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# A generating process of geomagnetic drifting field

- Takesi Yukutake
^{1}and - Hisayoshi Shimizu
^{1}Email authorView ORCID ID profile

**Received:**7 May 2018**Accepted:**11 August 2018**Published:**10 September 2018

## Abstract

## Keywords

- Geomagnetic secular variation
- Westward drift
- Sectorial harmonics
- Flow in Earth’s core

## Introduction

### Geomagnetic secular variation and westward drift

It is well known that some specific features of the geomagnetic field are drifting westwards, while many other features are standing at the same place, changing their intensity. Take, for example, the intense focus of the vertical component anomaly in the equatorial region near the western coast of African continent observed at the Earth’s surface. It has been moving westwards steadily for the past several hundred years (e.g., Bullard et al. 1950; Yukutake and Tachinaka 1968a). At the core surface, a focus corresponding to the African focus was confirmed to exist near the equator and drifting westwards (Bloxham et al. 1989; Jackson 2003; Finlay and Jackson 2003). Besides, the drifting foci are distributed in a narrow equatorial region (Jackson 2003; Finlay and Jackson 2003). These observations seem to suggest that the westward drift in the low latitudes is a special feature characteristic in the equatorial region.

From this, a question arises whether the drift might be a local phenomenon limited in the equatorial region. In the atmospheric and oceanic sciences, the equatorially trapped wave is a well-known phenomenon (e.g., Bretherton 1964; Matsuno 1964; Longuet-Higgins 1968; Pedlosky 1987; Zhang 1993). However, it is not certain whether such confinement occurs when a magnetic field exists. Employing an equatorial β-plane approximation for the surface layer of the core, Bergman (1993) examined how the equator-trapped wave was modified in the presence of the dipole field. Although full induction equations were not incorporated in his formulation, he found that the magnetic field released the wave from confinement in the equatorial region, and that the wave extended its undulation to higher latitudes.

Investigations of the core flow that produces the observed magnetic field and its secular variation are now being conducted intensively. These are mainly based on the frozen flux approximation (Roberts and Scott 1965) that ignores magnetic diffusion and regards the observed secular variation is due to the advection of field at the surface of the core. The frozen flux approximation is widely applied to the several decade data that include the satellite observation. Further assumptions are made such as tangentially geostrophy or quasi-geostrophy (see Bloxham and Jackson 1991; Holme 2015; Finlay et al. 2010, for review). In the tangentially geostrophic assumption, core surface flow has been estimated by assuming that the Lorentz force is negligibly weak at the core surface and the geostrophic balance holds. In the quasi-geostrophic assumption, the flow is pursued that produces the observed type of magnetic field and its temporal variation at the core surface by assuming that the flow in the core consists of quasi-geostrophic columnar flow (e.g., Pais and Jault 2008; Gillet et al. 2009; Amit and Pais 2013). On the other hand, the flow and field of numerical geodynamo models were examined whether they could generate the field compatible with the observation at the surface of the core. The model by Aubert et al. (2013), for example, which is based on the gravitational coupling between the inner core and the mantle, is a successful one. Latitudinal and longitudinal distributions of the secular variation similar to the observations are obtained. Furthermore, endeavors are being made to assimilate the observed field to the flow model in the core to pursue the development of the magnetic field (Kuang et al. 2009, 2010; Tangborn and Kuang 2015; Barrois et al. 2017, 2018). One of the issues common to these studies is azimuthal flow near the core surface, corresponding to the drifting of the African focus observed at the Earth’s surface. Strong westward flows are commonly obtained in the equatorial region of Atlantic hemisphere (e.g., Gillet et al. 2015; Finlay et al. 2016), although the existence of eastward drifting phase is also suggested, for example, in the higher latitudes (Finlay and Jackson 2003). However, detailed structure such as the equator- symmetric nature of the drifting field, which is one of the characteristic features of the drifting field (Yukutake and Shimizu 2015), is not well recovered yet.

Although the westward drift appears to be restricted to special features when the main field is examined, distribution of the temporal variation of the field, secular variation, is different. The westward drift is also recognized in the pattern of the secular variation as well. However, drifting features cover wider region, extending from equatorial region to higher latitudes (Yukutake and Tachinaka 1968b; Yukutake and Shinizu 2015). The secular variation seems to suggest that the westward drift is more like a global phenomenon.

