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# Magnetic field stretching at the top of the shell of numerical dynamos

*Earth, Planets and Space*
**volume 68**, Article number: 78 (2016)

## Abstract

The process of magnetic field stretching transfers kinetic energy to magnetic energy and by that maintains dynamos against Ohmic dissipation. Stretching at the top of the outer core may play an important role at specific regions. High-latitude intense magnetic flux patches may be concentrated by flow convergence. Reversed flux patches may emerge due to expulsion of toroidal field advected to the core–mantle boundary by fluid upwelling. Here we analyze snapshots from self-consistent 3D numerical dynamos to unravel the nature of field–flow interactions that induces stretching secular variation at the top of the core. We find that stretching at the top of the shell has a significant influence on the secular variation despite the relatively weak poloidal flow. In addition, locally stretching is often more effective than advection in particular at regions of significant field-aligned flow. Magnetic flux patches are concentrated by fluid downwelling and dispersed by fluid upwelling. Stretching is more efficient than advection in intensifying magnetic flux patches. Both stretching and the poloidal flow mostly depend on the magnetic Prandtl number *Pm*. Decreasing *Pm* gives smaller poloidal flow but stronger stretching. Accounting for field–flow interactions in both the advection and stretching terms suggests that the magnetic Reynolds number overestimates the actual ratio of magnetic advection to diffusion by ∼50 %. Morphological resemblance between local stretching in our dynamo models and local observed geomagnetic secular variation may suggest the presence of stretching at the top of the Earth’s core. Our results shed light on the kinematic origin of intense geomagnetic flux patches and may have implications to the convective state of the upper outer core.

## Introduction

The geomagnetic field is generated by convective motions of an electrically conductive fluid in Earth’s rapidly rotating liquid outer core. The field is measured by surface magnetic observatories and dedicated satellites. Geomagnetic measurements are inverted for spherical harmonic models which can be downward continued to the top of the region of field generation, i.e., the core–mantle boundary (CMB). Temporal changes in the geomagnetic field termed secular variation (SV) provide vital insight into the fluid dynamics and dynamo action at the top of the core. Indeed, geomagnetic field and SV models (e.g., Jackson et al. 2000; Olsen and Mandea 2008) have been used as constraints on numerical dynamo simulations (e.g., Christensen et al. 1998, 2010; Aubert et al. 2013) or to infer various aspects of Earth’s core dynamics (e.g., Finlay and Jackson 2003), in particular the fluid flow just below the CMB (for a review, see Holme 2007).

According to dynamo theory, the SV is comprised of magnetic advection, stretching and diffusion. Magnetic field advection transfers magnetic energy from one degree to another, whereas magnetic field stretching transfers kinetic energy to magnetic energy and by that maintains dynamos against Ohmic dissipation (e.g., Moffatt 1978; Mininni 2011). Therefore, magnetic field stretching is responsible for dynamo action. Better understanding of the field–flow interactions that yield magnetic field stretching is therefore fundamental for dynamo theory. Of course dynamo action might not necessarily occur at the entire outer core. For example, the dynamo may be deep seated due to stable stratification at the top of core, as was argued for Mercury (Christensen 2006) and for the Earth (Pozzo et al. 2012; Gubbins and Davies 2013). Here, however, we focus on the CMB, for comparison with geomagnetic field and SV models inferred from observations.

Fluid dynamics systems are often characterized by non-dimensional numbers. These numbers give valuable physical intuition concerning the relative importance of different processes in the system, for example the dominant force acting on the fluid and the role of turbulence. However, calculations of dynamo-related non-dimensional numbers using typical scales and ignoring field–flow interactions might provide non-representative values. Finlay and Amit (2011) calculated various alternative magnetic Reynolds numbers *Rm* that took into account different length scales of core dynamics. They extrapolated SV spectra to obtain an advective length scale; inferences from numerical dynamos (Amit and Christensen 2008) and from expansion of reversed flux patches (Chulliat and Olsen 2010) were used to infer a diffusive length scale. Finlay and Amit (2011) focused on magnetic field advection and ignored magnetic field stretching. It is important to re-evaluate non-dimensional numbers in order to better understand core dynamics in light of field–flow interactions and accounting for magnetic stretching effects.

Global criteria for characterizing the observed geomagnetic field (Christensen et al. 2010) are practical because the field spectrum is decreasing with degree (most energy at largest scale, i.e., dipole). In contrast, the geomagnetic SV spectrum is increasing with degree, which is a problem for global characterization. Some SV features like westward drift (Finlay and Jackson 2003) or Pacific/Atlantic dichotomy (Christensen and Olson 2003) could be related to external forcings such as gravitational coupling between the inner core and the mantle (Aubert et al. 2013) or core–mantle thermal interactions (Holme et al. 2011) rather than core convection itself. Alternatively, geomagnetic SV may be locally studied. Robust geomagnetic field features such as intense normal and reversed flux patches have a particular signature on the SV. Local analysis of field–flow interactions may provide a detailed interpretation of the SV in the vicinity of these robust field features.

