 Full paper
 Open access
 Published:
Geomagnetic Virtual Observatories: monitoring geomagnetic secular variation with the Swarm satellites
Earth, Planets and Space volume 73, Article number: 54 (2021)
Abstract
We present geomagnetic main field and secular variation time series, at 300 equalarea distributed locations and at 490 km altitude, derived from magnetic field measurements collected by the three Swarm satellites. These Geomagnetic Virtual Observatory (GVO) series provide a convenient means to globally monitor and analyze longterm variations of the geomagnetic field from lowEarth orbit. The series are obtained by robust fits of local Cartesian potential field models to alongtrack and East–West sums and differences of Swarm satellite data collected within a radius of 700 km of the GVO locations during either 1monthly or 4monthly time windows. We describe two GVO data products: (1) ‘Observed Field’ GVO time series, where all observed sources contribute to the estimated values, without any data selection or correction, and (2) ‘Core Field’ GVO time series, where additional data selection is carried out, then denoising schemes and epochbyepoch spherical harmonic analysis are applied to reduce contamination by magnetospheric and ionospheric signals. Secular variation series are provided as annual differences of the Core Field GVOs. We present examples of the resulting Swarm GVO series, assessing their quality through comparisons with ground observatories and geomagnetic field models. In benchmark comparisons with six highquality midtolow latitude ground observatories we find the secular variation of the Core Field GVO field intensities, calculated using annual differences, agrees to an rms of 1.8 nT/yr and 1.2 nT/yr for the 1monthly and 4monthly versions, respectively. Regular sampling in space and time, and the availability of data error estimates, makes the GVO series well suited for users wishing to perform data assimilation studies of core dynamics, or to study longperiod magnetospheric and ionospheric signals and their induced counterparts. The Swarm GVO time series will be regularly updated, approximately every four months, allowing ready access to the latest secular variation data from the Swarm satellites.
Introduction
The geomagnetic field undergoes gradual change, evolving year by year in a process known as geomagnetic secular variation. These changes are thought to result primarily from motions of liquid metal in the Earth’s outer core but this process is not yet well enough understood to allow accurate predictions of future behavior, even a few years ahead (e.g., Alken et al. 2020a). In this situation we are forced to rely on carefully monitoring the geomagnetic field and its changes in order to provide the information necessary for navigation and orientation applications, and for descriptions of nearEarth radiation belts and current systems.
To make progress beyond field monitoring, detailed information on the geomagnetic variations as a function of space and time must be combined with knowledge of the underlying physical processes. With the rapid development of numerical geodynamo models over the past decade (e.g., Aubert and Finlay 2019), there is now the prospect of assimilating such information into realistic models, such that the processes underlying secular variation can be better understood.
For both monitoring longterm geomagnetic variations, and for data assimilation applications, it is an advantage to have processed satellite magnetic field data available on a well organized grid, with a regular sampling rate in space and time. The Geomagnetic Virtual Observatory (GVO) method is one approach to obtain such a dataset.
The Geomagnetic Virtual Observatory method was first proposed by Mandea and Olsen (2006) as a tool for making satellite magnetic field measurements easily accessible as time series of the vector geomagnetic field at prespecified locations. The GVO method involves fitting a scalar magnetic potential to satellite magnetic field observations from a chosen time window and within a local region, defined by a cylinder centered on a GVO target point. The potential is then used to compute the magnetic field at the GVO target point such that a mean magnetic field over a chosen time window at satellite altitude is determined; see Fig. 1. The GVO time series thus mimics the time series produced by groundbased magnetic observatories on timescales of months and longer. The main advantage of the GVO time series is that they can be produced at any sites of interest that are covered by satellite data, and in particular, can provide a global grid of time series derived from measurements made by similar instruments onboard satellites such as the Swarm trio.
Applications of the GVO time series include geomagnetic jerk studies (Olsen and Mandea 2007), comparisons with spherical harmonic (SH) based geomagnetic field models (Olsen et al. 2009, 2010), core flow studies (Kloss and Finlay 2019; Rogers et al. 2019) and data assimilation studies (Barrois et al. 2018). The GVO method can also be used to derive estimates of the magnetic field gradient tensor (Hammer 2018).
Focusing on the core magnetic field, initial studies showed that the original GVO series were contaminated by ionospheric and magnetospheric sources (Beggan et al. 2009; Domingos et al. 2019; Olsen and Mandea 2007; Shore 2013). Recommendations for improving the original GVO concept and better removing such contamination have been proposed (Hammer 2018; Shore 2013). Some of these improvements were implemented in more recent GVO series that have been used for core flow studies by Barrois et al. (2018); Kloss and Finlay (2019); Rogers et al. (2019); and Whaler (2017).
Here, we present details of an updated processing GVO scheme that has been developed during a Swarm DISC (Data, Innovation and Science Cluster) project and is now being used to produce regularly updated Swarm GVO time series as an official ESA Level 2 product. The primary purpose of this paper serves as a reference describing the Swarm GVO series and presenting example validation comparisons with ground observatories. In addition to taking account of the most important recommendations from earlier GVO studies, the series presented here also take advantage of principal component analysis (PCA) (Cox et al. 2018) and spherical harmonic analysis (SHA) in an effort to better isolate the core field signal.
In the “Data” section we describe the input data from the Swarm satellite mission, and the adopted data selection strategies. In the Sect. “Methodology” we describe in detail how the GVO series are calculated. The Sect. “Results” presents examples of GVO time series, derived using Swarm measurements from December 2013 to March 2020 and describes comparisons with ground observatory magnetic field series and global field model predictions. In the Sect. “Discussion and conclusions” we reflect on what can be learned from these comparisons, describe possible applications for the GVO series and mention ideas for extending and improving the present GVO approach.
Data
This section describes the satellite magnetic field measurements used to derive the Swarm GVO time series. The GVO products take as input vector magnetic field measurements in the form of the Swarm Level 1b (L1b) product MAGX_LR_1B, which contains qualityscreened, calibrated and corrected measurements given in physical SI units (nT) in a North, East, Center, hereafter NEC, reference frame. For the results presented here, we use Swarm data versions 0506 from the 1Dec2013 to 30Mar2020.
From the Swarm L1b 1Hz magnetic field data, two separate data chains are produced. Data chain (a) simply extracts all available measurements using a subsampling of 15s.
Data chain (b) extracts, again using a subsampling of 15s, only those measurements that satisfy the following dark, geomagnetic quiettime selection criteria:

Gross measurement outliers for which the vector field components deviate more than 500 nT from the predictions of the latest CHAOS field model (here version CHAOS7.2 (Finlay et al. 2020)) are rejected

The Sun is at least \(10^{\circ }\) below horizon

Geomagnetic activity index \(K_p < 3^{0}\)

Time rate of change of Ring Current (RC) index \(\vert dRC/dt\vert <3\)nT/hr\(^{1}\) (Olsen et al. 2014)

Merging electric field at the magnetopause \(E_m <0.8 \mathrm {mV m^{1}}\), (Olsen et al. 2014)

