Mass-related excitation of polar motion: an assessment of the new RL06 GRACE gravity field models

Abstract

The new Release-06 (RL06) Gravity Recovery and Climate Experiment (GRACE) gravity field solutions are evaluated by converting them into equatorial effective angular momentum functions (so-called excitation functions) for polar motion and comparing these to respective time series based on space-geodetic observations (geodetic excitation). The same is performed for the older RL05 solutions using identical processing. Maps of equivalent water heights derived from both releases show that the signal-to-noise ratio is significantly improved in RL06. The derived polar motion excitation functions from RL05 and RL06 differ by about 15$\%$. An analysis of the contributions of different Earth subsystems revealed that the release update mainly influenced the hydrological (12$\%$) and oceanic excitations (17$\%$), but it has a relatively small impact on the cryospheric excitations related to Antarctica (4$\%$) and Greenland (1$\%$). The RL06 data from different GRACE processing centers are more consistent among each other than the previous RL05 data. Comparisons of the GRACE-based excitation functions with the geodetic and model-based oceanic excitations show that the latest release update improved the agreement by about 2 to 15 percentage points.

Introduction

Mass displacements within the Earth system cause variations of the Earth’s gravity field and its rotation. Thus, temporal variations of the gravity field can be used to study the mass-related excitation of polar motion. By separating the observed integral gravity signal into contributions from different Earth subsystems, also individual mechanisms of polar motion excitation can be studied. Most important are the variations of the degree-2 spherical harmonic potential coefficients ${C}_{21}$ and ${S}_{21}$ as these are directly related to polar motion excitation (Barnes et al. 1983).

Between 2002 and 2017, the satellite gravity mission Gravity Recovery and Climate Experiment (GRACE) observed the time variable gravity field of the Earth. The GRACE science teams at the Center for Space Research (CSR), Austin, the GeoForschungsZentrum (GFZ), Potsdam, and the Jet Propulsion Laboratory (JPL), Pasadena, provide monthly GRACE gravity field solutions. In irregular time intervals release updates were performed: 2003 (RL01), 2005 (RL02 and RL03), 2007 (RL04), 2012 (RL05) and recently in 2018 (RL06). A lot of studies exist in which GRACE RL05 gravity field solutions have been used to estimate the integral as well as individual mass-related effects on Earth rotation (e.g., Adhikari and Ivins 2016; Chen et al. 2013, 2017; Göttl et al. 2015; Malgorzata et al. 2017; Meyrath and van Dam 2016). It was shown that due to the release update from RL04 to RL05 the agreement between GRACE-derived effective angular momentum functions and the mass-related part of the so-called geodetic excitations (Brzeziński 1992) could be slightly improved. The latter can be derived from Earth Orientation Parameter (EOP) time series, such as EOP 14 C04 (Bizouard et al. 2014) of the International Earth Rotation and Reference Systems Service (IERS), reduced by the motion-related effects within the atmosphere (winds) and oceans (currents) based on geophysical model data. Recently, CSR, JPL and GFZ have produced the new RL06 GRACE gravity field solutions applying improved parameters, processing algorithms, data editing and background gravity models. Accordingly, the Institute of Theoretical Geodesy and Satellite Geodesy (ITSG) of the Graz University of Technology provides the new ITSG-Grace2018 monthly and daily gravity field models which also incorporate the new RL06 background gravity models. In particular, the degree-2 potential coefficients ${C}_{21}$ and ${S}_{21}$ are influenced by the change of the mean pole model from cubic to linear. The goal of this study is to analyze the new RL06 GRACE data regarding its consistency with the mass-related part of the geodetic excitation of polar motion (integrally and for individual subsystems), to quantify the improvement of RL06 data with respect to RL05, and to study the differences of the solutions from CSR, JPL, GFZ and ITSG.

The paper is outlined as follows: the next section provides an overview of the GRACE gravity field models [RL05 and RL06 from CSR, JPL and GFZ as well as the GRACE gravity field models ITSG-Grace2016 (incorporating the RL05 background models) and ITSG-Grace2018 (incorporating the RL06 background models)] and the processing steps in order to determine the equatorial effective angular momentum functions for polar motion excitation. Further, we introduce the time series EOP 14 C04 and the steps for the separation of the mass-related part of the geodetic excitation that will be used for the comparison with the GRACE-derived excitation in the third section. There, also maps of equivalent water heights from GRACE RL05 and RL06 data are analyzed with respect to the signal-to-noise ratio and the consistency of the solutions of the processing centers. Finally, the last section provides the conclusions.

