Colliding-Wind Binaries with Orbital Motion: Line Wind Formulation

Brendan Michael O'Connor


We apply the line wind approximation to thin shell bow shock and wind collision problems. Stellar wind collisions are observed in many binary star systems, where the orbital motion leads to the development of a spiral pattern. We discuss initial results for the shape of the shock structure in the co-rotating frame, which requires the inclusion of Coriolis and centrifugal effects. We only consider the problem for systems where the two winds are identical and the wind speeds greatly exceeds the orbital speed. Numerical integration of differential equations gives the shell shape.


shock waves, stars: mass loss, Hydrodynamics

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