Employing the Gauss coefficients of the geomagnetic potential expressed in spherical harmonic series, Yukutake and Tachinaka (1969) decomposed the geomagnetic field into drifting and standing fields. The drifting field is the field drifting westwards for the past several hundred years, while the standing field is the field staying at the same location. In the drifting field, two features are remarkable (Yukutake 1981; Yukutake and Shimizu 2015). One is the predominance of sectorial harmonics where the degree (*n*) and order (*m*) are equal. The vertical component (or magnetic potential) is symmetric about the equator with its maximum at the equator. The other remarkable feature is about the drift velocity. It is nearly uniform, about 0.3°/year, irrespective of harmonics. On the other hand, the standing field is largely anti-symmetric about the equator and its intensity is stronger than the drifting field. Accordingly, when the drifting and standing fields are synthesized, in the total field the drifting field is mostly concealed by the standing field and observable only in a narrow equatorial region as the African magnetic anomaly (Yukutake and Shimizu 2016).

In this study, we attempt to clarify the nature of the drifting field based on the drifting and standing field model. Particularly, we concentrate on the characteristic feature, predominance of sectorial harmonics in the drifting field.

### Outline of the generating process

We consider that the westward drift is a manifestation of hydromagnetic process near the surface of the core, where the dipole field is dominant. From a nature of the drifting field, we assume that the surface layer of the core is rotating westwards as a whole. The uniform drift rate, one of the characteristic features of the drifting field, implies that the drift velocity is nondispersive. It has long been a matter of controversy whether the westward drift is due to a material flow or a hydromagnetic wave (Bullard et al. 1950; Hide 1966; Holme 2015). The uniform drift rate seems to favor the material flow, in which the field is generated and conveyed together. Because the hydromagnetic wave is a dispersive wave in general, the wave velocity is highly dependent on harmonics. We assume here that the surface layer is rotating westwards, in which the sectorial type field is produced by interaction of fluid flow with the dipole field.

If we take the mantle to be electrically insulating, electrical currents normal to the core–mantle boundary must vanish at the boundary. This leads to predominance of sectorial harmonics in the toroidal flow. This type of toroidal flow, interacting with the dipole field, induces the sectorial type of poloidal field (Yokoyama and Yukutake 1989; Yukutake and Yokoyama 1988). This is the type of the observed drifting field for the lower harmonics up to *n *= *m* = 6 for the past 400 years (e.g., Yukutake and Shimizu 2015). When this process occurs in the layer rotating westwards, the induced sectorial poloidal field is observed as the drifting field that is characterized by the sectorial harmonics. In the poloidal flow system, on the other hand, the fluid motion is confined on a meridional plane in the surface layer aligned in the north–south direction. The meridional flow induces the zonal poloidal field that is immune to rotation. Then, it is impossible to observe the field produced by the poloidal flow as the drifting field. Consequently, only the sectorial field generated by the toroidal flow is observed as the drifting field. This process will be confirmed with a simplistic model in the following sections.

## Theory and methods

### Model and equations

*T*and

*S*are scalar functions for the magnetic field. With these scalar functions, we rewrite the equations.

*curl*and

*curl*.

*curl*of (6), (7), (9), we obtain their radial components as follows;

In this study, we take \(\nu = 0\), \(\kappa = 0\). Regarding the electrical conductivity, we study two cases. One is the case where the electrical conductivity in Region II is infinite, and the other is the case where it is finite.

### Boundary conditions

## Results

### Infinite conductivity in Region II

#### Predominance of sectorial harmonics in the toroidal flow

The flow structure in the surface layer is greatly affected by the boundary condition on the electric current at the core–mantle boundary. Stress-free flow is further restricted by the boundary condition on the electric currents. If we take the case where the electric current induced by the toroidal flow and the current by the poloidal flow respectively satisfy the boundary condition, sectorial harmonics dominate in the velocity potential of toroidal flow, and the velocity potential of poloidal flow is restricted to zonal harmonics.

*j*= 0, 1, 2, 3, …. This makes it clear that \(\psi\) is a function symmetric about the equator.

