# The Capon Method for Mercury's Magnetic Field Analysis

^{1}Institut für Theoretische Physik, Technische Universität Braunschweig, Braunschweig, Germany^{2}Space Research Institute, Austrian Academy of Sciences, Graz, Austria^{3}Institut für Geophysik und Extraterrestrische Physik, Technische Universität Braunschweig, Braunschweig, Germany^{4}DLR Institute of Planetary Research, Berlin, Germany

Characterization of Mercury's internal and external magnetic field is one of the primary goals of the magnetometer experiment on board the BepiColombo MPO (Mercury Planetary Orbiter) spacecraft. A novel data analysis tool is developed to determine the Gauss coefficients in the multipole expansion using Capon's minimum variance projection method. The construction of the estimator is presented along with a test against the numerical simulation data of Mercury's magnetosphere and a comparison with the least square fitting method shows, that Capon's estimator is in better agreement with the coefficients, implemented in the simulation, than the least square fit estimator.

## 1. Introduction

The reconstruction of planetary magnetic fields is one of the most important goals of a magnetometer experiment on board an orbiting spacecraft. Various inversion methods have successfully been applied to the data of former missions that visited different planets in our solar system. For example, generalized inversion [1] and elastic net regression [2] have been applied to the reconstruction of Jupiter's internal magnetic field. The weighted least square fit [3] and robust regression [4] appeared as useful methods for the analysis of Saturn's magnetic field. The Earth's magnetic field has been analyzed among other methods by using the maximum entropy method [5]. All these methods will be useful tools for Mercury's magnetic field analysis, which is one of the primary goals of the magnetometer experiment on board the BepiColombo mission. In this work we present an alternative method, namely Capon's method, for the analysis of Mercury's internal magnetic field.

Capon's method [6], also known as minimum variance distortionless response estimator (MVDR) [7], was introduced for reconstructing the velocities and wave vectors of seismic waves measured on an array of sensors on the Earth's surface. In space plasma physics, the method has first been successfully applied to the analysis of plasma waves in the terrestrial magnetosphere [8]. Later on, the method was extended for the mode decomposition of magnetic fields [9]. This establishes a basis to separate the planetary magnetic field from the total measured field in Mercury's magnetosphere.

The separation of the internal magnetic field from the external parts of the field, which are generated by currents flowing in the magnetosphere is important for the reconstruction of the internal field. There exists a paraboloid model of Mercury's magnetosphere [10] which has successfully been applied to the analysis of Mercury's internal magnetic field [11, 12]. Since Capon's method is applied to the analysis of Mercury's internal magnetic field for the first time, here only the internal parts of the field are considered in the parametrization as a proof of concept.

Concerning to the BepiColombo mission, in this work magnetic field data resulting from the plasma interaction of Mercury with the solar wind are simulated and Capon's method is applied to the magnetic field data to analyze Mercury's internal magnetic field.

## 2. Parametrization and Inversion Methods

### 2.1. Parametrization of Mercury's Magnetic Field

The parametrization of planetary magnetic fields is based on the Gauss representation [13]. If only data in curl-free regions are analyzed, Ampère's law ∂_{x} × __ B__ = 0, where

__is the magnetic field vector and ∂__

*B*_{x}is the spatial derivative, yields the existence of a scalar potential Φ, so that

__= −∂__

*B*_{x}Φ. In general, Φ is composed of internal and external parts. In the following only the internal parts Φ

_{i}will be considered. For the parametrization of the internal dipole and quadrupole fields the scalar potential is expanded into spherical harmonics

where planetary centered coordinates with radius *r*, azimuth angle λ∈[0, 2π], and polar angle θ∈[0, π] are chosen. *R*_{M} indicates the radius of Mercury and ${P}_{l}^{m}$ are the Schmidt-normalized associated Legendre polynomials of degree *l* and order *m*. The expansion coefficients ${g}_{l}^{m}$ and ${h}_{l}^{m}$ are the internal Gauss coefficients. Arranging the Gauss coefficients into a vector $\underset{\_}{g}:\text{}={\left({g}_{1}^{0},{g}_{1}^{1},{h}_{1}^{1},{g}_{2}^{0},{g}_{2}^{1},{h}_{2}^{1},{g}_{2}^{2},{h}_{2}^{2}\right)}^{T}$, for later application called ideal coefficient vector, the contribution of the internal magnetic field can be rearranged as

where the terms of the multipole series are arranged in the matrix $\underset{\_}{\underset{\_}{H}}$(r,θ,λ). The magnetic field measurements __ B__ and the underlying model $\underset{\_}{\underset{\_}{H}}$ are known. The unknown coefficient vector

