Collision of Orbiting Stellar Winds

The collision of supersonic stellar winds is a ubiquitous phenomenon observed in many binary star systems. We have applied a semi-analytic approach to determining the shock structure of such systems using a thin shell formalism and the analytic wind solutions of Wilkin & Hausner 2017. We use an arc length parametrization to describe the resulting shell in terms of a system of ordinary differential

equations, which yield the shock shape, mass surface density and momentum flow within it. The equations are singular at the stagnation

point and Taylor series expansion was required to begin the integrations. We present preliminary solutions for equal winds.