Constraints on IMF requiring \(B_z > 0\,\)nT and \(\vert B_y \vert <10\) nT.
2hourly means are computed from 1min values of the solar wind and IMF from the OMNI database (http://omniweb.gsfc.nasa.gov).
The Swarm GVO method described in the next section makes use of sums and differences of the satellite magnetic field measurements. Denoting the input magnetic data at a given position \({\mathbf {r}}\) by \(d_l({\mathbf {r}})=\hat{{\mathbf {l}}}\cdot {\mathbf {B}}({\mathbf {r}})\), where \({\mathbf {B}}({\mathbf {r}})\) is the vector magnetic field and \(\hat{{\mathbf {l}}}\) is a unit vector in the component direction, then \(\Sigma d_l\) and \(\Delta d_l\) denote sums and differences of the vector magnetic field components, respectively. Both alongtrack (AT) and East–West (EW) data sums and differences are considered such that \(\Sigma d_l=(\Sigma d_l^{\mathrm {AT}},\Sigma d_l^{\mathrm {EW}})\) and \(\Delta d_l=(\Delta d_l^{\mathrm {AT}},\Delta d_l^{\mathrm {EW}})\). Alongtrack data differences are calculated using the 15s differences \(\Delta d_l^{\mathrm {AT}} = [B_l({\mathbf {r}},t)  B_l({\mathbf {r}}+\delta {\mathbf {r}},t+15s)]\), where \(\delta {\mathbf {r}}=(\delta r,\delta \theta ,\delta \phi )\) is the change in position. A 15s alongtrack difference with a satellite speed of \(\approx 7.7\,\mathrm {km/s}\) corresponds to a distance of 115 km (Olsen et al. 2015). Alongtrack sums are similarly calculated as \(\Sigma d_l^{AT} = [B_l({\mathbf {r}},t) + B_l({\mathbf {r}}+\delta {\mathbf {r}},t+15\,s)]/2\). The East–West differences are calculated as \(\Delta d_l^{\mathrm {EW}} = [B_l^{\mathrm {SWA}}({\mathbf {r}}_1,t_1)  B_l^{\mathrm {SWC}}({\mathbf {r}}_2,t_2)]\) having an East–West orbit separation between the Swarm Alpha (SWA) and Charlie (SWC) satellites of \(\approx 1.4^{\circ }\), corresponding to 155 km at the equator (Olsen et al. 2015). The East–West sums were calculated as \(\Sigma d_l^{\mathrm {EW}} = [B_l^{\mathrm {SWA}}({\mathbf {r}}_1,t_1) + B_l^{\mathrm {SWC}}({\mathbf {r}}_2,t_2)]/2\). For a particular orbit of SWA, the corresponding SWC data were selected to be that closest in latitude with the condition that \(\vert \Delta t\vert =\vert t_1t_2\vert <50\) s.
Methodology
This section describes in detail the algorithms used to derive the following Swarm GVO products:

1)
1 and 4monthly time series of the ‘Observed Field’