Relative amplitude of \(a_{n}^{m}\) for \(r_{1}^{\prime} = 0.9\) and \(i = 1\)

\(a_{m}^{m}\) | \(a_{m + 2}^{m}\) | \(a_{m + 4}^{m}\) | \(a_{m + 6}^{m}\) | |
---|---|---|---|---|

\(m = 2\) | 1 | \(3.3 \times 10^{ - 2}\) | \(1.5 \times 10^{ - 3}\) | \(6.3 \times 10^{ - 5}\) |

\(m = 3\) | 1 | \(4.4 \times 10^{ - 2}\) | \(1.9 \times 10^{ - 3}\) | \(7.6 \times 10^{ - 5}\) |

\(m = 4\) | 1 | \(4.5 \times 10^{ - 2}\) | \(1.9 \times 10^{ - 3}\) | \(7.1 \times 10^{ - 5}\) |

\(m = 5\) | 1 | \(4.4 \times 10^{ - 2}\) | \(1.8 \times 10^{ - 3}\) | \(6.1 \times 10^{ - 5}\) |

\(m = 6\) | 1 | \(4.2 \times 10^{ - 2}\) | \(1.6 \times 10^{ - 3}\) | \(5.2 \times 10^{ - 5}\) |

#### Magnetic field in the generating layer

This is due to predominance of the sectorial term \(a_{m}^{m}\) in \(\psi\). The obtained \(S_{\psi }\) is exactly the observed type of field as the drifting field. Therefore, it can be said that the predominance of the sectorial term in the drifting field is a product of the boundary condition on the electric current at the core–mantle boundary.

*m*= 0 are nonzero by the boundary condition for \(\varPhi\), \(S_{\varPhi }\) is also represented only by zonal harmonics as

#### Characteristic frequency

In order to obtain the intensity of magnetic field, it is necessary to estimate the frequency of the system, as is clear in (33) and (34). The model in this study is an oscillating system caused by imbalance between Coriolis and Lorentz forces. In the following, we estimate the characteristic frequency of the system.

*T*and

*S*in momentum Eqs. (15) and (16) by means of induction Eqs. (17) and (18), we multiply them by \(G_{n} \left( {\alpha_{n,j} r} \right)P_{{n^{\prime}}}^{{m^{{\prime }} }} \left( {\cos \theta } \right)e^{{im^{{\prime }} \varphi }} r^{2} \sin \theta {\text{d}}r{\text{d}}\theta {\text{d}}\varphi\), and integrate over interior of the spherical shell. Then, we obtain

In \(\{ c_{tn1} ,c_{tn2} ,c_{tn3} , \ldots \}\) of the above equation, *n* should be taken to be *m* (*n* = *m*). The obtained frequency is separated into two classes, a relatively high frequency of the order of \(O\left( {10^{ - 4} } \right)\) 1/s and a low frequency lower than \(O\left( {10^{ - 10} } \right)\) 1/s. The higher frequency is inertial frequency, and the low frequency is magnetostrophic frequency. Approximate solution and numerical values when *m *= 2 are shown as the following.

*i*= 1.

Characteristic magnetostrophic frequency \(\omega_{m}\) for \(r_{1}^{{\prime }} = 0.9\) and \(i = 1\)

\(m = 2\) | \(m = 3\) | \(m = 4\) | \(m = 5\) | |
---|---|---|---|---|

\(\omega_{m}\) (s | \(- \;8.8 \times 10^{ - 14}\) | \(- \;7.3 \times 10^{ - 13}\) | \(- \;1.9 \times 10^{ - 12}\) | \(- \;3.6 \times 10^{ - 12}\) |

#### Magnetic field in the mantle

The magnetic field generated in Region II diffuses out into the mantle. The diffused field is derived by continuation of the normal component of magnetic flux density at the boundary.

*v*is constant, \(S_{\psi }\) in (33) and \(S_{\varPhi }\) in (34) are expressed in the coordinate system fixed to the mantle Region I as follows.

#### Toroidal velocity

*n*=

*m*= 6 are predominant. In Fig. 4, the maximum northward velocity for each harmonic order at the equator is plotted. The maximum velocity increases with the harmonic order. For

*m*= 2, for example, the velocity is \(2.1 \times 10^{ - 6}\) cm/s, while for

*m*= 6, it is \(4.7 \times 10^{ - 5}\) cm/s. This increasing trend means that, in order to generate the observable field, the higher velocities are necessary for the smaller scale fields. It should be noted, however, that the drifting-standing field in the present model is terminated with

*n*=

*m*= 6. When the analysis is extended to higher harmonics, the flow pattern is supposed to be more small-scale predominant.