Stretching may play an important role in specific regions of the CMB, such as high-latitude intense geomagnetic flux patches. These robust non-axisymmetric features typically reside near the edge of the inner core tangent cylinder (Jackson et al. 2000), possibly due to flow convergence at these latitudes (Olson et al. 1999). In rapidly rotating numerical dynamo models surface convergence is correlated with columnar cyclones (Olson et al. 2002; Amit et al. 2007), so the flow near these patches has a large field-aligned component and produces little magnetic advection (Finlay and Amit 2011). Regardless of whether the locations of downwellings are directly related to a thermal mantle anomaly (Gubbins 2003) or to the chaotic time-dependent buoyancy at the top of the core, the kinematic relation between concentrated magnetic flux and fluid downwelling is expected from the stretching term in the radial magnetic induction equation.

Magnetic field stretching may also be the underlying mechanism for regions of weak field intensity at Earth’s surface. Striking deviations of the geomagnetic field from axial dipolarity appear in the form of reversed flux patches, i.e., regions on the CMB where the sign of the radial field is opposite to that of the axial dipole field. In the past century, the most intense and extensive reversed flux patches have been growing and intensifying at the southern Atlantic of the CMB (e.g., Jackson et al. 2000; Olsen et al. 2014). At Earth’s surface these structures are expressed as a notably low-intensity zone termed the South Atlantic Magnetic Anomaly (Hartmann and Pacca 2009). The field intensity at this region is at present decreasing at rates of up to 12 % over the past 30 years (Finlay et al. 2010), much faster than the decline of the geomagnetic dipole moment (Olson and Amit 2006; Finlay 2008). It has been proposed that reversed flux patches emerge due to expulsion of toroidal field (Bloxham 1986) which is transported to the CMB by fluid upwelling (e.g., Aubert et al. 2008a).

It is under debate whether any stretching effects prevail at the top of Earth’s core. Seismic studies (Helffrich and Kaneshima 2010) and revised estimates of large core thermal conductivity from mineral physics calculations (Pozzo et al. 2012; Koker et al. 2012) suggest that the top of the core is stably stratified (Gubbins and Davies 2013). This may indicate that the flow just below the CMB is purely toroidal and no stretching SV is present there, although the radial flow may penetrate a stably stratified layer, e.g., if the convection columns are large enough (Takehiro and Lister 2001) or in the presence of certain waves (Buffett 2014). Low geomagnetic SV at special points where the radial field gradient is zero also supports stable stratification (Whaler 1980), but uncertainty in their exact locations renders such an interpretation questionable (Whaler and Holme 2007). In contrast, Zhang et al. (2015) claimed that the thermal conductivity is as low as previously estimated and thus the whole of the outer core convects. Regional interpretations of the geomagnetic SV also favor some local upwelling/downwelling (Olson and Aurnou 1999; Chulliat et al. 2010; Amit 2014).

Global core flow models inverted from the geomagnetic SV can be constructed with and without poloidal flow (Holme 2007). Based on various theoretical arguments, most models assume some relation between the toroidal and poloidal flows. In particular, quasi-geostrophic models rely on poloidal flow to project CMB flows to the volume of the core (Pais and Jault 2008; Gillet et al. 2009). Lesur et al. (2015) inverted geomagnetic data simultaneously for the field and the core flow. When a purely toroidal flow was incorporated in the inversion the data could not be adequately fitted, in contradiction to upper core stratification. However, inclusion of weak poloidal flow was sufficient to explain the SV. Lesur et al. (2015) concluded that the upper core is weakly stratified.

In this paper, we analyze output from self-consistent 3D numerical dynamos to unravel the nature of field–flow interactions and the contribution of magnetic field stretching to the SV at the top of the spherical shell. Analytical and statistical tools are designed to quantify these kinematic processes. We zoom-in to specific regions on the outer boundary to explore the kinematic origins of intense normal and reversed magnetic flux patches. The dependence of the results on the dynamo control parameters is explored. The results are discussed in the context of geomagnetic field and SV models.

## Methods

### Numerical dynamo models

Fluid motions in Earth’s outer core are governed by the magnetohydrodynamics equations: Navier–Stokes, magnetic induction, conservation of energy and mass (continuity for an incompressible fluid). In non-dimensional form these equations can be written (e.g., Olson et al. 1999) as follows:

where \(\vec {u}\) is the fluid velocity, \(\vec {B}\) is the magnetic field, *T* is temperature (or more generally co-density), *t* is time, \(\hat{z}\) is a unit vector in the direction of the rotation axis, *P* is pressure, \(\vec {r}\) is the position vector, \(r_{\text {o}}\) is the core radius, and \(\epsilon \) is heat (or buoyancy) source or sink. The magnetic field changes in time [first term in (2)] due to its generation by the fluid flow [second term in (2)] and its destruction (or magnetic diffusion) due to the finite electrical conductivity of the outer core fluid [third term in (2)]. In return the flow varies in time [first term in (1)] due to all the forces acting on it, including the magnetic Lorentz force [last term in (1)].