2)
1 and 4monthly time series of the ‘Core Field’ and its secular variation.
Each product involves time series of spherical polar components of the vector magnetic field on an approximately equalarea global grid of 300 locations at an altitude of 490 km above the mean Earth radius. An overview of the algorithm is presented in Fig. 2.
GVO locations and timestamps
For a given GVO target point, and considering a specified time window of either 1 or 4 months, input data that fall within a cylinder of horizontal radius \(r_{cyl}=700\) km around the target point, and which also satisfy the relevant selection criteria (see Sect. "Data"), are extracted. The GVO locations are specified in spherical polar coordinates \({\mathbf {r}}_{GVO}=(r,\theta ,\phi )\), at fixed radius \(r=r_a+h_{GVO}\) where \(h_{GVO}\) is the height above the Earth’s mean spherical radius \(r_a=6371.2\) km. For the Swarm data described \(h_{GVO}=490\) km, so the GVOs are located at approximately the mean orbital height of the Swarm satellites during 2013–2020, considering each of the lower pair to contribute with half weighting.
The GVO time series are provided in a global approximately equal area grid based on the sphere partitioning algorithm of Leopardi (2006). Selecting a number of GVO grid points, and an associated target cylinder search radius \(r_{cyl}\) that avoids overlap of the target cylinders to ensure independent data, involves a tradeoff; decreasing the number of target points and increasing the search radius allows for more data within each GVO cylinder but at the same time lowers the spatial resolution. Preliminary tests with Swarm data suggested that 300 GVO grid locations provided a suitable balance (Hammer 2018). If higher spatial resolution is required, longer time windows than used here are necessary in order to obtain stable GVO estimates. The surface area dS covered by each GVO target cylinder is the total surface area A divided by the number of GVOs, \(N_{GVO}=300\), i.e., \(dS \sim A/N_{GVO} = 4\pi (r_a+h_{GVO})^2/N_{GVO}\), where \(r_a\) is the Earth’s mean radius 6371.2 km and \(h_{GVO}\) is altitude of GVOs, here 490 km. Equating this area with the area of a circle surrounding the GVO, \(\pi r_{cyl}^2\), gives a target cylinder search radius of \(r_{cyl}=\sqrt{4 (r_a+h_{GVO})^2/N_{GVO}} \approx 700\mathrm {km}\), where we have rounded down to the nearest hundred kilometers to ensure no overlap. The distance between any two GVOs is thus \(\approx 1400\)km. This corresponds roughly to SH degree \(n=14\), since the SH degree n is associated with a horizontal wavelength at satellite altitude is \(\lambda _n \sim 2\pi (r_a +h_{GVO}) /\sqrt{n(n+1)}\) (Backus et al. 1996). With a target cylinder search radius of 700km, approximately 80% of the data are used; the combined area of the cylinder footprints thus does not span the entire area of the spherical surface, but the independence of each GVO estimate is ensured. The top panel in Fig. 3 illustrates the locations of the 300 globally distributed GVOs and the footprint of the data target cylinders for each GVO. The grid also contains GVOs at the North and South Poles. At these positions the \((r, \theta , \phi )\) frame is defined by letting \(\theta\) be aligned along the Greenwich meridian, r point upwards and \(\phi\) completes the righthanded coordinate system. When computing the main field at the North/South Pole from field models, the average of the main field values evaluated \(0.1^{\circ }\) in latitude from the North/South Pole at longitudes \(0^{\circ }\) and \(180^{\circ }\) was used.
For the 1monthly series each GVO estimate has a timestamp corresponding to the 15th day of the considered calendar month. For the 4monthly series, which are constructed using data from within the intervals January–April, May–August, and September–December, the GVO estimates have been allocated timestamps of the 1st of March, the 1st of July and the 1st of November. The secular variation series are computed from annual differences of the 1monthly and 4monthly series, so their timestamps are shifted by 6 months compared with the field series. GVO epoch times are for formal reasons given in GVO product files as milliseconds since 01Jan0000 00:00:00.000, following the convention for Swarm data products.
Data preprocessing
In order to derive the Observed Field GVO time series, we start from the geocentric spherical polar components of the vector magnetic field, \({\mathbf {B}}^{obs}=(B_r,B_{\theta },B_{\phi })\), and subtract predictions, \({\mathbf {B}}^{MF}\), from the IGRF main field model (Alken et al. 2020b) for spherical harmonic degrees \(n \in [1,13]\). This results in the following Observed Field residuals
These residuals are used to derive the GVO estimates as described in Sect. "GVO model parameterization and estimation" below. Note that IGRF predictions at the GVO target points and times are added back during this procedure.
In order to derive 1monthly Core Field GVO time series from data chain (a), predictions from a lithospheric field model \({\mathbf {B}}^{lith}\) are also removed:
Here, we calculate \({\mathbf {B}}^{lith}\) using SH degrees \(n \in [14,185]\) from the LCS1 model (Olsen et al. 2017).
To derive 4monthly core field GVO time series from data chain (b), models of the magnetospheric and ionospheric fields are also removed during the preprocessing:
where \({\mathbf {B}}^{mag}\) is the predicted largescale magnetospheric field and its Earthinduced counterpart field, as given by the CHAOS model (Finlay et al. 2020), and \({\mathbf {B}}^{iono}\) is the predicted ionospheric field and its Earthinduced field as given by the CI model (Sabaka et al. 2018).
Estimates of the main field are in all cases removed from the data before carrying out the GVO estimation, and then afterwards added back at the target location and time; this step is necessary in order to prewhiten the data before carrying out the GVO estimation. Previous studies have shown that such prewhitening by removing a main field model is necessary in order to avoid noisy GVO estimates. Hammer (2018, p.74, Fig 4.6) presents examples of GVO series computed with and without prewhitening applied. Without prewhitening robust estimation schemes, based on iteratively reweighted least squares, are unable to correctly identify and downweight disturbed data resulting in noisier estimates. The specific main field model used for the prewhitening is however not crucial. For example, comparing GVO estimates constructed using IGRF13 and the CHAOS7.2 main field model, we found rms differences compared to the benchmark ground observatories described in Sect. "Validation tests" that agreed to within 0.05 nT across all three components, for both 4monthly and 1monthly GVO estimates. We therefore chose to use IGRF13 for the prewhitening step in for producing the Swarm GVO series in order to emphasize that the results obtained are not simply a result of biasing towards the CHAOS model.
Note that when considering time windows of 1 or 4 months for the GVO estimates, any information on time variations with periods shorter than these intervals is, of course, lost.
GVO model parameterization and estimation
A Cartesian potential forward model
We assume that magnetic field measurements are made in a sourcefree region such that the residual magnetic field is a Laplacian potential field, which fulfills the quasistationary approximation (Backus et al. 1996). In the following, we will use the general notation \(\delta {\mathbf {B}}\) for the residual fields of Eqs. (1, 2, 3) and refer to the position of the Geomagnetic Virtual Observatory as the target location.
The residual magnetic field and the associated locations within a specific target cylinder are transformed from the spherical coordinate system to a righthanded local topocentric Cartesian frame centered on (and constant within) each target cylinder, where at the GVO location x points towards geographic south, y points towards East and z points upwards. The bottom panel in Fig. 3 illustrates the geocentric spherical and local topocentric frames. Note that the unit vectors of the local Cartesian frame, \(({\hat{\mathbf {e}}}_{x},{\hat{\mathbf {e}}}_{y},{\hat{\mathbf {e}}}_{z})\), coincide with the spherical unit vectors, \(({\hat{\mathbf {e}}}_{\theta },{\hat{\mathbf {e}}}_{\phi },{\hat{\mathbf {e}}}_{r})\), at the target location but not elsewhere.
The magnetic scalar potential, V, associated with the residual magnetic field in a sourcefree region must satisfy Laplace’s equation \(\nabla ^2 V=0\) and the potential is related to the residual field by \(\delta {\mathbf {B}}=\nabla V\). The solution to Laplace’s equation in Cartesian coordinates can be written as a sum of harmonic polynomials (e.g., Backus et al. 1996)
where \( l = a + b + c \), and \(C_{abc}\) are the expansion coefficients, a, b, c are nonnegative integers, and L is the expansion order. In tests we found that for a GVO cylinder radius of 700 km, it was sufficient to expand the magnetic scalar potential to cubic order \(L=3\); this involves the 19 parameters in the above expansion.
To be a valid potential field requires irrotational (\(\nabla \times \delta {\mathbf {B}}=0\)) and solenoidal (\(\nabla \cdot \delta {\mathbf {B}}=0\)) conditions be satisfied. First we consider the solenoidal divergencefree criteria. This requires \(\nabla ^2 V=0\) which on inserting for the potential from Eq. (4) implies