It is surprising that such slow velocity is capable of producing the observed drifting field. It is supposed to be caused by such extreme conductivity as infinite conductivity assigned to the generating layer Region II. Much higher velocity is expected for the finite conductivity.

### Finite electrical conductivity in Region II

Following the procedures of the infinite conductivity case, we have extended our study to a finite conductivity model. In this section, we summarize the results. Since the observed type of sectorial poloidal field is produced only by toroidal flow \(\psi\) and the whole process is essentially the same as that of the infinite conductivity case, we describe the results for toroidal flow \(\psi\).

#### Magnetic potential

*T*must be zero at the boundary. As the normal component of the current, here we take that of the current due to the induction before the current diffuses, which means that we take the current produced by the first term of (50) with the second term set aside. Then, we obtain,

Relative amplitude \(a_{n}^{m}\) for \(r_{1}^{{\prime }} = 0.9\) and \(i = 1\)

\(a_{m}^{m}\) | \(a_{m + 2}^{m}\) | \(a_{m + 4}^{m}\) | \(a_{m + 6}^{m}\) | |
---|---|---|---|---|

\(m = 2\) | 1 | \(3.3 \times 10^{ - 2}\) | \(5.3 \times 10^{ - 3}\) | \(1.4 \times 10^{ - 3}\) |

\(m = 3\) | 1 | \(4.3 \times 10^{ - 2}\) | \(6.2 \times 10^{ - 3}\) | \(1.4 \times 10^{ - 3}\) |

\(m = 4\) | 1 | \(4.3 \times 10^{ - 2}\) | \(5.6 \times 10^{ - 3}\) | \(1.1 \times 10^{ - 3}\) |

\(m = 5\) | 1 | \(4.0 \times 10^{ - 2}\) | \(4.7 \times 10^{ - 3}\) | \(8.3 \times 10^{ - 4}\) |

\(m = 6\) | 1 | \(3.7 \times 10^{ - 2}\) | \(3.9 \times 10^{ - 3}\) | \(6.2 \times 10^{ - 4}\) |

*S*becomes symmetric about the equator, while the toroidal potential

*T*is anti-symmetric. This is clearly seen in the following equations.

*S*, as in the observed drifting field. In order to confirm whether this is also true in the finite conductivity case, we need to estimate the frequency \(\omega\).

#### Characteristic frequency

Characteristic magnetostrophic frequency \(\omega_{m}^{{}}\) (s^{−1}) for \(m = 2\), \(r_{1}^{{\prime }} = 0.9\) and \(i = 1\)

Initial guess \(\omega_{2}^{{}}\) (s | Obtained \(\omega_{2}^{{}}\) (s | |
---|---|---|

Step 1 | \(2.83 \times 10^{ - 12} + 1.31 \times 10^{ - 13} i\) | \(6.41 \times 10^{ - 13} + 1.02 \times 10^{ - 12} i\) |

Step 2 | \(6.41 \times 10^{ - 12} + 1.02 \times 10^{ - 12} i\) | \(3.67 \times 10^{ - 13} + 7.26 \times 10^{ - 12} i\) |

Step 3 | \(3.67 \times 10^{ - 13} + 7.26 \times 10^{ - 12} i\) | \(4.18 \times 10^{ - 13} + 6.55 \times 10^{ - 12} i\) |

Characteristic magnetostrophic frequency \(\omega_{m}^{{}}\) (s^{−1}) for \(r_{1}^{{\prime }} = 0.9\) and \(i = 1\)

\(\omega_{m}^{m}\) (s | |
---|---|

\(m = 2\) | \(4.18 \times 10^{ - 13} + 6.55 \times 10^{ - 12} i\) |

\(m = 3\) | \(1.25 \times 10^{ - 12} + 1.62 \times 10^{ - 12} i\) |

\(m = 4\) | \(2.48 \times 10^{ - 12} + 2.82 \times 10^{ - 12} i\) |

\(m = 5\) | \(4.09 \times 10^{ - 12} + 4.17 \times 10^{ - 12} i\) |

\(m = 6\) | \(6.06 \times 10^{ - 12} + 5.69 \times 10^{ - 12} i\) |

#### Predominance of sectorial terms in the toroidal flow and the poloidal field

*S*and

*T*. We rewrite (55) and (56) as follows.

