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The static part of the internal field to degree and order 40 for the two parent models and to degree and order 60 for Pomme-6 2.
Table 1 Root mean square and mean differences (in nT) for the two parent models and for Swarm A and C. The B misfit corresponds to intensity rms difference computed from the VFM dataset.
It was constructed with the help of models Ørsted 09d/04) and Ørsted 09g/04) of Olsen et al. (2005) and POMME-3.0 of Maus et al. (2006), all of which contributed to IGRF-10 or came directly from IGRF-10 parent models and are freely available.
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Figure 6 Mean and root mean square of the residuals between parent model and input satellite data.
Figure 5 Mean of the residuals between parent model and input satellite data for each magnetic component.
We also describe the parent model and the process used to fit its parameters, and we describe the core-flow method of modelling and predicting secular variation.
Different components may come from a same parent model and different models may provide similar components, which have different internal structures and calculations but perform the same functionality.
In Section 3 we describe the parent model and the process used to fit its parameters, while in Section 4 we evaluate the model coefficients.
The production of our BGS candidate models was carried out in three steps: selection of data from Ørsted, CHAMP, and ground observatories; fitting and evaluating the parent model; and finally extraction of the IGRF-11 candidate MF and SV coefficients.
Table 3 shows the global RMS differences between the BGS candidate, derived from the parent model and core-flow prediction, and those of other institutes, computed at the reference radius of 6,371.2 km.
There is also some evidence of periodic, possibly annual, signals in these data, too. Figure 8 Mean and root mean square of the residuals between parent model and input observatory data.
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