Four non-dimensional parameters in (1)–(3) control the dynamo action. The heat flux Rayleigh number (Olson and Christensen 2002) represents the strength of buoyancy force driving the convection relative to retarding forces

where \(\alpha \) is thermal expansivity, \(g_{\text {o}}\) is gravitational acceleration on the outer boundary at radius \(r_{\text {o}}\), \(q_{\text {o}}\) is the mean heat flux across the outer boundary, *D* is shell thickness, *k* is thermal conductivity, \(\kappa \) is thermal diffusivity, and \(\nu \) is kinematic viscosity. The Ekman number represents the ratio of viscous and Coriolis forces

where \(\varOmega \) is the rotation rate. The Prandtl number is the ratio of kinematic viscosity to thermal diffusivity

and the magnetic Prandtl number is the ratio of kinematic viscosity to magnetic diffusivity \(\lambda \)

The condition for dynamo action is that the magnetic field generation term will sufficiently exceed the diffusion term in (2). The scaled ratio between these two terms is given by the magnetic Reynolds number

where *U* is a typical velocity scale.

Numerical dynamos provide self-consistent solutions to the full set of Eqs. (1)–(5) in a spherical shell (Christensen and Wicht 2007). We used the numerical implementation MagIC (Wicht 2002). Due to computational limitations, dynamo simulations use control parameters very far from Earth-like conditions, and therefore, relating the results to the real core conditions is challenging. Our chosen control parameters (Table 1) are even more moderate than what modern computers are capable of. The reason is that smaller *E* values produce such small-scale structures that the local relations between the field and the flow would become difficult to interpret. We focus on dynamos in the non-reversing dipole-dominated regime (e.g., Kutzner and Christensen 2002; Christensen and Aubert 2006).

The shell geometry is identical to Earth’s core with an inner to outer boundary radii ratio of 0.35. The inner and outer boundaries of the shell are set to be insulating and rigid. To simulate generic thermochemical convection (e.g., Aubert et al. 2008b), on the inner core boundary fixed co-density is set, on the outer boundary fixed heat flux is prescribed, and the source/sink term in (3) is set to \(\epsilon =0\). The number of radial grid points \(N_r\) is chosen to accommodate at least five grid points across the Ekman boundary layer. In our models, \(N_r\) varies from 49 for the larger \(E=1 \times 10^{-3}\) cases to 61 for the lower \(E=1 \times 10^{-4}\) cases. Horizontal resolution is also increased with decreasing Ekman number, from maximum degree and order \(\ell _{\text {max}}=64\) for the \(E=1 \times 10^{-3}\) cases to \(\ell _{\text{ max }}=96\) for the \(E=1 \times 10^{-4}\) cases.

It is of particular interest to examine the radial component of the induction equation just below the outer boundary, because only the radial component of the geomagnetic field at the CMB is accessible from observations. The radial component of (2) at the top of the shell where the radial velocity vanishes is

where \(B_{r}\) is the radial field, \(\vec {u}_{h}\) is the 2D velocity vector tangent to the spherical surface, \(\nabla _{h}=\nabla -\dfrac{\partial }{\partial r}\), and *r* is the radial coordinate. The first term in (11) is the SV, the second term represents magnetic field advection, the third term represents magnetic field stretching, and the term on the right-hand side denotes magnetic diffusion.

The frozen-flux theory (Roberts and Scott 1965) assumes that the majority of SV on short timescales and large length scales is produced by the advection and stretching action due to the velocity field rather than diffusion of the magnetic field. Based on the observed SV and inferences from mineral physics experiments Rm ∼ 500 in Earth’s outer core (e.g., Bloxham and Jackson 1991), supporting the frozen-flux hypothesis. Under this assumption (11) simplifies to

This equation is the common starting point for modeling the flow at the core surface (e.g., Holme 2007). It is termed the frozen-flux induction equation, because accordingly magnetic field lines are simply carried by the flow.

The radial magnetic field \(B_r\) and the tangential velocity \(\vec {u}_h\) were taken at the top of the free stream (just below the Ekman boundary layer) to analyze the different terms of the radial induction equation. Note that in the dynamo models at the top of the free stream the radial velocity is more than an order of magnitude smaller than the tangential velocity hence (11) holds. In order to obtain statistics of the dynamical characteristics of the simulations, for each dynamo model ten snapshots were taken at arbitrary times enough separated so that their structures are non-correlated. Overall, 90 snapshots were globally analyzed, of which more than 350 zoom-ins to local regions of intense magnetic flux patches were selected.

