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The outer heliosphere is a dynamic region shaped largely by the interactionbetween the solar wind and the interstellar medium. While interplanetarymagnetic field and plasma observations by the Voyager spacecraft havesignificantly improved our understanding of this vast region, modeling theouter heliosphere still remains a challenge. We simulate the three-dimensional,time-dependent solar wind flow from 1 to 80 astronomical units (AU), where thesolar wind is assumed to be supersonic, using a two-fluid model in whichprotons and interstellar neutral hydrogen atoms are treated as separate fluids.We use 1-day averages of the solar wind parameters from the OMNI data set asinner boundary conditions to reproduce time-dependent effects in a simplifiedmanner which involves interpolation in both space and time. Our model generallyagrees with Ulysses data in the inner heliosphere and Voyager data in the outerheliosphere. Ultimately, we present the model solar wind parameters extractedalong the trajectory of New Horizons spacecraft. We compare our results with insitu plasma data taken between 11 and 33 AU and at the closest approach toPluto on July 14, 2015.

Modeling the Solar Wind at the Ulysses, Voyager, and New Horizons Spacecraft