Each of the terms in parenthesis must equal zero for this to be satisfied. This means that
The cubic potential series is thereby reduced by 4 parameters to a total of 15 parameters
The potential Eq. (6) also fulfills the curlfree criteria.
With an expansion for the magnetic potential established, we can now write a linear forward problem relating a vector \(\mathbf{m}\), consisting of the model coefficients \(C_{abc}\), to a vector \({\mathbf {d}}^{vec}\) of predictions for the residual magnetic field components in the local Cartesian system, \((\delta B_x,\delta B_y,\delta B_z)\), at the positions of satellite observations that fall with the GVO target cylinder for the time window under consideration,
Here \(\underline{\underline{{\mathbf {G}}}}^{vec}\) is then a design matrix constructed from appropriate spatial derivatives of the potential.
Olsen et al. (2015) and Sabaka et al. (2018) have demonstrated that using East–West differences (between Swarm A and C) and alongtrack differences (for all three Swarm satellites) improves the resolution of both the lithospheric field and the core field. They argued that correlated errors due to incompletely modeled largescale magnetospheric fields are reduced when using such field differences. In addition to field differences, East–West and alongtrack sums of the measurements also need to be included in order to adequately constrain the largest wavelength parts of the field (Hammer 2018; Sabaka et al. 2013). Based on this, we have chosen to use sums and differences of the vector components of the residual magnetic field, constructed along satellite tracks and considering East–West pairs of data between Swarm A and C. This results in a data vector \({\mathbf {d}}=\{\Delta d_{x}^{vec},\Delta d_{y}^{vec},\Delta d_{z}^{vec},\Sigma d_{x}^{vec},\Sigma d_{y}^{vec},\Sigma d_{z}^{vec}\}\), where \(\Delta\) and \(\Sigma\) denote the differences and sums of the residual field described in Sect. "Data". The design matrix linking the sums and differences to the coefficients of the potential is constructed as \(\underline{\underline{{\mathbf {G}}}}=\{\Delta G_x^{vec};\Delta G_y^{vec};\Delta G_z^{vec};\Sigma G_x^{vec};\Sigma G_y^{vec};\Sigma G_z^{vec})\}\) where \(\Delta G_{k}^{vec} = [G_{k}^{vec}({\mathbf {r}}_1)  G_{k}^{vec}({\mathbf {r}}_2)]\) and \(\Sigma G_{k}^{vec} = [G_{k}^{vec}({\mathbf {r}}_1) + G_{k}^{vec}({\mathbf {r}}_2)]/2\) with \(k=(x,y,z)\).
Robust least squares estimation
Based on the above definitions of \({\mathbf {d}}\) and \(\underline{\underline{{\mathbf {G}}}}\) for sums and differences of the residual magnetic field, the coefficients of the GVO model can be estimated using the following robust leastsquares inversion scheme
Here \(\underline{\underline{{\mathbf {W}}}}\) is a diagonal weight matrix, consisting of robust (Huber) weights for each entry in the data vector (e.g., Constable 1988), and an additional downweighting factor of 1/2 for data from satellites Alpha and Charlie which takes into account that these two satellites fly sidebyside and therefore provide similar measurements.
Having determined the potential, estimates of the residual magnetic field components, in local cartesian coordinates, at GVO target location (i.e., \(x=0, y=0, z=0\)) are computed as follows:
At the GVO target location, the local Cartesian field components are directly related to spherical polar field components (see Fig. 3) with \(\delta B_{GVO,r}=\delta B_{GVO,z}\) , \(\delta B_{GVO,\theta }=\delta B_{GVO,x}\) and \(\delta B_{GVO,\phi }=\delta B_{GVO,y}\). Each estimate is for a specific target GVO location \({\mathbf {r}}\) and epoch t, which is the center of the considered time window. The above procedure is repeated for each time window at each target location to obtain time series of estimates of the residual vector field at all GVO target locations.
A final step is needed to obtain the GVO estimates for the field. This is to add back the prediction of the main field model \({\mathbf {B}}_{GVO}^{MF}({\mathbf {r}},t)\), at each target point and epoch, using the same model (here IGRF13) that was removed from each satellite measurement during the preprocessing. This step is carried out separately for each component at each GVO location and each epoch, such that we finally obtain the GVO vector field time series
The estimated GVO magnetic field is provided in spherical polar \((r, \theta , \phi )\) vector components.
Observed Field GVOs
We define ‘Observed Field’ GVOs as field estimates computed from satellite observations while retaining all observed geomagnetic field sources. Observed Field GVO time series are derived from the sums and differences of the residual field computed using Eq. (1) and then applying the GVO method described by Eqs. (8–10). Onemonthly observed field GVOs are computed from data chain a) while 4monthly observed field GVOs are computed from data chain b).
Error estimates, \(\sigma _{obs}\), for the Observed Field GVOs are assumed to be timeindependent and spatially uncorrelated. They are calculated separately for each GVO times series (i.e., for each field component at each GVO location) based on a robust version of the total mean square error (e.g., Bendat and Piersol 2010), that includes both mean square residual and the mean residual squared, between the input data \(d_i\) and the GVO estimates \({\hat{d}}_i\) for a given series. With \(e_i=d_i{\hat{d}}_i\) this is calculated as
where the index i runs over all data contributing to a given series, \(\mu _w = \sum _i w_{i} e_{i} / \sum _i w_{i}\) is the robust mean residual and the robust weights \(w_i\) are calculated iteratively assuming a longtailed Huber distribution (Constable 1988):
with \(\epsilon _{i}=abs(e_{i})/std(e)\) and \(c_w=1.5\) is the chosen breakpoint for the Huber distribution.
Core Field GVOs and Secular Variation
We define ‘Core Field’ GVOs as field estimates computed from satellite observations with noncore fields removed (as far as possible). The core field and associated secular variation (SV) GVO time series are produced as follows. First, 1 and 4monthly GVO data files are produced, after which the 1monthly GVOs are denoised by a principal component analysis. Next, an epochbyepoch spherical harmonic analysis is carried out and the resulting external and toroidal magnetic fields (i.e., noninternal parts) are removed. Finally, annual differences of each series are computed in order to obtain the GVO core field SV time series.
For the 1monthly Core Field GVOs, GVO estimates are computed from sums and differences of the field residuals using Eq. (2) based on data chain (a) (i.e., without data selection criteria). For the 4monthly GVOs Core Field GVOs, GVO estimates are computed from sums and differences of the field residuals using Eq. (3) based on data chain (b) (i.e., with dark geomagnetically quiettime criteria applied).
Principal component analysis
Since the 1monthly Core Field GVOs were derived without data selection and having no model estimates of the ionosphere nor magnetosphere removed, external magnetic field signals remain. Such signals are considered as contamination (‘noise’) in the current context because our goal is to produce GVO estimates of the core field only. The monthly sampling rate means that a local time sampling bias also contaminates the GVO estimates, as it takes approximately 4 months for each satellite to revisit the same local time on Earth’s surface when considering both ascending and descending orbit tracks (see Shore 2013). To produce 1monthly Core Field GVOs we therefore employ the principal component analysis (PCA) method and Python package (MagPySV) described in Cox et al. (2018), to separate out and remove the various contaminating signals from the 1monthly GVO estimates. This procedure is based on earlier work by Wardinski and Holme (2011) and Brown et al. (2013), who used the PCA method to denoise ground observatory data one observatory at a time, rather than denoising time series from several locations simultaneously, as in Cox et al. (2018) and this work. A brief summary of this method is provided here; the reader is referred to Cox et al. (2018), Cox et al. (2020) and the companion to this paper Brown et al., in preparation for further details.
Domingos et al. (2019) applied PCA to an earlier version of the 4monthly GVO data series, considering both CHAMP and Swarm measurements. They performed PCA directly on GVO data series, rather than on annual differences of GVO series after subtracting predictions from a core field model as we do. Hence, our PCA analysis looks for coherent signals that remain once features like the largescale internal variations identified by Domingos et al. (2019) have been removed. Whilst their focus was on modes associated with the variance of internal field, they also identified an interesting mode associated with annual variations of the external field in their Swarm GVO series. Our analysis is not well suited to studying annual variations since we apply PCA to annual difference estimates of SV. After carrying out tests with our PCA procedure we decided there was not much advantage in applying it to the 4monthly GVOs. Our 4monthly GVO SV series contain fewer identifiable coherent external signals on which we would apply the PCA. This is due to the dark quiettime data selection criteria, the applied corrections for magnetospheric and ionospheric fields, and the absence (by design) of the 4month local time sampling bias that remains in the 1month series where PCA denoising is applied.