### Statistical measures

We calculate several statistical properties to analyze the results, including global and local RMS ratios (\(\left\| X\right\| /\left\| Y\right\| \)) and spatial correlations corr(*X*, *Y*) between *X* and *Y*. The RMS \(\left\| X\right\| \) is obtained by integration of *X* over the spherical surface at the top of the free stream. We compute the ratio of RMS stretching to RMS advection St/Ad as well as the ratio of RMS poloidal flow to RMS toroidal flow \({\mathcal {P}}/{\mathcal {T}}\). We also calculate the spatial correlation coefficient between tangential divergence \(\delta _h \equiv \nabla _h \cdot {\vec u_h}\) and plus/minus radial vorticity \(\omega _r \equiv \hat{r} {\cdot } \nabla \times {\vec u}\) (where \(\hat{r}\) is the radial unit vector) in the Northern/Southern Hemisphere, respectively, termed helical flow by Amit and Olson (2004)

where \(\theta \) is co-latitude. The correlation coefficient between the absolute radial field and downwelling is \({\text{ corr}}(|B_r|,\delta _h^-)\) with \(\delta _h^-\) defined by

Likewise, the correlation coefficient between absolute radial field and upwelling is \({\text{corr}}(|B_r|,\delta _h^+)\) with \(\delta _h^+\) defined by

Local analyses are classified by polarity, i.e., normal or reversed, and by latitude. High latitudes are arbitrarily defined by patches that are centered at higher than 45° latitude. Classified this way, four types of patches are possible: normal polarity at high latitudes (HN), normal polarity at low latitudes (LN), reversed polarity at high latitudes (HR) and reversed polarity at low latitudes (LR). In addition, normalized integrated values allow evaluation of level of cancellation in a given region

where *f* is the studied quantity in a region *S* and \({\text {d}}S=r^2 \sin \theta {\text {d}}\phi {\text {d}}\theta \) is a spherical surface increment. If all advection has the same sign in a region then \(\xi _{\text {a}}=1\), whereas if the advection has alternating signs of equal amount then \(\xi _{\text {a}}=0\). The same type of interpretation holds for the stretching efficiency \(\xi _{\text {s}}\). In order to test whether the stretching intensifies or weakens the magnetic flux, the normalized integrated value of their product is evaluated:

If the stretching SV and \(B_{r}\) have the same sign (i.e., field intensification by stretching) then \(\xi _{\text {e}}>0\), whereas if \(\xi _{\text {e}}<0\) then stretching has an opposite sign to \(B_{r}\) and it therefore locally weakens the field.

Next we estimate an effective magnetic Reynolds number that accounts for field–flow interactions. For the advective part, following Finlay and Amit (2011) we calculate the angle \(\gamma \) between the vectors \(\vec {u}_h\) and \(\nabla _h B_r\) so that \((\pi /2-\gamma )\) is the angle between a \(B_r\)-contour and the core surface flow \(\vec {u}_h\). The level of field-aligned flow is represented by

If the field and the flow are perfectly aligned then \(\gamma =\pi /2\) and advection is zero, whereas if the flow is perpendicular to \(B_r\)-contours then \(\gamma =0\) and advection efficiency is optimal. Accordingly, the effective advective magnetic Reynolds number \(Rm_{\text {a}}\) is then

The effective stretching magnetic Reynolds number \(Rm_{\text {s}}\) is simply

In order to combine \(Rm_{\text {a}}\) and \(Rm_{\text {s}}\) the correlation between the two SV contributions should be accounted for. We therefore compute the interaction between the two terms by

If St and Ad are correlated then \(\xi _{Rm}=1\). If St and Ad are non-correlated then \(\xi _{Rm}=\sqrt{1+c^2}/(1+c)\) where *c* is their amplitude ratio. In this case a minimum of \(\xi _{Rm}=\sqrt{2}/2\) is obtained for \(c=1\) (i.e., equal advection and stretching amplitudes). Finally, if St and Ad are anti-correlated then \(\xi _{Rm}=|-1+c|/(1+c)\). In this case for \(c=1\)
\(\xi _{Rm}=0\), i.e., advection and stretching cancel each other to yield zero inductive SV. The effective magnetic Reynolds number is then given by

To get some intuition to the quantities \(\cos \gamma \) and \(\xi _{Rm}\) we report their values for some large-scale synthetic cases. For the radial field, we use a dipole with present-day Earth-like tilt (Olsen et al. 2014) and for the flow we use large-scale degree-1 toroidal and poloidal flows (Table 2). Obviously for the toroidal flows stretching is zero and \(\xi _{Rm}=1\). Because the dipole field is dominantly axial, the most effective advection scenario (i.e., largest \(\cos \gamma \)) occurs when the flow is oriented north-south (\({\mathcal {P}}_1^0\)). Overall the two quantities \(\cos \gamma \) and \(\xi _{Rm}\) are clearly distinctive with either one larger for different cases.