*m*= 2. The figure indicates that the sectorial harmonics

*n*=

*m*dominate over other harmonics

*n*=

*m*+ 2,

*m*+ 4,…. This means that the observable field becomes sectorial term predominant. (In “Appendix: Explicit expression of

*S*in (59) for

*m*= 2”,

*S*for

*m*= 2 is given with numerical coefficients.)

Absolute values of \(\left\{ {T_{gu,n}^{m} ,T_{gv,n}^{m} ,T_{A,n}^{m} , T_{B,n}^{m} } \right\}\) are plotted in Fig. 5b for *m* = 2. In this case, the term for *n* = *m *+ 1 is predominant. The field is anti-symmetric about the equator.

#### Toroidal velocity

*m*= 2, while in the infinite conductivity model, higher harmonic flow is outstanding.

*m*in Fig. 7. A difference from the case of infinite conductivity is that the velocity for

*m*= 2 is faster than any other harmonics. For

*m*= 2, the velocity is \(1.7 \times 10^{ - 4}\) cm/s, while it is \(1.4 \times 10^{ - 4}\) cm/s for

*m*= 6. A further difference is that the velocity is 10–10

^{2}times faster than that of the infinite conductivity case. This is reasonable because, in the finite conductivity case, greater energy is required for the liquid flow against Joule dissipation to generate the observed field.

## Summary of the results

It has been presumed that the observed drifting field is produced by interaction of core surface flow with the axial dipole field. In order to understand the essential process, we have examined an extreme case. The mantle is electrically insulating, and the field-generating layer is of infinite conductivity. Fluid viscosity and thermal diffusivity are zero. Then, the top surface is stress free. Although the observed field is not a simple dipole field but the nondipole field also exists near the core–mantle boundary, we approximated the field by an axial dipole field only. Then, we examined the field generated by fluid flows in a thin shell at the core surface.

We have found that the boundary condition on the electric current at the core–mantle boundary exerts the vital effect on generating the observed type of drifting field. The normal component of the current must vanish at the core–mantle boundary. This strongly constrains the flow pattern at the surface. When the current induced by the toroidal flow satisfies the boundary condition, the flow becomes the type of sectorial harmonics predominant. Interacting with the dipole field, this flow induces the poloidal magnetic field with the sectorial harmonics predominant, which is exactly the same type of field as the observed drifting field. On the other hand, the poloidal flow becomes the flow confined on the meridional plane. It induces the zonal poloidal field that cannot be observed as the drifting field.

The characteristic frequency is different between the two models. For the infinite conductivity, the frequency is lower than for the finite conductivity. It is \(\omega_{m} = - 8.8 \times 10^{ - 14}\) 1/s for *m* = 2 for the infinite conductivity, whereas it is \(\omega_{m} = 4.2 \times 10^{ - 13} + 6.6 \times 10^{ - 13} i\) 1/s for *m* = 2 for the finite conductivity model. Since the toroidal velocity is proportional to frequency, the velocity to induce the observed magnitude of the drifting field is slower for the infinite conductivity than for the finite conductivity. It is about \(10^{ - 6} - 10^{ - 5}\) cm/s for the infinite conductivity, while it is about \(10^{ - 4}\) cm/s for the finite conductivity. It is reasonable that the slower velocity is sufficient for the higher conductivity to induce the observed field. It is also noted that the velocity obtained here is much slower than the velocity inferred from the westward drift of the magnetic field, \(10^{ - 2}\) cm/s.

*D*) of 175 km, 350 km and 700 km in case of infinite conductivity. The frequency increases with the thickness. This may sound somewhat strange, because the magnetostrophic frequency decreases with thickness as \(D^{ - 2}\), provided the magnetic field is constant. In the present case, however, the dipole field increases its intensity with depth as \(r^{ - 3}\). This intensity change is supposed to affect the frequency increase with thickness. As discussed before, the increase in frequency leads to increase in the fluid velocity that is needed to produce the observed drifting field. However, the frequency change is not so large as in the case of changing conductivity. Therefore, the change in the velocity due to the change of the thickness is rather limited. This suggests that participation of the deeper part of the surface flow is not very sensitive in generating the drifting field.