__is to be determined. In most applications the number of known magnetic data points is much larger than the number of the expansion coefficients, resulting in an overdetermined inversion problem. Therefore, $\underset{\_}{\underset{\_}{H}}$ is a rectangular matrix in general and the direct inversion of Equation (2) is impossible. But there exist several inversion methods for estimating__

*g*__[7].__

*g*### 2.2. Least Square Fit (LSF) Method

The most commonly used method for inverse problems is the least square fit method. The method minimizes the quadratic deviation between the disturbed measurements __ B__ and the model $\underset{\_}{\underset{\_}{H}}$ [7]

Providing us

where † symbolizes the Hermitian adjunction. The LSF estimator *g*_{L} realizing the minimal deviation is given by

### 2.3. Capon's Method

Capon's method is based on the construction of a filter matrix $\underset{\_}{\underset{\_}{w}}$ so that the output power

is minimized with respect to $\underset{\_}{\underset{\_}{w}}$, subject to the distortionless constraint

where $\text{tr}\left[{\underset{\_}{\underset{\_}{w}}}^{\u2020}\underset{\_}{\underset{\_}{M}}\underset{\_}{\underset{\_}{w}}\right]$ is the trace of the matrix ${\underset{\_}{\underset{\_}{w}}}^{\u2020}\underset{\_}{\underset{\_}{M}}\underset{\_}{\underset{\_}{w}}$ and $\underset{\_}{\underset{\_}{I}}$ is the identity matrix. The matrix $\underset{\_}{\underset{\_}{M}}:\text{}=\langle \underset{\_}{B}\xb0\underset{\_}{B}\rangle $ is called the data covariance matrix, where the angular brackets indicate averaging over ensemble, e.g., different samples, realizations, or measurements. The error of the magnetic data is assumed to be Gaussian with variance σ_{n} and zero mean. In this case, the data covariance matrix can be written as $\underset{\_}{\underset{\_}{M}}=\langle \underset{\_}{B}\rangle \xb0\langle \underset{\_}{B}\rangle +{\sigma}_{n}^{2}\underset{\_}{\underset{\_}{I}}$. Capon's estimator realizing the minimal output power, subject to the distortionless constraint, results in [9]

which has the same structure as the LSF estimator (Equation 4), but with additional weighting by the covariance matrix. This demonstrates that the Capon filter discriminates between preferred and deprived data whereas the LSF treats all data equally. Adding a constant value ${\sigma}_{d}^{2}$ to the diagonal of the covariance matrix improves the robustness of Capon's estimator [14]. The diagonal loaded covariance matrix results in

where ${\sigma}^{2}:={\sigma}_{n}^{2}+{\sigma}_{d}^{2}$.

## 3. Simulation of Mercury's Magnetic Field

For the evaluation of Capon's estimator in comparison with the LSF estimator simulated magnetic field data are analyzed. The data are simulated with the hybrid code AIKEF [15], that has successfully been applied to several problems in Mercury's plasma interaction [16]. The internal Gauss coefficients ${g}_{1}^{0}=-190\mathrm{\text{nT}}$ and ${g}_{2}^{0}=-78\mathrm{\text{nT}}$ [17], defining the non-vanishing components of the ideal coefficient vector __ g__ (Equation 2), are implemented in the simulation code and the magnetic field resulting from the interaction of Mercury with the solar wind is simulated. The solar wind velocity of 400km/s is orientated parallel to the

*x*-axis and the solar wind magnetic field with

*B*

_{0}= 20nT is orientated toward the

*z*-axis. The

*y*-axis completes the right hand system. The solar wind density was chosen to 30cm

^{−3}. In Figure 1, the simulated magnitude of the magnetic field

*B*is displayed in the

*x*-

*z*-plane (meridional plane).