Finally, we examine the dependence of the statistical quantities on the non-dimensional control parameters of the dynamo models. Each quantity (St/Ad, \({\mathcal {P}}/{\mathcal {T}}\), \(H_u\), etc.) may be expressed as a generic power law:

where *f* is the statistical quantity and *C*, *a*, *b*, *c* are fitting coefficients. The relative misfit \(\sigma _r\) of the power law is given by

where \(f^{\text {dyn}}\) is the statistical quantity obtained from the dynamo models and *n* is the number of dynamo models analyzed. Relative misfits larger than an arbitrary threshold value of 0.07 were considered inadequate, and in these cases, the fits were not interpreted.

The power law fits (23) obtained by the misfit minimization (24) are applied to time-average statistical quantities. The time-dependence is expressed by the standard deviation (Tables 3, 4). Note that the standard deviation was not used to assess the fits.

This paper contains many variables. While some are conventional, others were introduced to denote newly defined properties. For clarity we list in the “Appendix” all the variables used in this paper.

## Results

### Kinematics of intense magnetic flux patches

Figure 1 shows an arbitrary snapshot from dynamo model 4. As in all models considered in this study, the radial magnetic field on the outer boundary exhibits axial dipole dominance (Fig. 1a). The tangential divergence \(\delta _h\) is highly correlated with the radial vorticity \(\omega _r\) in the Southern Hemisphere and highly anti-correlated in the Northern Hemisphere (Fig. 1c, d). The toroidal flow dominates over the poloidal flow at the top of the free stream (\({\mathcal {P}}/{\mathcal {T}}<1\)). Nevertheless globally, the stretching contribution to the frozen-flux SV is larger than that of advection (Fig. 1e, f). Intense magnetic flux patches present positive and negative correlations with downwelling and upwelling structures, respectively. Because our dynamo models are dominated by the axial dipole, most of the intense flux patches are obviously of normal polarity at high latitudes (HN) and only a few are normal (LN) and reversed (LR) at low latitudes. The flux patches are rather large scale and are significantly more intense than their surroundings.

Figure 2 shows a typical intense high-latitude normal polarity (HN) magnetic flux patch (see upper polygon in Fig. 1a). This patch is located close to the center of an anti-clockwise vortex (Fig. 2a, c) that is highly correlated with a downwelling structure (Fig. 2d). The flow in this region is predominately toroidal. The main part of the flow is aligned with the \(B_r\)-contours (Fig. 2a), causing non-efficient advection (Fig. 2e). In contrast, the high correlation between the magnetic flux patch and the downwelling structure produces a strong stretching SV (Fig. 2f) that locally intensifies the magnetic field with an efficiency of \(\xi _{\text {e}}=0.94\). Consequently, the local stretching SV is remarkably twice larger than advective SV.

Another HN (lower polygon in Fig. 1a) is located west of a strong southward flow (Fig. 3a). This flow system produces an intense advective SV at the eastern part of the patch. In the western part, the flow and hence the advection are weak. Despite the relatively weak poloidal flow, the downwelling structure shown in Fig. 3d produces intense stretching SV (Fig. 3f). In this patch, the stretching SV is only slightly larger than advective SV, but it is still able to locally intensify the magnetic field with an efficiency of \(\xi _{\text {e}}=0.87\).

Overall we found three types of intense magnetic flux patches (out of the four possible types): Most of them are high-latitude normal polarity flux patches (HN), whereas a smaller number are low-latitude normal polarity (LN) and low-latitude reversed polarity (LR). Reversed flux patches at high latitudes (RH) are rare. The same holds for all the dynamo models examined here. From hereafter we therefore report local analyses of HN, LN and LR only.

Next we examine a dynamo model with a larger *Ra*, and otherwise all parameters unchanged (Table 1). Figure 4 shows an arbitrary snapshot from dynamo model 6. As in model 4, the radial magnetic field has the characteristic axial dipolar dominance and the flow is predominantly toroidal. The global correlation of radial vorticity and tangential divergence is again high. Intense magnetic flux patches are positively correlated with downwelling structures and negatively with upwelling structures. However, the field and flow features are smaller scale and advection is globally stronger than stretching.

Figure 5 shows an intense high-latitude normal polarity flux patch (lower polygon in Fig. 4a). This HN is at the center of a clockwise vortex correlated with a downwelling structure (Fig. 5c, d). A large part of the flow is field aligned, so advection is confined to a region close to the patch center (Fig. 5a, e). The interaction of the downwelling structure with the intense flux patch on the northern part produces a strong stretching structure (Fig. 5f), but some shift in the southern part leads to moderate St/Ad RMS ratio. The stretching and advective contributions to the SV are comparable despite the relatively weak poloidal flow.

Next we analyze an LR (upper polygon in Fig. 4a). The southward flow is roughly perpendicular to the \(B_r\)-contours (Fig. 6a), producing a strong advective SV (Fig. 6e). The downwelling structure in Fig. 6d is well correlated with this reversed flux patch, and hence the stretching structure shown in Fig. 6f also presents an important contribution to the SV. In contrast, stretching locally intensifies the magnetic field with a smaller efficiency than in the HN (Fig. 5). In addition, the poloidal flow is relatively larger than in HN.