The key premise to our approach is that the SV residuals (the difference between observed GVO SV and that predicted by an internal magnetic field model) provide information about contaminating signals that are present in the GVO data but not in the internal model. The PCA of the SV residual covariance matrix leads to a proxies for these contaminating signals that are then removed from the GVO data. We approximate the GVO SV series using annual differences and the SV residuals are calculated as the difference between the GVO SV estimates and the SV predicted by the CHAOS7.2 model (Finlay et al. 2020) evaluated up to SH degree 13 at the same times and locations. Comparable results can be achieved using alternative field models, provided they represent time variation of the main field in a continuous manner when detrending each GVO SV series.
In their application to ground magnetic data, Cox et al. (2018) found that this method is most effective when considering groups of observatories at similar magnetic latitudes because the dominant external magnetic field source varies with magnetic latitude. Suitably grouped observatories experience similar noise at the same times and these correlated signals show clearly in the dominant principle components (PCs) of the SV residuals. On that basis, we estimated the mean magnetic latitude at GVO locations using the AACGMv2 Python package (Burrell et al. 2020; Shepherd 2014) and assigned them to one of five magnetic latitude regions: Polar North, Polar South, Auroral North, Auroral South and Low to Midmagnetic latitudes (see Table 1).
For N GVO locations, the SV residual covariance matrix for the vector time series is 3N by 3N, and can be decomposed into 3N eigenvalues and eigenvectors, describing the PCs of the SV residual data set. The contributions of the K dominant PCs, corresponding to the K largest eigenvalues, are removed from the SV residuals, and afterwards the internal model SV from the CHAOS72 model is added back to the corrected residuals to form the denoised SV.
In this application, we remove the most significant K PCs entirely, as opposed to removing the scalar projection of a proxy signal for the PC content as described in Cox et al. (2018) and earlier related works. Our removal of PCs here involves the removal of the associated eigenvectors and the component of signal at each GVO location in the projected directions of these eigenvectors. Note the number K differs by region, depending on how many PCs can be confidently identified as arising from one of the expected contaminating sources described above.
We identify PCs as noise sources based on their geographic distributions, correlations to annual differences of external magnetic field proxies (e.g., Dst, Polar Cap North/South, Em, AE (Kauristie et al. 2017)), or peaks in their discrete Fourier transform (DFT) at the local time bias frequency. Table 1 gives the number of PCs identified as noise, along with the percentage of variance in the SV residuals accounted for by each of these PCs and the total percentage variance removed in each region.
In a last step, the denoised SV are numerically integrated to produce denoised onemonthly magnetic field time series, again treating SV as annual differences. The denoised magnetic field must be releveled at the start of this calculation. We use the original GVO field values for the first 12 time samples for this purpose, meaning that the denoised field values start 12 months after the original GVO time series begins.
Spherical harmonic analysis
The magnetic field time series produced by the GVO method assumes a potential field description. This implies that no electrical currents exist within the measurement region. In reality however, satellite magnetic measurements are made in the ionospheric Fregion where in situ electrical currents may be present (Olsen 1997; Sabaka et al. 2010), especially in the auroral regions. Due to space–time aliasing, these nonpotential fields can leak into the GVO estimates (Olsen and Mandea 2007).
In the situation of nonvanishing, but purely radial, currents within the shell of measurements the magnetic field can written in terms of poloidal, \({V^{int},V^{ext}}\), toroidal, \(T^{sh}\), and scalar potentials (e.g., Backus 1986; Olsen 1997; Olsen and Mandea 2007):
where each of the potentials can be represented by expansions up to some maximum SH degree N:
where \(r_a=6371.2\)km is the reference value for the Earth’s mean spherical radius, n and m are here the SH degree and order, respectively, and \(P_n^m\) are the associated Schmidt seminormalized Legendre functions. In the three expansions, \(\{g_n^{m},h_n^{m}\}\) are the internal coefficients, \(\{q_n^{m},s_n^{m}\}\) are the external coefficients and \(\{t_n^{m,c},t_n^{m,s}\}\) are the expansion coefficients associated with the toroidal scalar potential.
Predictions of the geomagnetic field components at the GVO locations are linearly related to the above expansion coefficients such that a forward problem can be written
where the data for a given epoch, t are given by \({\mathbf {d}}_{GVO}=\{B_r({\mathbf {r}}_1,t),...,B_r({\mathbf {r}}_{N_{GVO}},t),...\) \(B_{\theta }({\mathbf {r}}_1,t),...,B_{\theta }({\mathbf {r}}_{N_{GVO}},t),B_{\phi }({\mathbf {r}}_1,t),...,B_{\phi }({\mathbf {r}}_{N_{GVO}},t)\}\), where \(N_{GVO}\) is the number of GVOs, related to the expansion coefficients \({\mathbf {m}}_{SH}=\{g_n^m,h_n^m,q_n^m,s_n^m,t_n^{m,c},t_n^{m,s}\}\) via a design matrix \(\underline{\underline{{\mathbf {G}}}}_{SH}\), which is constructed from the spatial derivatives of Eqs. (14, 15 and 16). Here, we truncated the internal, external and toroidal expansions at SH degree 13 and the model coefficients were determined epoch by epoch from the GVO estimates using a simple leastsquares solution:
At epochs where an insufficient number of GVOs are available to ensure a stable solution, the external and toroidal coefficients were determined by a linear interpolation between nearby epochs. Following the SHA, external and toroidal field estimates are removed epoch by epoch from the 1 and 4monthly time series to produce final Core Field GVO time series.
Secular variation estimates
The secular variation of the Core Field series at a particular GVO location, \({\mathbf {r}}\), for a given epoch t, is computed using annual differences between field values at time \(t+0.5\) yr and at time \(t0.5\) yr:
Annual differences are a well established way to estimate the core field secular variation since they remove annual signals from ionospheric and magnetospheric signals that are otherwise difficult to isolate. Note however that such annual signals do remain in the GVO field series themselves.
Error estimates
The error estimates, \(\sigma _{core}\), for each Core Field GVO time series are assumed to be timeindependent and spatially uncorrelated. They are computed separately for each field component at each GVO based on the residuals between the GVO data and the corresponding predictions of the timedependent internal part of the CHAOS field model for SH degrees \(n \in [1,20]\). Denoting the residuals by \({\mathbf {e}}={\mathbf {d}}_{GVO}{\mathbf {d}}_{CHAOS}\) the error estimates are given by
where \(i=1,...,M\) denotes the ith data element, and M is the number of data in a given series and \(\mu\) is the residual mean.
Error estimates of the secular variation GVO time series are computed in a similar manner as described above but using residuals between the SV GVO data, \(SV_{GVO}\), and the SV predictions of the CHAOS timedependent internal field model.
Validation tests
Comparison of GVO series with ground magnetic observatories
Validation tests were performed by comparing the GVOs and independent ground observatory (GObs) records, which are the established standard reference data series for monitoring longterm variations of the geomagnetic field. Our validation tests considered data from 28 INTERMAGNET (International Realtime Magnetic Observatory Network) ground observatories, listed in Table 2. These were chosen for their representative geographic coverage, spanning both polar and nonpolar latitudes and all longitude sectors. Below we refer to polar stations as being the 13 stations with colatitudes \(0^{\circ }\) to \(36^{\circ }\) and \(144^{\circ }\) to \(180^{\circ }\), with the remaining 15 stations referred to as nonpolar stations. From these stations we further selected six ‘benchmark’ stations (Chambon la Forêt, Kakioka, Honolulu, Guam, Hermanus and Canberra) from midtolow latitudes that are well known for their high quality. We use these in an attempt to establish, in wellunderstood conditions, the extent to which Swarm GVO series agree with ground records, with an emphasis on how well the core field secular variation is captured.
We used the Swarm AUX_OBS_2_ hourly mean ground observatory dataset, version 0122 from February 2020, maintained by the British Geological Survey (BGS), retrieved from ftp://ftp.nercmurchison.ac.uk/geomag/Swarm/AUX_OBS. These data have been checked and corrected for known baseline jumps (Macmillan and Olsen 2013). From these hourly mean values for each selected observatory we compute:

