Our 1D hydrodynamical model for the slow solar wind used to derive the inner boundary conditions for our binary wind simulation. From top to bottom, the plots show particle number density, velocity, and temperature in the wind against distance from the central star. The dashed line in the velocity plot shows the sound speed as a function of radius. The vertical dotted lines in each plot show the location of 0.1 AU, which is where we take the values for the inner boundary condition in the binary wind simulation.