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The structure and dynamics of the magnetospheres of the outer planets,particularly Saturn and Jupiter, have been explored both through remote andin-situ observations. Interpreting these observations often necessitatessimultaneous knowledge of the solar-wind conditions impinging on themagnetosphere. Without an available upstream monitor, solar-wind context istypically provided using models initiated with either the output ofmagnetogram-constrained coronal models or, more commonly, in-situ observationsfrom 1 AU. While 1-AU observations provide a direct measure of solar windconditions, they are single-point observations and thus require interpolationto provide inputs to outer-heliosphere solar-wind models. In this study we testthe different interpolation methods using synthetic 1-AU observations oftime-evolving solar-wind structure. The simplest method is "corotation", whichassumes solar-wind structure is steady state and rotates with the Sun. Thismethod of reconstruction produces discontinuities in the solar-wind inputs asnew observations become available. This can be reduced by corotating both backand forward in time, but this still introduces large errors in the magnitudeand timing of solar wind streams. We show how the dynamic time warping (DTW)algorithm can provide around an order-of-magnitude improvement in solar-windinputs to outer-heliosphere model from in-situ observations near 1 AU. This isintended to build the foundation for further work demonstrating and validatingmethods to improve inner-boundary conditions to outer-heliosphere solar-windmodels, including dealing with solar wind transients and quantifying theimprovements at Saturn and Jupiter.

monthly notices of the royal astronomical society

Using in-situ solar-wind observations to generate inner-boundary  conditions to outer-heliosphere simulations, 1: Dynamic time warping applied  to synthetic observations