**Figure 1**. Simulated magnitude of the magnetic field *B* in multiples of the solar wind magnetic field *B*_{0} = 20nT in the *x*-*z*-plane. The black lines describe the magnetic field lines. The white circle of radius 1*R*_{M} symbolizes Mercury. The implemented internal Gauss coefficients are ${g}_{1}^{0}=-190\mathrm{\text{nT}}$ and ${g}_{2}^{0}=-78\mathrm{\text{nT}}$ [17].

## 4. Application and Discussion

Now Capon's method is applied to the simulated data for reconstructing the ideal Gauss coefficients implemented in the simulation. The comparison of Capon's estimator *g*_{C} with the ideal coefficient vector __ g__ enables the judgement of the method. To classify the role of Capon's method in terms of the diversity of existing inversion methods, Capon's estimator furthermore is compared with the LSF estimator

*g*_{L}. The data are evaluated at an ensemble of data points with distance 0.2

*R*

_{M}from the surface on the night side of Mercury (

*x*< 0). The reconstructed Gauss coefficients are presented in Table 1.

The underlying model only describes the internal magnetic field $\underset{\_}{\underset{\_}{H}}\underset{\_}{g}$. The external parts of the field $b:\text{}=\underset{\_}{B}-\underset{\_}{\underset{\_}{H}}\underset{\_}{g}$ are not parameterized. Thus, the deviation of the LSF estimator and the ideal coefficient vector is given by

whereas the difference between Capon's estimator and the ideal coefficient vector results in

To judge the quality of Capon's estimator the comparison of individual coefficients presented in Table 1 is not a vital metric. For example, the Gauss coefficient ${g}_{2}^{0}$ reconstructed by the LSF method is in better agreement with the ideal coefficient than the coefficient estimated by Capon's method. But for all coefficients together *g*_{C}−__ g__<

*g*_{L}−

__holds.__

*g*Therefore, Capon's estimator is in better agreement with the ideal coefficient vector than the LSF estimator.

The choice of the diagonal loading parameter ${\sigma}_{d}^{2}$ is essential for the difference *g*_{C}−__ g__. The diagonal loaded covariance matrix results from the additional quadratic constraint $\text{tr}\left({\underset{\_}{\underset{\_}{w}}}^{\u2020}\underset{\_}{\underset{\_}{w}}\right)={T}_{0}$, where

*T*

_{0}= const. and ${\sigma}_{d}^{2}$ is the corresponding Lagrange multiplier [14]. The choice of

*T*

_{0}controls the diagonal loading parameter ${\sigma}_{d}^{2}$ and defines how the data will be weighted by the filter matrix $\underset{\_}{\underset{\_}{w}}$. It depends on the underlying model and the evaluated data. Figure 2 illustrates how σ in principle controls the difference

*g*_{C}−

__. For σ → 0 Capon's estimator shows a large deviation to__

*g*__. If σ → ∞, Capon's estimator approaches the LSF estimator. But if the data are not completely described by the model (__

*g*__≠0) there exists a parameter $\sigma =\sqrt{{\sigma}_{n}^{2}+{\sigma}_{d}^{2}}={\sigma}_{0}$, so that for all σ≥σ__

*b*_{0}

Furthermore it even exists an optimal parameter σ_{opt.}, that realizes the best agreement between Capon's estimator and __ g__. For the results presented in Table 1 this optimal parameter is σ

_{opt.}≈276nT.

**Figure 2**. Sketch of the deviation *g*_{C}−__ g__ between Capon's estimator

*g*_{C}and the ideal coefficient vector

__subject to σ. For large σ → ∞ the deviation converges to the deviation of the least-square-fit estimator__

*g*

*g*_{L}and the implemented coefficient vector

__. There exists σ__

*g*_{0}so that

*g*_{C}−

__≤__

*g*

*g*_{L}−

__, for all σ≥σ__

*g*_{0}, and an optimal parameter σ

_{opt.}, that realizes the best agreement between Capon's estimator an the ideal coefficient vector.