Dynamo model 9 (Fig. 7) has lower *E* and larger *Ra* resulting in larger *Rm* (Table 1) and a more complex behavior. As in previous models, the flow is predominately toroidal and tangential divergence and radial vorticity correlation is high. However, the magnetic flux patches in this model are small scale and a larger number of them appear at low latitudes (Table 3). The main contribution to the SV is advective.

Figure 8 shows an HN (upper polygon in Fig. 7a) from dynamo model 9. This patch is at the center of an anti-clockwise vortex (Fig. 8a) related to a downwelling structure (Fig. 8d). Advection is effective at the peak of the patch (see Fig. 8e). In contrast, the downwelling structure exhibits a phase shift with the \(B_r\) patch resulting in a weak stretching (Fig. 8f) and thus an advective dominant SV.

In dynamo model 9 some intense normal polarity flux patches appear at low latitudes (LN). Figure 9 shows an LN (lower polygon in Fig. 7a). This patch is located west of an anti-clockwise vortex correlated with an upwelling structure (Fig. 9d). A large component of the flow is perpendicular to the \(B_r\)-contours and consequently, the advective SV efficiency is high. Stretching is less efficient due to the phase shift between the downwelling structure (Fig. 9d) and the intense flux patch. In this low-latitude intense flux patch, the stretching locally intensifies the magnetic field with an efficiency of \(\xi _{\text {e}}=0.88\).

Table 3 summarizes the global statistics of all snapshots from each dynamo simulation, while Table 4 summarizes the local statistics per patch type. In all models, both globally and for the patches, absolute magnetic flux is positively/negatively correlated with downwelling/upwelling, respectively. The best global correlation of absolute magnetic flux and downwelling is obtained in dynamo model 9 (Table 3). In dynamo model 4 for HN and LN the flux to downwelling correlations are highest, while LR has the best flux to downwelling correlation in dynamo model 3 (Table 4).

### Parameters dependence

In order to examine more quantitatively the dependence of the statistical measures on the non-dimensional control parameters, we used a generic power law (23). The fitting parameters *C*, *a*, *b* and *c* were calculated using a conventional least-squared fit. Power law fits were applied for global and local measures.

The best fit for the global St/Ad ratio is given by

with a relative misfit of \(\sigma _r=0.063\). In (25) the *E* and *Ra* powers are comparable, which motivates the following approximation:

The best fit of (26) is

with \(\sigma _r=0.063\). Then (27) could be approximated in logarithmic scale as

Figure 10a confirms the similarity between the \(-0.152\) slope of the fitted linear curve and the approximated power of \(-\frac{1}{6}\) in (28). The parameter dependence of the global St/Ad is thus given by

Considering the modified Rayleigh number \(Ra'=\frac{E \cdot Ra}{Pr}\) (e.g., Olson et al. 1999), and \(Pr=1\), Eq. (29) could be written as

Globally, relative stretching in the dynamo models increases with increasing rotation (decreasing *E*), but decreases when convection (*Ra*) and electrical conductivity (*Pm*) increase. The dependence is strongest on *Pm* (30).

We followed a similar fitting process for the St/Ad ratio of HN. The parameter dependence of St/Ad of HN is given by (Fig. 10b)

In qualitative agreement with the global case (Fig. 10a), relative stretching increases with rotation, but decreases when convection and electrical conductivity increase. In high-latitude normal intense flux patches (HN), relative stretching exhibits a strong dependence on *Pm*, but less than in global.

We also attempted to find power law fits for St/Ad of LN and LR, but no satisfactory fit (large \(\sigma _r\)) was found. The same holds for the other statistical quantities. Fits were therefore obtained for global and HN but not for LN and LR.

Next we fitted the global \({\mathcal {P}}/{\mathcal {T}}\) ratio. The best fit is

with \(\sigma _r=0.021\). The *Pm* power is dominant, motivating

with \(\sigma _r=0.022\). Then (33) may be approximated in logarithmic scale as

The 0.179 slope in Fig. 11a well approximates the \(-\frac{1}{6}\) prediction in (34). Then, the parameter dependence of global \({\mathcal {P}}/{\mathcal {T}}\) is approximated by

Globally, the relative poloidal flow is mostly influenced by *Pm*, increasing with increasing electrical conductivity.

We followed similar fitting process for the \({\mathcal {P}}/{\mathcal {T}}\) ratio of HN. The parameter dependence of \({\mathcal {P}}/{\mathcal {T}}\) in HN is given by (Fig. 11b)

In HN, the relative poloidal flow also increases when electrical conductivity increases.

We also attempted to fit the global and local \(H_u\) ratio. In both cases, we found much lower powers than in (30), (31), (35) and (36), indicating that the parameter dependence of \(H_u\) is weak. We therefore do not plot this parameter dependence.