Characteristic frequency \(\omega_{m}^{{}}\) (s^{−1}) for \(i = 1\)

\(D = 175\) (km) | \(D = 350\) (km) | \(D = 700\) (km) | |
---|---|---|---|

\(m = 2\) | \(- \;7.1 \times 10^{ - 14}\) | \(- \;8.8 \times 10^{ - 14}\) | \(- \;1.4 \times 10^{ - 13}\) |

\(m = 3\) | \(- \;5.9 \times 10^{ - 13}\) | \(- \;7.3 \times 10^{ - 13}\) | \(- \;1.1 \times 10^{ - 12}\) |

\(m = 4\) | \(- \;1.5 \times 10^{ - 12}\) | \(- \;1.9 \times 10^{ - 12}\) | \(- \;2.9 \times 10^{ - 12}\) |

Inviscid fluid with zero viscosity is another extreme approximation. This allows the free surface condition at the core–mantle boundary. However, this is not an actual case. Since the fluid core is viscous liquid, the core–mantle boundary must be taken as the rigid surface. Surprisingly if the rigid boundary condition is applied, the radial component of the field induced by fluid flow becomes zero at the core–mantle boundary, so that the induced field cannot be observed at the Earth’s surface. This problem will be surmounted by attaching a thin viscous layer with finite electrical conductivity to the mantle. Then, the boundary between this thin layer and the field-generating layer is stress-free surface. The thin top layer works only to attenuate the field from inside.

## Discussion

In this study, we have pursued a generation process of the drifting field, considering that the drifting and standing fields are of different origin. This is a different approach to the core dynamics from that of many current investigations that attempt to derive the flow structure from the total field without discriminating the different type of fields. Such remarkable features as westward drifting flux patches in the equatorial region of the Atlantic hemisphere or low secular variation in the Pacific area are common issues to these investigations. They were attempted to explain by specific numerical dynamo simulations by ascribing inhomogeneous boundary conditions at the inner-outer core or core–mantle boundary (e.g., Amit and Choblet 2012; Aubert et al. 2013).

In our model, however, these features are a natural consequence of coexistence of two types of fields, drifting and standing fields (Yukutake and Shimizu 2015, 2016). Westward drift becomes remarkable at the equator by superposition of the standing field, whose vertical component is anti-symmetric about the equator, on the sectorial type of equator-symmetric drifting field. Time variation is also different between the two types of fields. Some of the standing fields are growing rapidly, and the other decaying. Low secular variation in the Pacific is supposed to be caused by the drifting field’s passing over the changing standing fields. The problem is, therefore, to find the flow structure of the drifting and the standing fields separately.

One of the attractive ideas about the westward drift is wave propagation. Magnetostrophic wave (often called magnetic Rossby wave) generated by combined effect of Coriolis, Lorentz and/or gravitational forces has been considered to be a cause of the westward drift of the magnetic field (see, e.g., Finlay et al. 2010 for review). Yoshida and Hamano (1993), Hori et al. (2018), for example, examined the magnetostrophic waves in the framework of quasi-geostrophic approximation. Yoshida and Hamano (1993) obtained the westward drifting field with phase velocity similar to the observed, which was excited by the oscillation of the mantle with respect to the core with heterogeneous topographic bottom boundary. To be noted is that they obtained the wave that was symmetric about the equator as expressed by sectorial harmonics. That is exactly the type of the observed field. This stems from the type of the toroidal field they assumed as the background. It was equatorially symmetric field. Interaction of the columnar flow, which is essentially symmetric type in the quasi-geostrophic approximation, with the symmetric toroidal field induces equatorially symmetric poloidal field. Accordingly, the problem in their study is whether the toroidal field is equatorially symmetric or not. Hori et al. (2018) conducted geodynamo simulations and found the magnetostrophic waves that were compatible with those derived from quasi-geostrophic approximation. Unfortunately, however, their waves were of equatorially anti-symmetric type. This is due to the toroidal field in their simulation, which was anti-symmetric about the equator, although it is very usual in the geodynamo simulations (see, e.g., Christensen and Wicht 2009). Through interaction with anti-symmetric toroidal field, columnar flow induces anti-symmetric field.

