only an electric current exists. Hence, for (20)Figure 5 (left) displays the resulting γ_{z} as positive (i.e. the flow is downwards) and of order γ_{z} ≃ 0.24 in units of c_{ac}/ 100 which, with c_{ac} ≃ 10 km s^{1} approximately^{1}, leads to a downward pumping of 20 m/s. The simulated electromotive force ℰ_{y} vanishes as required by (20).
The alternative example with yields ℰ_{x} = 0 and (21)Indeed, the numerically simulated ℰ_{x} vanishes while ℰ_{y} is negative (see Fig. 5, right).
In Fig. 6 the two components of the electromotive force are shown for a field with global helicity, i.e. . From (18) one finds(22)where the tildes mark the magnetically quenched values of the pumping velocity and the eddy diffusivity. The top panels of the plots only concern the advection velocity , which is always positive. It sinks from γ_{z} ≃ 0.42 to for B_{x} = 10 by the magnetic suppression. From the definition of , one immediately finds for the quenching coefficient (19) in units of 100H/c_{ac}. The code works with ρ_{0} = 1. We note that in all cases the numerical values of ⟨ u × b ⟩ are very small compared with the scalar product u_{rms} and b_{rms} given in Fig. 2. The resulting correlation coefficients here are very small.
The existence of an α effect in the expression (17) for the electromotive force would require a term . No such term resulted from the quasilinear approximation for the influence of helical largescale fields on nonhelically driven turbulence. This finding can be probed with numerical simulations. We note that three models in Figs. 5 and 6 are computed for constant B_{x} and for growing helicity (, 50, 100). If an α effect existed, we should find that the values of ℰ_{y} grow for growing helicity. The numerical results for the three models, however, are always identical. They do not show any numerical response to the growing helicities, which indicates that the nonexistence of an α term that is proportional to . The nonexistence of the α term in the electromotive force (17) in the quasilinear theory is thusconfirmed by nonlinear simulations.
Equation (22) enables us to derive the magnetic diffusivity from the simulations. By eliminating o from the definitions we find the relation . With the given mean values for all snapshots, the model with provides , so that η_{T} = 0.27 in units of Hc_{ac}/ 100 for the unquenched eddy diffusivity. Compared with the traditional estimate η_{T} ≃ (1 / 3)u_{rms}ℓ_{corr} we find the reasonable result ℓ_{corr} ≃ 0.1H in accordance direct inspections of the resulting convection patterns.
Fig. 6
As in Fig. 5, but for the helical background fields with , (left panels) and , (right panels). The averages over all snapshots are noted in the plots. 

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3.2. Variation of the magnetic Prandtl number
We still need to verify the analytical formulation (11) after which the ratio of the smallscale current helicity to the largescale helicity grows with the magnetic Reynolds number. This is certainly only true for large values of Rm (highconductivity limit). Large Rm require high values of the Reynolds number Re, and/or not too small Pm. It would be more realistic to increase the Reynolds number rather than the magnetic Prandtl number, but Re of order 10^{3} is the upper limit that is allowed by the technical restrictions.
So far the simulations were performed with a fixed magnetic Prandtl number Pm = 0.1. For fixed molecular viscosity its increase (decrease) by one order of magnitude effectively increases (decreases) the magnetic Reynolds number by a factor of ten. We expect a similar reaction of the smallscale current helicity (11). Because of Rm = Pm Re for a fixed Reynolds number, the magnetic Reynolds number runs with Pm.
The results for variations of the magnetic Prandtl number are shown by the plots in Fig. 7. From left to right the magnetic Prandtl number is reduced by a factor of 33. Also the current calculated helicity sinks (by a factor of about 17). The calculated helicity for Pm = 0.1 is 186 (see Fig. 4) and is thus wellsituated between the values for Pm = 0.03 and Pm = 1. The current helicity indeed runs with Rm, for which the plots of Fig. 4 in both cases yield values of about 20, which is indeed smaller than the global magnetic Reynolds number of order 100. Also the condition for the highconductivity limit as the basis of Eq. (11) can be considered as (approximately) fulfilled. Since in Paper I the resulting Rm for weaker fields were much higher, it is possible that, for the present models, the magnetic quenching effect already reduces the numerical values.
Fig. 7
ℋ_{curr} for for Pm = 1 (left) and Pm = 0.03 (right). 