The St/Ad ratio is a good measure of the stretching influence in the SV, but it is not enough to measure the stretching efficiency. In Fig. 12 we compare the St/Ad and the \({\mathcal {P}}/{\mathcal {T}}\) ratios, globally and locally (HN, LN and LR). Although poloidal flow is necessary to produce stretching, Fig. 12a shows that global St/Ad is larger than global \({\mathcal {P}}/{\mathcal {T}}\) except for the large *Pm* case 2 where the two quantities are nearly identical. The larger St/Ad is an evidence for the presence of an important stretching contribution even when the toroidal flow dominates. Locally, HN shares the global behavior with even larger difference between the values of St/Ad and \({\mathcal {P}}/{\mathcal {T}}\) (Fig. 12b). In all dynamo models St/Ad is larger in HN than in global despite \({\mathcal {P}}/{\mathcal {T}}\) being smaller in HN than in global, evidence for the particularly high stretching efficiency in HN. LN exhibits higher values of \({\mathcal {P}}/{\mathcal {T}}\) in some of dynamo models but in most models St/Ad is larger (Fig. 12c). LR exhibits an opposite behavior: \({\mathcal {P}}/{\mathcal {T}}\) is larger in most models (Fig. 12d). In addition, the \({\mathcal {P}}/{\mathcal {T}}\) values in LR are significantly larger than in global or in the other patch types.

Figure 13 shows the efficiency of advection \(\xi _{\text {a}}\) and stretching \(\xi _{\text {s}}\) in each intense \(B_r\) patch type. In all dynamo models the stretching appears more efficient than the advection. The highest efficiency is found in all dynamo models for the magnetic flux intensification \(\xi _{\text {e}}\).

## Discussion

Globally, in our dynamo models stretching varies between half to comparable of advection SV, whereas the toroidal flow is 2–3 times larger than the poloidal flow (Table 3). Locally, stretching may dominate SV in field-aligned flow regions where advection is not effective. Such stretching dominance is found at high-latitude normal polarity flux patches in some dynamo models. The stretching contribution varies depending on the patch type. On average, stretching to advective SV RMS ratio in HN is 0.82, whereas the poloidal to toroidal flow RMS ratio is only 0.32 (Fig. 12b; Table 4), i.e., \({\text{St}}/{\text{Ad}}>{\mathcal {P}}/{\mathcal {T}}\) and hence stretching is much more efficient than advection in these patches. Stretching is also more efficient than advection in LN, though to a lesser extent (St/Ad is 0.61, whereas \({\mathcal {P}}/{\mathcal {T}}\) is 0.49 on average, Fig. 12c; Table 4). In contrast, stretching to advective SV RMS ratio in LR is 0.68, and the poloidal to toroidal flow RMS ratio is 0.72 (Fig. 12d; Table 4), so advection and stretching are comparably efficient in regions of reversed flux patches at low latitudes.

The magnetic field in our models is generated by the \(\alpha \)-dynamo mechanism via a helical flow (Olson et al. 1999). The surface expression of this process is a high correlation between tangential divergence and radial vorticity, providing a useful way to couple toroidal and poloidal motions at the top of the shell (Olson et al. 2002; Amit and Olson 2004). In our dynamo models, helical flow is a very good approximation (correlations of 0.78–0.87, see Table 3). The helical flow approximation is especially applicable at high latitudes where axial convective columns impinge the CMB (Amit et al. 2010, Table 4).

Positive/negative correlations of magnetic flux with downwelling/upwelling, respectively, indicate that the magnetic field is concentrated by downwelling (Christensen et al. 1998) and dispersed by upwelling (Olson and Aurnou 1999). Moderate correlations appear because as downwellings are advected, magnetic field structures persist and diffuse slowly (Amit et al. 2010) causing a phase shift between the field concentrations and the cyclones that maintain them (Olson and Christensen 2002; Aubert et al. 2007; Takahashi et al. 2008).

The level of cancellation of the SV structures at high-latitude normal polarity flux patches shows that stretching is more efficient than advection (Fig. 13a). This results in a highly effective local magnetic flux intensification by stretching (\(\xi _{\text {e}}=0.9\) on average). In LN, the efficiency of stretching and advective structures as well as the stretching efficiency to locally intensify the magnetic flux in these patches are lower (Fig. 13b). The advective bipolar structures seen in LR are more balanced (hence the lowest \(\xi _{\text {a}}\) value) and the intensification of the magnetic field by stretching is less effective than at other patch types (\(\xi _{\text {e}}=0.66\) on average).

Globally, relative stretching increases with increasing rotation, but decreases when convection and electrical conductivity increase, with the strongest dependence being on *Pm* (Fig. 10a). The relative global poloidal flow is also influenced by *Pm*, increasing with increasing electrical conductivity. The helical flow correlation \(H_u\) depends on *Pm* and *Ra* (stronger dependence on *Pm*). However, the much lower powers of \(H_u\) compared to the powers of the St/Ad and \({\mathcal {P}}/{\mathcal {T}}\) fits indicate that its parameter dependence is much weaker.