Common to these wave theories there is a serious problem. It is a dispersive nature of the wave velocity. The phase velocity highly depends on the harmonics, while there is no significant dispersive relationship between harmonics in the observed field (Yukutake and Shimizu 2015). Considering the nondispersive drift velocity, we considered in this study that the field is buried in the zonal flow near the core surface and carried westwards as a whole. The zonal flow has been approximated by a rotating spherical shell. This is similar to the classical Bullard et al.’s model (1950). Since this is a very crude approximation and the change of the layer thickness does not have serious effect on the results, it does not necessarily rule out the possibility of the flow structure gradually changing with depth. However, the approximation by the surface layer is in harmony with the stratification model near the core surface (e.g., Braginsky 1998, 1999; Buffet 2014). And it seems to favor the stratification model.

Regarding the sectorial nature of the drifting field, we have considered interaction of sectorial toroidal flow with the dipole field. This interaction induces the observed type of sectorial poloidal field. The problem is why the surface toroidal flow is sectorial. This has been solved by the boundary condition on the electric current. Into the insulating mantle, no electric current is allowed to penetrate. This condition strongly constrains the surface flow. Then, it has been found that only the sectorial type flows are possible to exist.

Regarding the standing field, we have not deepened the examination. We simply guess, as in many of dynamo simulations, that it is produced by columnar rolls in the deeper part of the core under the surface layer. Interacting with the anti-symmetric toroidal field, the columnar flow induces anti-symmetric poloidal field. For example, the intense anomaly rapidly growing over the Eurasian continent is supposed to be one of those products.

## Conclusions

The drifting field is comprised mostly of sectorial harmonics. This is one of the characteristic features of the drifting field. We pursued the cause of this characteristic feature. A simple model was employed.

The field is generated by fluid flow within the surface layer of thickness *D* (e.g., *D* = 350 km). The geomagnetic field near the core–mantle boundary is approximated by an axial dipole field. The core fluid is inviscid. The mantle is electrically insulating. Regarding the electrical conductivity of the generating layer, we examined two cases, infinite conductivity and finite conductivity (\(5 \times 10^{5}\) S/m).

The normal component of the electric current must vanish at the core–mantle boundary. This boundary condition imposes a strong constraint on the fluid motion in the layer. The toroidal flow that produces the current with no normal component at the boundary becomes sectorial type flow that consists of harmonics \(P_{m + 2j}^{m} \left( {\cos \theta } \right)\) (*j* = 0, 1, 2, 3,…) with sectorial harmonics \(P_{m}^{m} \left( {\cos \theta } \right)\) predominant. The poloidal flow becomes meridional type flow that is expressed only by zonal harmonics \(P_{n}^{0} \left( {\cos \theta } \right)\). The flow is confined on the meridional plane.

Interaction of the sectorial type toroidal flow with the axial dipole field induces the sectorial type poloidal field. Since the sectorial harmonics dominates in the toroidal flow, the sectorial harmonics is also predominant in the poloidal field. As the generating layer rotates westward, the sectorial field rotates together. This is observed as the drifting field with sectorial harmonics predominant. On the other hand, the meridional type flow, interacting with the axial dipole field, induces the poloidal field of zonal harmonics. Rotation of the zonal field induces zero secular variation. Therefore, the zonal field is not observed as the drifting field. Consequently, the sectorial type field produced by the sectorial type toroidal flow is the only field that is observed as the drifting field.

## Declarations

### Authors’ contributions

TY designed the study, carried out the calculations, and prepared the manuscript. HS helped in designing a part of research, checking the calculations, and preparing the manuscript. Both authors read and approved the final manuscript.

### Acknowledgements

We thank two anonymous reviewers for their valuable comments, which were very helpful in improving the manuscript.

### Competing interests

The authors declare that they have no competing interests.

### Availability of data and materials

Drifting and standing magnetic field model is published as Table 1 in Yukutake and Shimizu (2015).

### Funding

HS is supported by JSPS KAKENHI Grant Number 15H05832.

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## Authors’ Affiliations

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