Neural network modeling of solar wind-magnetosphere interaction

Details Neural network modeling of solar wind-magnetosphere interaction Neural network modeling of solar wind-magnetosphere interaction

Jul 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997jgr...10214457w&link_type=abstract

Journal of Geophysical Research, Volume 102, Issue A7, p. 14457-14466

Physics

20

Ionosphere: Modeling And Forecasting, Magnetospheric Physics: Solar Wind/Magnetosphere Interactions, Magnetospheric Physics: Storms And Substorms, Magnetospheric Physics: Instruments And Techniques

Scientific paper

We study solar wind-magnetosphere interaction using partially recurrent neural networks to find the best coupling functions. Hourly data of the solar wind and Dst are selected, from the period 1963 to 1992, covering 10,554 hours. The best coupling functions are found from the out-of-sample performance of trained neural networks, which are then compared with those obtained from cross-correlation analyses. In most cases, good agreement is found. This indicates that cross-correlation analysis can be used to optimize input parameters for neural networks, albeit at a limitation due to the assumption of linearity. However, there exist exceptions where coupling functions strongly correlated with Dst give poor predictions. Based on neural network modeling, if we take the coupling function in the form of PλVμBsν, then the conditions, 0<=λ<=1, 0.5<μ<=2 and 0.5<=ν<=2, will result in solar wind input functions well suited for predicting geomagnetic storms, e.g., P1/4VBs, P1/6VBs, P1/5VBs, P1/3VBs, P1/2VBs, V2Bs, and VBs. In contrast, ɛ and the polar cap potential are less good candidates for storm predictions. Therefore the best coupling functions do not necessarily have the dimension of power, energy or electric field. Furthermore, we predict geomagnetic storms up to five hours in advance with good accuracy from the best coupling functions. The confidence limits on the prediction accuracy are computed to show the statistical significance of the predictions and to confirm the best coupling functions. Finally, we discuss how the partially recurrent network models solar wind-magnetosphere interaction.

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