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It is easy to verify this statement. It is known that the advection term γ_{z}, represented after (20) by , does not vary with Rm (see Kitchatinov et al. 1994). Hence, we do not expect a similar behavior as in Fig. 7 for the electromotive force ℰ_{x}. Indeed, Fig. 8 demonstrates that, for small Rm, the reduction of the magnetic Prandtl number by the factor of 33 leaves the electromotive force ℰ_{x} basically unchanged.
The results of Figs. 7 and 8 can also be understood as probing the inner consistency of the models and the numerical procedures. It is also shown that basic results of the quasilinear approximation are confirmed by simulations.
Fig. 8
As in Fig. 7 but for ℰ_{x}. A similar dependence on the magnetic Prandtl number as in Fig. 7 does not exist. 

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4. Conclusions
By analytical (quasilinear) theory and numerical simulations, it is shown that, in a nonrotating convective layer, a largescale helical magnetic background field produces a smallscale current helicity, while the kinetic helicity vanishes. The current helicity possesses the same sign as the helicity of the largescale field. The ratio of both pseudoscalars runs with the magnetic Reynolds number of the convection. The same magnetic model provides finite values of the diamagnetic pumping term γ and the eddy diffusivity η_{T}, but an α effect does not occur in the same order.
If it is true that the α effect in the stellar convection zones is due to the action of the Coriolis force on the turbulent convection, then it is positive (negative) on the northern (southern) hemisphere, which according to Eq. (2) would lead to the opposite signs for the smallscale current helicity – as is indeed observed as dominating during the activity cycle. The new effect of the smallscale current helicity that is due to the influence of a largescale field combined with a parallel electric current yields opposite signs. During the minimum phase of the solar activity cycle only these signs sometimes occur. Zhang et al. (2010) give
the approximative value 10^{5} G^{2}/cm for the observed smallscale current helicity. With the radial scale of 100 Mm and with G^{2}, one only needs a magnetic Reynolds number Rm of the fluctuations of order 10 to fulfill the numerical constraints.
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All Figures
Fig. 1
Snapshots of temperature (red lines) and density (blue lines) during the run for , . The values at the outer surface of the convective domain are fixed to unity. Here, as in all following images, the abscissae give z/H for the vertical coordinate varying from z = 0 to z = 2H with the convection domain reaching from z = H to z = 2H. 

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In the text 
Fig. 2
Turbulenceintensities (left) and (right) for , . The numbers in the graphs are the volume averages of the coefficients over the whole convective domain. The averages over all blueline snapshots here and in all the plots below are indicated by solid red lines. 

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In the text 
Fig. 3
As in Fig. 2, but for the correlation coefficients c_{kin} (left) and c_{curr} (right). The numbers below the graphs are the volume averages of the coefficients over the whole convective domain. The average of all snapshots in both cases is below unity. 

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In the text 
Fig. 4
Smallscale current helicity ⟨ b·curl b ⟩ the result of the largescale current helicity for , (left) and , (right). The numbers in the plots indicate the averages of all given snapshots in z = [ 1,2 ]. The stratified layer is convectively unstable on the righthand side of the vertical dashed line. 

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In the text 
Fig. 5
Two horizontal components (top: ℰ_{x}, bottom: ℰ_{y}) of the turbulenceinduced electromotive force for background fields without helicity. Left panels: , (only homogeneous magnetic field in y direction); right panels: , (only homogeneous electric current in y direction). The averages over all snapshots are noted in the plots. 

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In the text 
Fig. 6
As in Fig. 5, but for the helical background fields with , (left panels) and , (right panels). The averages over all snapshots are noted in the plots. 

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In the text 
Fig. 7
ℋ_{curr} for for Pm = 1 (left) and Pm = 0.03 (right). 

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In the text 
Fig. 8
As in Fig. 7 but for ℰ_{x}. A similar dependence on the magnetic Prandtl number as in Fig. 7 does not exist. 

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In the text 
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