It is tempting to insert Earth-like control parameters to our power laws. This yields stretching that is much larger (by two orders of magnitude) than advective SV. This is obviously unrealistic and may result from the small number of dynamo models studied which led to a poor extrapolation. Nevertheless, qualitatively we may hypothesize that stretching at the top of Earth’s core is even stronger than in our dynamo models.

Conventional magnetic Reynolds number estimates might not represent the induction accurately because field–flow interactions are not considered. The \(\cos \gamma \) values in Table 5, which represent the level of field-aligned flow, are in agreement with the values found by Finlay and Amit (2011). This means that the advective effective magnetic Reynolds number \(Rm_{\text {a}}\) is about 30 % lower than the conventional *Rm*. The stretching effective magnetic Reynolds number \(Rm_{\text {s}}\) varies between half to one \(Rm_{\text {a}}\). Finally, \(Rm_{\text {e}}\), which combines the effective advective and stretching magnetic Reynolds numbers, is about two-thirds of the conventional *Rm* (Table 5). This 50 % increase is the level of overestimation of the magnetic Reynolds number when field–flow interactions are ignored for both advection and stretching.

We note that surprisingly the two quantities \(\cos \gamma \) and \(\xi _{Rm}\) are very similar (Table 5). Our synthetic tests of these quantities clearly show that there is no apparent reason for this similarity (Table 2). This suggests that the particular field–flow interactions in the dynamo models produce same field–flow alignment (represented by \(\cos \gamma \)) and advection/stretching interference (represented by \(\xi _{Rm}\)). The intermediate \(\cos \gamma \) values arise from low contributions at high latitudes where the flow is nearly aligned with the radial field, balanced by large contributions at low latitudes where the flow is nearly perpendicular to the radial field (Finlay and Amit 2011). The intermediate \(\xi _{Rm}\) values stem from the nearly non-correlated advection and stretching SV patterns. Indeed, for RMS ratio St/Ad ∼ 0.5–1 the purely non-correlated relation gives ∼0.7–0.75, while some overlap introduces some anti-correlation with lower \(\xi _{Rm}\) contributions (see expressions after 21). At the moment, however, the precise reason for this similarity between \(\cos \gamma \) and \(\xi _{Rm}\) in the dynamo models is still unknown to us.

Resemblance between the stretching signature in our dynamo models and local geomagnetic SV structures may provide some evidence for the existence of stretching and hence upwelling/downwelling at the top of the Earth’s core. We find same sign radial field and stretching SV signatures in zones of intense flux patches (see Figs. 2, 3, 5, 6, 8, 9). Amit (2014) found same sign persistent radial field and total SV below the Indian Ocean. In the same region, studies of geomagnetic field models identified formation of flux patches (Jackson et al. 2000; Finlay and Jackson 2003) and studies of core flow models reported strong poloidal flows (e.g., Amit and Pais 2013; Baerenzung et al. 2016). Overall, local morphological similarities between stretching SV in our dynamo models and total SV in the geomagnetic field (Amit 2014) may suggest that the whole of the outer core convects.

Naively it may be expected that the role of stretching would be represented by the relative size of poloidal flow. However, we found that the global ratio of RMS stretching to RMS advection is systematically larger than the ratio of RMS poloidal flow to RMS toroidal flow. The larger relative stretching than relative poloidal flow is even more pronounced at zones of high-latitude normal polarity intense flux patches. In these regions the toroidal flow is often aligned with \(B_r\)-contours and hence it produces little advection (Finlay and Amit 2011). In contrast, downwelling is often correlated with these patches, rendering stretching efficient in concentrating and maintaining these robust features. Lesur et al. (2015) argued that the geomagnetic SV requires weak poloidal flow, which led them to conclude that the top of the core is weakly stratified. According to our dynamo models, even if the poloidal flow is weak stretching SV may be significant in the kinematics at the top of the core.

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## Authors’ contributions

HA ran the dynamo simulations. DP analyzed the models’ output, produced the graphics, calculated the statistics and wrote the paper. All authors read and approved the final manuscript.

### Acknowledgements

We thank two anonymous reviewers for constructive comments that improved the paper. This study was supported by the Centre National d’Etudes Spatiales (CNES). D.P. was supported by a Ph.D. research grant from Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES) and a grant by LPG-Nantes. K.P. was supported by la Région des Pays de la Loire and Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES- Proc no BEX 2498/13-8).

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We confirm that we read SpringerOpen’s guidance on competing interests. We declare that none of the authors have any competing interests in the manuscript.

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## Appendix: Variables

### Appendix: Variables

See Table 6.

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Peña, D., Amit, H. & Pinheiro, K.J. Magnetic field stretching at the top of the shell of numerical dynamos.
*Earth Planet Sp* **68**, 78 (2016). https://doi.org/10.1186/s40623-016-0453-x

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DOI: https://doi.org/10.1186/s40623-016-0453-x

### Keywords

- Secular Variation
- Outer Core
- Dynamo Model
- Magnetic Reynolds Number
- Dynamo Action