Since the choice of σ controls $\text{tr}\left({\underset{\_}{\underset{\_}{w}}}^{\u2020}\underset{\_}{\underset{\_}{w}}\right)$, the value of the optimal diagonal loading parameter is not directly related with an error of the magnetic measurements. More likely σ_{opt.} can be understood as a parameter that measures the model mismatches.

When Capon's method is applied to real spacecraft data, the ideal coefficient vector __ g__ is not available anymore and therefore the deviation

*g*_{C}−

__cannot be used as metric for calculating the optimal diagonal loading parameter. In this case, there exist other methods for estimating σ__

*g*_{opt.}, e.g. the L-curve method, that solely depend on the underlying model and the data [18].

## 5. Summary and Outlook

In this work Capon's method has been applied to simulated magnetic field data to analyze Mercury's internal magnetic field. The internal field, parameterized by the internal Gauss coefficients, was implemented in the simulation code AIKEF and the magnetic field resulting from the plasma interaction of Mercury and the solar wind was simulated. The comparison of Capon's method and the commonly used least square fit method showed that Capon's estimator is in better agreement with the implemented Gauss coefficients than the least square fit estimator. A helpful procedure is the diagonal loading of the data covariance matrix, that improves the robustness of Capon's estimator. It turns out that there exists an optimal diagonal loading parameter where Capon's estimator is nearest to the ideal coefficient vector.

Since only the internal magnetic field was parameterized, Capon's estimator shows some deviation to the implemented coefficients. Additional parameterizing of the external contributions of the magnetic field, for example by using the paraboloid model for Mercury's magnetosphere [10], may still improve Capon's estimator, especially when data points are collected in some distance above the planetary surface. Moreover, this enables us to reconstruct higher-order terms such as octupole terms. Furthermore, as the Gauss representation is restricted to curl-free regions, the Mie representation (poloidal-toroidal decomposition) would extend the data collection to regions where electrical currents flow.

## Data Availability Statement

The raw data supporting the conclusions of this article will be made available by the authors, without undue reservation.

## Author Contributions

All authors contributed conception and design of the study. DH organized the database. ST, YN, and UM performed the statistical analysis and wrote the first draft of the manuscript. All authors contributed to manuscript revision, read, and approved the submitted version.

## Funding

We acknowledge support by the German Research Foundation and the Open Access Publication Funds of the Technische Universität Braunschweig. This work by YN was supported by the Austrian Space Applications Programme at the Austrian Research Promotion Agency under contract 865967. DH was supported by the German Ministerium für Wirtschaft und Energie and the German Zentrum für Luft- und Raumfahrt under contract 50 QW1501.

## Conflict of Interest

The authors declare that the research was conducted in the absence of any commercial or financial relationships that could be construed as a potential conflict of interest.

## Acknowledgments

The authors are grateful for stimulating discussions and helpful suggestions by Karl-Heinz Glassmeier, Patrick Kolhey, and Alexander Schwenke.

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Keywords: diagonal loading, Gauss coefficients, least–squares method, magnetic field analysis, Capon's method

Citation: Toepfer S, Narita Y, Heyner D and Motschmann U (2020) The Capon Method for Mercury's Magnetic Field Analysis. *Front. Phys.* 8:249. doi: 10.3389/fphy.2020.00249

Received: 31 March 2020; Accepted: 05 June 2020;

Published: 14 July 2020.

Edited by:

Luca Sorriso-Valvo, National Research Council, ItalyReviewed by:

Tommaso Alberti, Institute for Space Astrophysics and Planetology (INAF), ItalyIgor Ivanovich Alexeev, Lomonosov Moscow State University, Russia

Copyright © 2020 Toepfer, Narita, Heyner and Motschmann. This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) and the copyright owner(s) are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.

*Correspondence: Simon Toepfer, s.toepfer@tu-braunschweig.de