Data and data processing

GRACE gravity field solutions

In this study, we use the RL05 and the new RL06 GRACE gravity field solutions from CSR, JPL and GFZ, namely CSR RL05 (Bettadpur 2012), CSR RL06 (Bettadpur 2018), JPL RL05¹ (Watkins and Yuan 2014), JPL RL06 (Yuan 2018), GFZ RL05² (Dahle et al. 2012) and GFZ RL06 (Dahle et al. 2018). Further, we use the GRACE gravity field solutions from ITSG, namely ITSG-Grace2016 (Mayer-Gürr et al. 2016) and ITSG-Grace2018 (Mayer-Gürr et al. 2018). Beside changes in the processing algorithms and data editing, there are also significant changes in the background models as shown in Table 1. The GRACE gravity field solutions are provided as Level-2 products GSM³, GAC⁴ and GAD⁵. Figure 1 shows the time series of the potential coefficients ${C}_{21}$ and ${S}_{21}$ of the CSR RL05 and RL06 GSM products. A significant modification of these coefficients was caused in particular by the change of the mean pole model from cubic to linear. The introduction of a new mean pole model was motivated by a significant mismatch between the cubic polygon fitted to a filtered time series of polar motion and the observed polar motion after 2010. Accordingly, the IERS Conventions (Petit and Luzum 2010) have been updated by a new conventional linear mean pole model based on the full extent of the IERS EOP C01 series (1900–2017). The relative standard deviations (RSD) of CSR RL05 and RL06 for ${C}_{21}$ and ${S}_{21}$ are up to 32$\%$. The RL06 solution is smoother, especially for ${S}_{21}$, and changes of the trend are clearly visible. The new RL06 GRACE Atmosphere and Ocean De-Aliasing Level-1B (AOD1B) product (Dobslaw et al. 2017b) provides, compared to its predecessor in RL05 (Flechtner et al. 2015), an increased temporal and spatial resolution, a clear separation of tidal and non-tidal signals and an improvement of long-term consistency (Dobslaw et al. 2017a). The oceanic component is no longer based on the Ocean Model for Circulation and Tides (OMCT; Dobslaw et al. 2013) but on the Max-Planck-Institute Ocean Model (MPIOM; Jungclaus et al. 2013), while the atmospheric component is still based on atmospheric re-analysis of the European Center for Medium-Range Weather Forecasts (ECMWF). The a posteriori correction models GAE, GAF and GAG of the AOD1B RL05 product (Fagiolini et al. 2015) that account for updates at ECMWF, are no longer necessary for RL06. However, the impact of the changes in the AOD1B product on the coefficients ${C}_{21}$ and ${S}_{21}$ is small (14$\%$ for ${C}_{21}$ and 8$\%$ for ${S}_{21}$).

Table 1 Background models used within the RL05 and RL06 GRACE gravity field processing

Fig. 1

Comparison of the CSR RL05 (blue) and CSR RL06 (red) solutions for the normalized spherical harmonic potential coefficients $\Delta \bar{C}_{21}$ and $\Delta \bar{S}_{21}$ (mean values of the time series are removed). The corresponding correlation coefficient and relative standard deviation (RSD) are provided

