On the interaction of pulsar winds and clumpy stellar winds
2020 February 25
High-mass binaries hosting a non-accreting pulsar are sources of gamma rays, which are thought to originate in the wind-wind collision region. The stellar wind is expected to be clumpy, which could have important effects on the emitting flow dynamics, and thus on the associated non-thermal radiation. We adopt here a combination of Monte-Carlo and semi-analytical hydrodynamic calculations to explore the impact of clumps on the shocked wind structure on the scales of the binary system.