(i)
Onemonthly and fourmonthly simple mean field values, for each of the three spherical polar components. These are used for comparisons with the Observed Field GVO products.

(ii)
Onemonthly and fourmonthly versions of revised means (Olsen et al. 2014), wherein the CHAOS magnetospheric field (Finlay et al. 2016) and CM4 ionospheric field predictions (Sabaka et al. 2004) (and their induced counterparts) are first removed from the hourly means for each of the three spherical polar field components and then robust (Huberweighted) means are computed over 1 or 4monthly nonoverlapping windows. These series are used for comparisons with the Core Field and Secular Variation GVO products.
To enable direct comparisons with these ground observatory series, we computed dedicated GVO time series directly above each selected ground observatory, using the approach described in the Sect. "GVO model parameterization and estimation". We removed crustal bias estimates from each series (computed as the median residual from the CHAOS7.2 internal field model to up SH degree 16) and mapped the GVO estimates downwards to the position of the ground observatory at Earth’s surface by removing the difference between CHAOS7.2 model predictions at the GVO location and the ground observatory location. This results in series we refer to as \({\widetilde{B}}_j^{GObs}(t_i)\) for the ground observatories and \({\widetilde{B}}_j^{GVO,map}(t_i)\) for the GVOs, respectively, both at the ground observatory location. The subscript j indicates either the r, \(\theta\) or \(\phi\) component, or the scalar field intensity F (computed by taking the squareroot of the sum of the squares of the three spherical polar components). The rootmeansquare (rms) deviation between the correspond ground observatory and GVO series was then computed as
where the summation runs over the length of the time series \(i=1,...,N_d\) where data are available from both series. The rms differences for secular variation series are computed in the same fashion, using annual differences of the ground observatory field, \({\widetilde{B}}_j^{GObs}(t_i)\), and Core Field GVOs mapped to the ground observatory positions, \({\widetilde{B}}_j^{GVO,map}(t_i)\). We computed summary means over these rms values for groups of series from the polar regions, the nonpolar region and benchmark observatories. For these tests we used the time interval 2015–2018 when there is good availability of both definitive observatory data and Swarm data.
We note that despite being the best available information concerning secular variation, the ground observatory records are themselves inherently imperfect. INTERMAGNET standards require that longterm accuracy of main field series be better than 5 nT, with the best observatories having an estimated baseline uncertainty of up to 0.4 nT (Lesur et al. 2017). Beyond observatory measurement uncertainties, a further source of differences between ground observatory data and GVO estimates is that the latter use data above the ionospheric Elayer, while ground data are collected at the Earth’s surface. They therefore observe ionospheric and magnetosphereionosphere coupling currents differently. Our potential field mapping used to downward continue the GVO estimates to Earth’s surface does not account for this difference, and so it is a source of discrepancy between the two series, particularly for the horizontal components.
Comparisons of GVO series with field model predictions
A second set of validation tests involved comparisons between the GVO products and predictions from geomagnetic field models. These have the advantage that the GVO product, provided on a global grid, can be tested directly (without any mapping) and the global quality of the products can be assessed. However, unlike the comparisons with ground observatories, tests against field model predictions are not fully independent as Swarm data were also used in the construction of the field models.
Comparisons to models are based on the rms deviation between a given GVO time series, \(B_j^{GVO}(t_i)\), and field model predictions, \(B_j^{mod}(t_i)\), at the GVO data location and times
where the summation runs over the length of the GVO time series \(i=1,...,N_{GVO}\) and j indicates a specific spherical polar component r, \(\theta\), \(\phi\) of the vector field or the scalar field intensity F.
For comparisons with the Observed Field GVOs, \(B_j^{mod}(t_i)\) is computed using the CHAOS7.2 timedependent internal field for degrees \(n \in [1,13]\), the LCS1 lithopsheric field model degrees \(n \in [14,185]\), as well as the CHAOS7.2 magnetospheric field (and induced counterparts) and the CIY4 ionospheric field (Sabaka et al. 2018) (and induced counterparts). The magnetospheric and ionospheric fields and their counterparts are computed as mean values for each 1monthly or 4monthly time window, considering the times of the actual data used to derive the GVO estimates. We note the model values compared to the Observed Field GVOs are not fully representative of all the fields contributing to the GVOs, in particular they do not include realistic ionospheric fields in the polar region, or magnetosphere–ionosphere coupling currents.
For comparisons with the Core Field GVOs, \(B_j^{mod}(t_i)\) is computed using the timedependent internal field from the CHAOS7.2 model (Finlay et al. 2020) using SH degrees up to 20, with the LCS1 lithospheric model (Olsen et al. 2017) for degrees \(n \in [14,20]\) removed. For comparisons with the Core Field Secular Variation GVOs, \(B_j^{mod}(t_i)\) is computed using the first time derivative of the timedependent internal field from CHAOS7.2, again up to SH degree 20. In the global grid there are 78 polar and 222 nonpolar GVOs and Benchmark values were computed using GVOs \(\pm 30^\circ\) in latitude from the equator. Comparisons were made between 2014 and 2020, throughout the time interval when GVO data were available.
Results
A global overview of the Swarm GVO time series
To illustrate the 1monthly GVO secular variation data series, Fig. 4 presents a global map of annual differences of the radial field component of the Observed Field GVO time series (blue dots) and of the Core field GVO time series (red dots). Fig. 5 presents a similar summary of the global results for the 4monthly GVO time series. Note the small difference in the time scales shown at the bottom left of these two figures; the SV of the 1monthly GVOCORE time series begins in 2015.5, since the GVOCORE time series starts only in 2015 due to the PCA processing, while the SV of the 4monthly GVOCORE begins in 2014.7 since no PCA is not performed on these.
Validation statistics: comparisons with ground observatories and field models
The results of the validation comparisons carried out are presented here in the form of two summary tables of statistics. Table 3 collects results of the validation tests against independent ground observatories and field models for the 1monthly GVO products, while Table 4 collects similar statistics for 4monthly GVO products. See Sect. "Validation tests" above for details of the tests.
When considering the statistics presented here, it is important to recall that the number of ground observatories is split into 13 “Polar” stations, 15 “nonpolar” stations and six “benchmark” stations. As mentioned in Sect. "Validation tests" the stations in each category were selected in order to obtain as far as possible reasonable geographic coverage of both the polar and nonpolar regions. The aim with the benchmark stations was to document and validate the performance of the GVO time at known highquality stations from midtolow latitudes where external contributions are less prominent. The error estimates provided along with the GVO products are also presented in these tables for reference. In these tables GVOOBS, GVOCORE and GVOSV denotes the Observed Field GVOs, the Core Field GVOs and the Core Field Secular Variation GVOs, respectively.
Example comparisons of GVO and ground observatory time series
More detailed insight comes from direct examination of the time series of the ground observatory and associated GVO series as described in Section "Validation tests". Fig. 6 presents the 1monthly Observed Field (GVOOBS, blue dots) and Core Field (GVOCORE, red dots) GVO estimates, mapped down to the Earth’s surface at three of the benchmark ground observatories. These figures include \(\pm \sigma\) uncertainty estimates, where we have made the assumption that these estimates remain unchanged when mapping the field to ground level. When examining the Observed Field GVOs we present time series of the field itself rather than the SV, so as not to filter out any signals that may be of interest by taking annual differences. Also plotted for comparison are the ground observatory hourly monthly means (omm, yellow dots) and revised monthly means (rmm, black dots).
Radial field variations observed at the benchmark stations are followed closely by the GVO series, for example at Kakioka (KAK) in Japan (left column, Fig 6) where both the trend in the field and its acceleration are in agreement. The ability of the Observed Field GVO series to track subannual field changes is illustrated by the southward \(\theta\)component, for example the peak observed in the second half of 2017 at Kakioka. This feature, likely of magnetospheric origin, is seen simultaneously at all benchmark stations in both the GVO and ground observatory series, and is particularly clear at Kakioka (KAK) and Hermanus (not shown here). The amplitude of the peak is slightly lower in the GVO series. More scatter is seen in the eastward \(\phi\)component of the GVO series compared to the ground observatory benchmark series (e.g., at Honolulu, HON). The source of this scatter may be ionospheric or fieldaligned currents seen by the satellites that are less prominent at ground; the amplitude of this scatter was larger 20142016, which may indicate a solar cycle dependence.
Figure 7 presents Observed Field (GVOOBS) and Core Field (GVOCORE) GVO estimates along with their \(\pm \sigma\) uncertainty, together with corresponding ordinary and revised ground observatory monthly means, from stations in the more challenging polar regions. At these locations, there are strong ionospheric Eregion currents lying between the satellites and the ground stations, and the satellites at times fly through intense fieldaligned currents. Nonetheless, the comparisons are encouraging and the trends seen at the ground stations are well captured by the GVO series. At the polar stations, the amplitude of the error bars has been significantly reduced for the Core Field GVO series compared to the Observed Field GVO series.