The coefficients ${C}_{21}$ and ${S}_{21}$ are proportional to the mass-related part of the equatorial effective angular momentum functions $\chi _1^{{\rm mass}}$ and $\chi _2^{{\rm mass}}$ that describe the excitation of polar motion (e.g., Barnes et al. 1983; Gross 2007; Wahr 2005). Conversion formulas given by Göttl (2013) are used here. While the integral excitation can be derived directly from the sum of the GSM and GAC products, individual contributions of the continental hydrosphere $\chi ^{H}$, oceans $\chi ^{O}$, Antarctica $\chi ^{A}$ and Greenland $\chi ^{G}$ are computed from the sum of the GSM and GAD products by applying adequate filter techniques, masks and global spherical harmonic synthesis/analysis. In this study, we use different versions of the anisotropic decorrelation filter DDK (Kusche 2007) in order to demonstrate that the signal-to-noise ratio could be significantly improved due to the release update. The degree-1 Stokes coefficients are replaced by solutions from Swenson et al. (2008) derived from GRACE data and ocean model outputs in order to account for the fact that mass displacements are referenced to a coordinate system attached to the Earth’s crust which moves relative to the Earth’s center-of-mass frame used in the GRACE data processing. Furthermore, as recommended, the inaccurate ${C}_{20}$ coefficient of the GSM product is replaced by an improved external satellite laser ranging (SLR) solution from Cheng et al. (2013) based on GRACE RL05 (GRACE Technical Note 07) or on GRACE RL06 (GRACE Technical Note 11), respectively. In order to identify individual excitations of polar motion, the effect of glacial isostatic adjustment (GIA) must be removed from the GRACE observations. We use the global GIA model IJ05_R2 from Ivins et al. (2013).

Polar motion

Polar motion values are taken from the time series EOP 14 C04 of the IERS which is based on a combination of space-geodetic observation techniques (Bizouard et al. 2014). The daily pole coordinates x and y are fully consistent with the International Terrestrial Reference Frame 2014 (ITRF2014), and the mean uncertainties of the pole coordinates are below 40 μas. From this time series, the so-called geodetic excitation of polar motion, i.e., the equatorial effective angular momentum functions $\chi ^{C04}$, are determined by applying the conversion formulas given by Gross (1992). They represent the combined excitation from the redistribution of masses (mass effect) and their motion (motion effect) within the Earth system. In order to compare the GRACE-derived excitation with the geodetic excitation, the motion-related part needs to be reduced from the latter. This is achieved by using the geophysical model data described below.

Geophysical models

For the reduction of the motion-related part from the geodetic excitation, we apply geophysical model data describing the effects of wind and ocean currents as provided by the Global Geophysical Fluids Center (GGFC) of the IERS. These data are derived from two consistent atmosphere/ocean model combinations: The atmospheric re-analysis from NCEP (National Centers for Environmental Prediction; Zhou et al. 2006) in combination with the ocean model ECCO (Estimating the Circulation and Climate of the Ocean; ftp://euler.jpl.nasa.gov/sbo/oam_global/ECCO_kf079.chi) (henceforth referred to as NE), and the atmospheric and oceanic effective angular momentum functions computed by the Earth System Modelling group at Deutsches GeoForschungsZentrum (ESMGFZ) based on operational and re-analysis data from the ECMWF and the ocean model MPIOM (henceforth referred to as ESMGFZ; Dobslaw and Dill 2018). Due to the fact that the modeled motion-related effective angular momentum functions suffer from model uncertainties (in particular due to a lack of precise measurements of wind and ocean velocities on global scale), the remaining mass-related part of the geodetic excitation of polar motion $\chi ^{C04-{\rm NE}}$ and $\chi ^{\rm C04-ESMGFZ}$ is afflicted with some (unknown) uncertainty. For a comparison with the GRACE-derived oceanic excitation, we will later use the mass-related parts of the two oceanic excitation series from the ocean model ECCO and from ESMGFZ. The latter combines the effective angular momentum functions for the dynamic ocean (OAM) and for the barystatic sea-level (SLAM) to take into account the inflow of terrestrial water into the oceans.

Results and comparisons

Mass redistribution within the Earth system

Mass changes within the Earth system are commonly expressed in terms of equivalent water heights (Wahr et al. 1998). Figure 2 shows the standard deviations of the GRACE-based equivalent water heights over 13 years (2003–2015) by applying the filters DDK3 ($a=10^{12}$, $p=4$) or DDK2 ($a=10^{13}$, $p=4$) in order to reduce the meridional stripes in the RL05 and RL06 GRACE gravity field solutions. The signal is significantly larger over the continents than over the oceans (the color bar of the figure is selected to visualize the differences over the oceans). One can see that the signal-to-noise ratio is significantly improved by the release update. The reduction of the meridional stripes with the DDK3 filter is much more effective for RL06 than for RL05. The signal-to-noise ratio of the solutions RL06 DDK3 lies in between the signal-to-noise ratios of the solutions RL05 DDK3 and RL05 DDK2. The RL06 DDK2 solutions are even smoother than the RL05 DDK2 solutions.