The radial component at high northern latitudes in Canada, at the Resolute Bay observatory (RES) inside the polar cap, shows a particularly clear annual variation in the monthly means, peaking in the northern summer. These fluctuations, which are likely due to farfield effects of polar electrojet currents, are well tracked by the GVO estimates.
Larger differences between the GVO and ground observatory series are seen in the eastward \(\phi\)component at these stations, the difference being largest from 2014 to 2017 (up to 25 nT seen at RES in summer months). The eastward \(\phi\)component in the GVO and ground stations agrees more closely at slightly lower latitudes in both the northern hemisphere (e.g., in Alaska at College station CMO, not shown here) and in the Southern hemisphere at Macquarie Island (MCQ), middle row Fig. 7. Ground stations in the auroral zone see signals in the southward \(\theta\)component that are less prominent in the GVO estimates; these may be caused by polar electrojet currents that are closer to the ground stations. At Mawson observatory in Antarctica (MAW) the southward \(\theta\)component has fluctuations of opposite sign to fluctuations seen at the same time in the GVO estimates. The relative position and orientations of the ionospheric currents and the ground and satellite observation points are clearly important for understanding such effects.
Figure 8 presents plots of the 1monthly revised monthly mean SV from ground observatories (black dots) and the 1monthly Core Field GVO SV series (red dots) at the three low/mid benchmark locations. Note the difference in scale here when looking at the secular variation, compared to the earlier plots that show the Observed Field/Core Field GVO values without taking annual differences.
The absolute levels (i.e., amplitude of secular variation) and trends (i.e., secular acceleration) in these benchmark ground observatory records of the core field secular variation are well matched by the Core Field SV GVO series. Peaks (secular variation impulses/geomagnetic jerks) such as that in the radial field at Honolulu (HON) in 2017 (Fig. 8, middle column, top row) are well captured and there is no indication of loss of temporal resolution in these annual difference secular variation series compared to the ground records. This indicates timedependent SV with time scales down to 1 year is well captured in the Swarm Core Field Secular Variation GVO product. The scatter is slightly larger in the GVO series for the southward \(\theta\)component and there are indications of remaining noise (perhaps to due ionospheric or interhemispheric fieldaligned currents) with period close to one year in the eastward \(\phi\)component. Figure 9 shows similar comparisons for a selection of the polar observatories. Here the scatter is larger in both the ground and GVO data, due to the difficult of isolating the core field signal, but again the observed trends agree well.
Figures 10 and 11 present plots of the 4monthly ground observatory SV (black dots) and 4monthly GVO SV time series (red dots) at the same three low/mid and polar latitude benchmark locations. Considering Fig. 10, the scatter observed in the 1monthly Core Field SV time series has been reduced and the independent ground and Swarm series show excellent agreement. The peak in the SV observed in the radial component at Honolulu (HON) in 2017 is again well captured. Differences are apparent at some epochs between the GVO series and the ground observatory series in the eastward \(\phi\)components, especially in 2015 and 2016 when solar activity was higher. This is particularly noticeable in the 4monthly SV series in January 2015 and January 2016 and seems to be related to the fields measured by the Swarm satellites during summer 2015 (see e.g., Fig. 10). Comparisons with ground observatories and internal field models such as CHAOS show a noticeable bias in the \(B_\phi\) component during this period which contributes to longer tails in the distribution of residuals for \(B_\phi\) all epochs and also results in enhanced rms differences for the \(\phi\)components of SV in comparison to ground observatories, see Table 4. A similar bias is also seen when comparing the original Swarm data to internal field models during summer 2015, particularly for Swarm B. The residuals during this time are largest in the northern polar region and seem to be geophysical in origin, perhaps related to strong fieldaligned currents measured by the satellites during this epoch.
Despite the slightly higher scatter at the polar stations in Fig. 11, the agreement is again encouraging with trends seen at ground stations being captured in the GVOs. Largest differences are seen in the horizontal components for Mawson station (MAW) in Antarctica where a sawtooth pattern about the ground series is visible in the 4monthly GVO estimates. This enhanced scatter is reflected in the error estimates supplied together with the GVO products, but illustrates that caution is needed when interpreting SV variations on interannual and shorter timescales in the auroral zone. Further work is required to better understand these features.
Discussion and conclusions
In Table 3 find that the 1monthly Swarm GVO products Observed Field series agree with independent ground observatory and field model predictions to within 5 nT in all components at nonpolar latitudes. Given that the requirement for a good standard (INTERMAGNET) ground observatory is an accuracy of 5 nT this indicates that the GVO method yields results comparable on these time scales with good ground observatories. The 4monthly estimates agree even better, to within 3 nT. Larger differences are found at polar latitudes where comparisons are complicated by the presence of strong ionospheric and magnetosphere–ionosphere coupling currents that have different signatures at ground and satellite altitude. The processing applied to obtain Core Field GVOs results in close agreement with ground observatory revised monthly means and with internal field models.
Taking annual differences to obtain SV estimates, further improves the agreement. We find the secular variation of the field intensity in the 1monthly Core Field GVOs agrees with six benchmark ground observatories from mid and low latitudes to a level of 1.8 nT/yr. For the 4monthly Core Field GVOs the difference to the secular variation recorded at the ground observatories decreases to 1.2 nT/yr. These numbers may be considered an upper bound on the accuracy of the Swarm GVO secular variation estimates, since they also include the measurement errors inherent in the ground observatories (perhaps 0.5 nT/yr at excellent observatories) as well as differences due to incomplete separation of noncore sources which will affect ground and GVO data in different ways.
In this paper, we have presented a global network of Geomagnetic Virtual Observatories constructed from vector magnetic field measurements made by the Swarm satellites. The series are provided in two variants, each with 1monthly and 4monthly cadences, and each with associated uncertainty estimates:
(1) ‘Observed’ magnetic field GVO series, with 1 and 4month cadence
(2) ‘Core’ magnetic field GVO series, and associated annual difference secular variation series, with 1 and 4month cadence.
Good agreement has been demonstrated between the Swarm GVO series, ground observatory data, and existing field models. The Swarm GVO series thus provide consistent and accurate global information on geomagnetic secular variation.
We recommend the Core Field GVOs along with their supplied error estimates for use in studies of core dynamics. Adopting the traditional approach of taking annual differences to obtain the SV helps avoid small annual signals that can remain in the Core Field series. For future work, we propose carrying out PCA denoising based on first differences of monthly GVOs, rather than annual differences, as a promising direction to further isolate core field signal.
Earlier versions of GVO series have already been used in inversions for the core surface flow (Kloss and Finlay 2019; Whaler and Beggan 2015) and in data assimilation studies where the core field signals seen in GVOs are combined with information from geodynamo models in order to estimate the state of the core (Barrois et al. 2018). GVO series are particularly well suited for global studies of rapid core dynamics where a number of physical hypotheses are currently under exploration (Aubert and Finlay 2019; Buffett and Matsui 2019; Gerick et al. 2020). The Observed Field GVOs provide additional information on longperiod variations of magnetospheric and ionsospheric origin. Longperiod magnetospheric variations may prove useful for deep electromagnetic induction studies (e.g. Harwood and Malin 1977). At high latitudes signatures of the polar electrojets are clearly seen in the 1monthly Observed Field GVO series, for example the distinctive annual variations in the vertical component seen in Figure 7, reflecting seasonal variations of the polar electrojet current system. Both applications will become increasingly attractive as the time series provided by the Swarm satellites lengthens.
The Swarm GVO dataset is now available as a regularly updated ESA product (see ftp://swarmdiss.eo.esa.int/Level2longterm/ ) updates will take place approximately every 4 months. Similarly processed GVO series from CHAMP, Cryosat2 and Ørsted are also available from the Swarm DISC GVO project webpage https://www.space.dtu.dk/english/research/projects/projectdescriptions/geomagneticvirtualobservatories.
Availability of datasets and materials
Regularly updated versions of the Swarm GVO data series are available at ftp://ftp.swarmdiss.eo.esa.int/Level2longterm/. Further details including additional documentation, GVO datasets from other satellites and software are available from the Swarm DISC GVO project webpage, https://www.space.dtu.dk/english/research/projects/projectdescriptions/geomagneticvirtualobservatories. Swarm data are available at https://earth.esa.int/web/guest/swarm/dataaccess. Ground observatory data are available from ftp://ftp.nercmurchison.ac.uk/geomag/Swarm/AUX_OBS/hour/. The RC index is available from http://www.spacecenter.dk/files/magneticmodels/RC/. The CHAOS7 model and its updates are available at http://www.spacecenter.dk/files/magneticmodels/CHAOS7/.
Change history
26 February 2021
Duplicated equations 4 & 6 have been removed.
Abbreviations
 AT:

Alongtrack
 CHAOS:

CHAMP, Ørsted, and Swarm field model
 CI:

Comprehensive inversion model
 DFT:

Discrete Fourier transform
 ECEF:

EarthCentered EarthFixed reference frame
 EW:

East–West
 GVO:

Geomagnetic Virtual Observatory
 IGRF:

International geomagnetic reference field
 IMF:

Interplanetary magnetic field
 INTERMAGNET:

International realtime magnetic observatory network
 Kp:

K planetary index
 LCS:

Lithospheric model from CHAMP and Swarm
 MF:

Main field
 nT:

NanoTesla
 OMM:

Observed monthly mean
 PC:

Principal component
 PCA:

Principal component analysis
 QD:

Quasidipole
 RC:

Ring current index
 rms:

Rootmean square
 RMM:

Revised monthly mean
 SH:

Spherical harmonic
 SHA:

Spherical harmonic analysis
 SV:

Secular variation
 DISC:

Data, innovation and science cluster
 yr:

Year
References
Alken P et al (2020a) Evaluation of candidate models for the 13th generation International Geomagnetic Reference Field. Earth Planets Space. https://doi.org/10.1186/s40623020012814
Alken P et al (2020b) International geomagnetic reference field: the thirteenth generation. Earth Planets Space. https://doi.org/10.1186/s4062302001288x
Aubert J, Finlay C (2019) Geomagnetic jerks and rapid hydromagnetic waves focusing at Earth’s core surface. Nat Geosci 12:393–398. https://doi.org/10.1038/s4156101903551
Backus G (1986) Poloidal and toroidal fields in geomagnetic field modelling. Rev Geophys 24:75–109
Backus G, Parker R, Constable C (1996) Foundations of Geomagnetism. Cambridge Univ. Press, New York
Barrois O, Hammer MD, Finlay CC, Martin Y, Gillet N (2018) Assimilation of ground and satellite magnetic measurements: inference of core surface magnetic and velocity field changes. Geophys J Int 215:695–712
Beggan CD, Whaler KA, Macmillan S (2009) Biased residuals of core flow models from satellitederived virtual observatories. Geophys J Int 177(2):463–475
Bendat J, Piersol A (2010) Random data, analysis and measurement procedures. Wiley, New Jersey
Brown W, Mound J, Livermore P (2013) Jerks abound: an analysis of geomagnetic observatory data from 1957 to 2008. Phys Earth Planet Int 223:62–76
Buffett B, Matsui H (2019) Equatorially trapped waves in Earth’s core. Geophys J Int 218(2):1210–1225
Burrell A, Meeren CVD, Laundal KM (2020) aburrell/aacgmv2: Version 2.6.0, https://doi.org/10.5281/ZENODO.3598705
Constable C (1988) Parameter estimation in nonGaussian noise. Geophys J Int 94(1):131–142
Cox G, Brown W, Billingham L, Holme R (2018) Magpysv: a python package for processing and denoising geomagnetic observatory data. Geochem Geophys Geosyst 19(9):3347–3363
Cox G, Brown W, Beggan C, Hammer M, Finlay C (2020). Denoising Swarm geomagnetic virtual observatories using principal component analysis. https://doi.org/10.5194/egusphereegu20209957
Domingos J, Pais MA, Jault D, Mandea M (2019) Temporal resolution of internal magnetic field modes from satellite data. Earth Planets Space 71(1):1–17
Finlay CC, Olsen N, Kotsiaros S, Gillet N, TøffnerClausen L (2016) Recent geomagnetic secular variation from Swarm and ground observatories as estimated in the CHAOS6 geomagnetic field model. Earth Planets Space 68(1):1–18
Finlay CC, Kloss C, Olsen N, Hammer MD, TøffnerClausen L, Grayver A, Kuvshinov A (2020) The CHAOS7 geomagnetic field model and observed changes in the South Atlantic Anomaly. Earth Planets Space 72(1):1–31. https://doi.org/10.1186/s40623020012529
Gerick F, Jault D, Noir J (2020) Fast quasigeostrophic magnetocoriolis modes in the Earth’s core, 856 Geophys. Res Lett. https://doi.org/10.1029/2020GL090803
Hammer MD (2018) Local estimation of the Earth’s core magnetic field, Ph.D. thesis, Technical University of Denmark
Harwood JM, Malin SRC (1977) Sunspot cycle influence on the geomagnetic field. Geophys J Int 50(3):605–619. https://doi.org/10.1111/j.1365246X.1977.tb01337.x
Kauristie K, Morschhauser A, Olsen N, Finlay C, McPherron R, Gjerloev J, Opgenoorth H (2017) On the usage of geomagnetic indices for data selection in internal field modelling. Space Sci Rev. 206:61–90. https://doi.org/10.1007/s1121401603010
Kloss C, Finlay CC (2019) Timedependent low latitude core flow and geomagnetic field acceleration pulses. Geophys J Int 217:140–168
Leopardi P (2006) A partition of the unit sphere into regions of equal area and small diameter. Electronic Trans Numerical Anal 25(12):309–327
Lesur V, Heumez B, Telali A, Lalanne X, Soloviev A (2017) Estimating error statistics for ChambonlaForêt observatory definitive data. Annales Geophysicae 35(4):939–952. https://doi.org/10.5194/angeo359392017
Macmillan S, Olsen N (2013) Observatory data and the Swarm mission. Earth Planets Space 65(11):1355–1362. https://doi.org/10.5047/eps.2013.07.011
Mandea M, Olsen N (2006) A new approach to directly determine the secular variation from magnetic satellite observations. Geophys Res Lett 33(15):L15306
Olsen N (1997) Ionospheric F region currents at middle and low latitudes estimated from Magsat data. J Geophys Res Space Phys 102(A3):4563–4576
Olsen N, Mandea M (2007) Investigation of a secular variation impulse using satellite data: the 2003 geomagnetic jerk. Earth Planet Sci Lett 255(1):94–105
Olsen N, Mandea M, Sabaka TJ, TøffnerClausen L (2009) CHAOS2—a geomagnetic field model derived from one decade of continuous satellite data. Geophys J Int 179(3):1477–1487
Olsen N, Mandea M, Sabaka TJ, TøffnerClausen L (2010) The CHAOS3 geomagnetic field model and candidates for the 11th generation IGRF. Earth Planets Space 62(10):719–727
Olsen N, Lühr H, Finlay CC, Sabaka TJ, Michaelis I, Rauberg J, TøffnerClausen L (2014) The CHAOS4 geomagnetic field model. Geophys J Int 197(2):815–827
Olsen N et al (2015) The Swarm Initial Field Model for the 2014 geomagnetic field. Geophys Res Lett 42(4):1092–1098
Olsen N, Ravat D, Finlay CC, Kother LK (2017) LCS1: a highresolution global model of the lithospheric magnetic field derived from CHAMP and Swarm satellite observations. Geophys J Int 211(3):1461–1477
Rogers HF, Beggan CD, Whaler KA (2019) Investigation of regional variation in core flow models using spherical slepian functions. Earth Planets Space 71(1):19
Sabaka TJ, Olsen N, Purucker ME (2004) Extending comprehensive models of the Earth’s magnetic field with Ørsted and CHAMP data. Geophys J Int 159(2):521–547
Sabaka TJ, Hulot G, Olsen N (2010) Mathematical properties relevant to geomagnetic field modeling, in Handbook of Geomathematics. Springer: Berlin. pp. 503–538
Sabaka TJ, TøffnerClausen L, Olsen N (2013) Use of the Comprehensive Inversion Method for Swarm satellite data analysis. Earth, Planets and Space 65:1201–1222
Sabaka TJ, TøffnerClausen L, Olsen N, Finlay CC (2018) A comprehensive model of the Earth’s magnetic field determined from 4 years of Swarm satellite observations. Earth Planet Space 70(1):130
Shepherd SG (2014) Altitudeadjusted corrected geomagnetic coordinates: definition and functional approximations. J Geophys Res Space Phys 119(9):7501–7521
Shore RM (2013) An improved description of Earth’s external magnetic fields and their source regions using satellite data, Ph.D. thesis, The University of Edinburgh
Wardinski I, Holme R (2011) Signal from noise in geomagnetic field modelling: denoising data for secular variation studies. Geophys J Int 185(2):653–662
Whaler K, Beggan C (2015) Derivation and use of core surface flows for forecasting secular variation. J Geophys Res Solid Earth 120(3):1400–1414
Whaler KA (2017) Probing the core surface flow with satellite data, IAGA Joint Assembly Session A02—Earth’s core dynamics and planetary dynamos (DIV I)
Acknowledgements
We wish to thank the European Space Agency (ESA) for the prompt availability of Swarm L1b data. The staff of the geomagnetic observatories and INTERMAGNET are thanked for supplying highquality observatory data. Highresolution 1min OMNI data were provided by the Space Physics Data Facility (SPDF), NASA Goddard Space Flight Center. We like to thank two anonymous reviewers for comments that helped improve the manuscript.
Funding
This study was funded by ESA through the Swarm DISC GVO project, contract no. 4000109587.
Author information
Authors and Affiliations
Contributions
MDH developed the Swarm GVO data processing and modeling scheme and drafted the manuscript. GAC developed the PCA denoising scheme with assistance from WJB, applied it to the one monthly series and wrote the related part of the manuscript. CCF and CDB designed the project and contributed to the writing of the manuscript. All authors read and approved the final manuscript.
Corresponding author
Ethics declarations
Competing interests
The authors declare that they have no competing interests.
Additional information
Publisher’s note
Springer Nature remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.
Rights and permissions
Open Access This article is licensed under a Creative Commons Attribution 4.0 International License, which permits use, sharing, adaptation, distribution and reproduction in any medium or format, as long as you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons licence, and indicate if changes were made. The images or other third party material in this article are included in the article's Creative Commons licence, unless indicated otherwise in a credit line to the material. If material is not included in the article's Creative Commons licence and your intended use is not permitted by statutory regulation or exceeds the permitted use, you will need to obtain permission directly from the copyright holder. To view a copy of this licence, visit http://creativecommons.org/licenses/by/4.0/.
About this article
Cite this article
Hammer, M.D., Cox, G.A., Brown, W.J. et al. Geomagnetic Virtual Observatories: monitoring geomagnetic secular variation with the Swarm satellites. Earth Planets Space 73, 54 (2021). https://doi.org/10.1186/s40623021013579
Received:
Accepted:
Published:
DOI: https://doi.org/10.1186/s40623021013579