Fig. 2

Standard deviations of equivalent water heights over 13 years (2003–2015) derived from different GRACE gravity field solutions by applying different versions of the DDK filter: CSR RL05 DDK3 (top, left), CSR RL05 DDK2 (top middle), CSR RL06 DDK3 (middle, left), CSR RL06 DDK2 (middle, middle). Furthermore the following differences are shown: CSR RL05 DDK3–CSR RL05 DDK2 (top, right), CSR RL06 DDK3–CSR RL06 DDK2 (middle, right), CSR RL05 DDK3–CSR RL06 DDK3 (bottom, left), CSR RL05 DDK2–CSR RL06 DDK2 (bottom, middle) and CSR RL05 DDK2–CSR RL06 DDK3 (bottom, right)

Figure 3 provides the empirical standard deviations of the GRACE RL05 and RL06 fields of equivalent water heights (DDK2 filter applied) from CSR, JPL, and GFZ as well as from the two ITSG solutions. Due to different processing strategies and background models (see Table 1), the equivalent water heights differ significantly in all solutions. The empirical standard deviations of the RL06 residuals are on average 0.7 cm for CSR, 0.6 cm for JPL, 0.7 cm for GFZ, and 0.7 cm for ITSG, whereas the empirical standard deviations of the RL05 residuals are on average 0.9 cm for CSR, 1.3 cm for JPL, 1.2 cm for GFZ, and 0.8 cm for ITSG. Especially in the polar regions and mid-latitudes, the differences between the solutions from CSR, JPL, GFZ and ITSG are clearly reduced by the release update. Among the RL05 models, the ITSG-Grace2016 monthly solution exhibits the smallest empirical standard deviation. For RL06, the empirical standard deviations of all investigated solutions are quite similar.

Fig. 3

Empirical standard deviations of GRACE RL05 and RL06 equivalent water height solutions (2004–2014): CSR RL05 DDK2, JPL RL05 DDK2, GFZ RL05 DDK2, ITSG-Grace2016 DDK2 (top, from left to right), CSR RL06 DDK2, JPL RL06 DDK2, GFZ RL06 DDK2, ITSG-Grace2018 DDK2 (bottom, from left to right)

Polar motion excitation: integral effect

As mentioned before, equatorial effective angular momentum functions describing the integral mass-related part of the excitation functions of polar motion can directly be derived from the potential coefficients ${C}_{21}$ and ${S}_{21}$ (GSM + GAC). In this conversion, no filtering of the GRACE gravity field solutions is required. Figure 4 shows the equatorial effective angular momentum functions from GRACE (CSR RL05 and RL06). A difference in the trend is clearly visible for $\chi _1^{{\rm mass}}$ as well as for $\chi _2^{{\rm mass}}$ . The RSD of the polar motion excitation functions amount to 15$\%$.

Fig. 4

Comparison of the equatorial effective angular momentum functions $\chi _1^{{\rm mass}}$ and $\chi _2^{{\rm mass}}$ computed from CSR RL05 (blue) and CSR RL06 (red) (mean values of the time series are removed). The corresponding correlation coefficients and relative standard deviations (RSD) are provided

In analogy to the previous section, we also investigate the differences of the excitation functions derived from the GRACE RL06 solutions from CSR, JPL, and GFZ and ITSG-Grace2018. Like for the equivalent water heights, the differences between the excitation functions from the different GRACE solutions are much smaller for RL06 than for RL05 (see Fig. 5 and Table 2). The release update improves the agreement of the derived $\chi _1^{{\rm mass}}$ series by about 5 percentage points; the improvement for $\chi _2^{{\rm mass}}$ is a bit smaller (about 3 percentage points). ITSG-Grace2016 shows the smallest empirical standard deviation among the RL05 solutions, while CSR shows the smallest empirical standard deviation among the RL06 solutions.

Fig. 5

Differences of the equatorial effective angular momentum functions $\chi _1^{{\rm mass}}$ and $\chi _2^{{\rm mass}}$ from GRACE RL05 (blue) and RL06 (red) data with respect to the mean excitation functions

Table 2 Empirical standard deviations (mas) of the RL05 and RL06 GRACE-based equatorial effective angular momentum functions

The GRACE-based effective angular momentum functions are compared with the reduced geodetic excitations (mass-related part) $\chi ^{\rm C04-NE}$ and $\chi ^{\rm C04-ESMGFZ}$. Table 3 shows the root mean square (RMS) differences and correlation coefficients between the excitation functions derived from GRACE data (CSR RL05, CSR RL06, JPL RL05, JPL RL06, GFZ RL05, GFZ RL06, ITSG-Grace2016, ITSG-Grace2018) and the excitation functions based on space-geodetic observations. It can be seen that the agreement could be significantly improved by the release update, especially in the case of JPL. The best agreement can be seen between the excitation functions from ITSG-Grace2018 and C04-NE.

Table 3 RMS differences (mas)/correlation coefficients between the GRACE-based equatorial effective angular momentum functions and the mass-related part of the geodetic excitation of polar motion

Polar motion excitation: individual effects from subsystems

This section presents an analysis of the contributions of individual Earth subsystems to the mass-related excitation of polar motion. Therefore, the integral GRACE signal needs to be separated using filter techniques and masks. As shown before, the signal-to-noise ratio of the GRACE results could be significantly improved by the release update from RL05 to RL06. Thus, it can be expected that also the quantification of individual mass-related contributions to polar motion excitation on the basis of GRACE observations benefits strongly from the improvement. Figure 6 shows the resulting excitation functions from CSR RL05 DDK2 and CSR RL06 DDK2 for the mass effects of the continental hydrosphere $\chi ^{H}$, the oceans $\chi ^{O}$, and the cryosphere. The latter are presented separately for Antarctica $\chi ^{A}$ and Greenland $\chi ^{G}$. Larger discrepancies between the old and new releases are visible for $\chi ^{H}$ (${\rm RSD}=12\%$) and $\chi ^{O}$ (${\rm RSD}=17\%$). This can be explained by the fact that the change of the $C_{21}$ series in the course of the release update has a dominant effect on the oceanic mass estimates, and changes in $S_{21}$ dominate the mass estimates in the continental regions of North America, South America and Asia as well as in the Indian Ocean (see Fig. 7). In contrast, the changes for $\chi ^{A}$ (${\rm RSD}=4\%$) and $\chi ^{G}$ (${\rm RSD}=1\%$) are relatively small as the mass estimates for Antarctica and Greenland are only slightly influenced by the change of the potential coefficients $C_{21}$ and $S_{21}$ from RL05 to RL06. Figure 8 shows the differences of the excitation functions from the CSR, JPL, GFZ and ITSG GRACE gravity models with respect to the mean of all four excitation functions. The corresponding empirical standard deviations are given in Table 4. The release update improved the agreement between the four GRACE solutions by about 7 percentage points for $\chi _1^{O}$, 4 percentage points for $\chi _2^{H}$, 1 percentage point for $\chi _2^{A}$, and only 0.2 percentage points for $\chi _2^{G}$. Note that for the oceans $\chi _1$ is the prominent component, whereas $\chi _2$ is dominant for continental hydrology, Antarctica and Greenland. Again, ITSG-Grace2016 exhibits the smallest empirical standard deviation among the RL05 solutions, while CSR features the smallest empirical standard deviation among the RL06 solutions.

Fig. 6

Excitation functions from CSR RL05 DDK2 (blue) and CSR RL06 DDK2 (red) for the mass effects of the continental hydrosphere $\chi ^{H}$, the oceans $\chi ^{O}$, Antarctica $\chi ^{A}$ and Greenland $\chi ^{G}$ (mean values of the time series are removed)

Fig. 7

Standard deviations of equivalent water height differences between the two CSR solutions (RL05 DDK2–RL06 DDK2) using only the potential coefficients $C_{21}$ (left) and $S_{21}$ (right) over 13 years (2003–2015)

Fig. 8

Differences of the excitation functions for the mass effects of the continental hydrosphere $\chi ^{H}$, the oceans $\chi ^{O}$, Antarctica $\chi ^{A}$ and Greenland $\chi ^{G}$ derived from GRACE RL05 (blue) and RL06 (red) data with respect to the mean excitation functions

Table 4 Empirical standard deviations (mas) of the GRACE-based equatorial effective angular momentum functions for the continental hydrosphere (H), oceans (O), Antarctica (A) and Greenland (G)

In Fig. 9 and Table 5, we present a comparison of the GRACE-derived individual polar motion excitation functions with independent data exemplarily for the oceans (model results for the contributions of the continental hydrosphere and the two continental ice sheets are characterized by higher uncertainties). The polar motion excitation functions for the oceanic mass effect from GRACE data and from ocean models differ significantly with respect to their trends. However, the trends of the ocean models cannot be viewed as realistic as they are Boussinesq models that conserve volume rather than mass. Mass conservation is reached by adding a homogeneous shell of mass at every time step. Therefore, the trends of all series are reduced before the computation of RMS differences and correlation coefficients (Table 5). The update from RL05 to RL06 improved the agreement of the GRACE-derived oceanic effective angular momentum functions with modeled mass-related oceanic polar motion excitation functions by about 5 percentage points for CSR, 15 percentage points for JPL, 4 percentage points for GFZ and 5 percentage points for ITSG. In general, the agreement of the GRACE-derived oceanic effective angular momentum functions with ocean model results from ESMGFZ is better than with ocean model results from ECCO. The best agreement can be seen between the oceanic effective angular momentum functions from ITSG-Grace2018 and ESMGFZ (OAM + SLAM).

Fig. 9

Mass-related oceanic polar motion excitation functions derived from GRACE RL05 (blue) and RL06 (red) data as well as from the ocean model ECCO and the model results from ESMGFZ (OAM + SLAM) (green)

Table 5 RMS differences (mas)/correlation coefficients between the GRACE-based equatorial effective angular momentum functions for the oceanic mass effect and ocean model results

Conclusion

With the GRACE Release 06 solution, the estimation of mass redistributions has significantly been improved, and the noise in the GRACE gravity field solutions has been reduced. Furthermore, the consistency of the analyzed GRACE solutions of CSR, JPL, GFZ and ITSG was increased. Concerning polar motion excitation, in particular the change in the potential coefficients ${C}_{21}$ and ${S}_{21}$ (about 32$\%$ RL05/RL06) due to the change of the mean pole model from cubic to linear plays a great role. On the other hand, the update of the AOD1B product has only a minor influence. The changes in the potential coefficients ${C}_{21}$ and ${S}_{21}$ amount to only 14 and 8$\%$ respectively. While the integral effect of the mass-related polar motion excitation can be directly derived from the potential coefficients ${C}_{21}$ and ${S}_{21}$ (GSM + GAC), the determination of individual contributions from the Earth’s subsystems is based on the full set of potential coefficients (GSM + GAD) and requires adequate filtering and masking. Due to the improvement of the signal-to-noise ratio in the RL06 gravity field models, the decorrelation filter DDK3 delivers good results (this is not the case for the RL05 gravity field models). Looking at the GRACE-based results for the integral mass-related polar motion excitation, the change due to the update from RL05 to RL06 is about 15$\%$. The changes of the time series of ${C}_{21}$ and ${S}_{21}$ have a large impact on the oceanic (17$\%$) and hydrological excitation (12$\%$), but the effect on the contributions from ice loss in Antarctica (4$\%$) and Greenland (1$\%$) is small. The trend, in particular of the oceanic mass variation, is significantly reduced in RL06, and the agreement of the excitation functions computed from the CSR, JPL, GFZ and ITSG solutions was improved. For the integral polar motion excitation, the empirical standard deviations of the four solutions amount to 3.8 to 7.3 mas for RL05 and only to 2.2 to 3.9 mas for RL06. The largest improvement can be seen for the mass-related polar motion excitation of the ocean (7 percentage points), followed by the continental hydrology (4 percentage points), Antarctica (1 percentage point) and Greenland (0.2 percentage points). A validation with external results is difficult due to the relatively large uncertainties of geophysical models. For the ocean, our results showed that the latest release update led to a generally higher agreement between the excitation functions from GRACE and model data (improvement 4 to 15 percentage points), where the excitation functions from the ITSG-Grace2018 solution and from the ESMGFZ model agree best. The agreement of the GRACE-derived effective angular momentum functions with the mass-related part of the geodetic excitation could be improved by 2 to 7 percentage points due to the release update. The time series of polar motion excitation derived from ITSG-Grace2018 and C04-NE shows the highest agreement.