1994/05/29 by Vladimir V. Usov, Usov, Vladimir V.
Engineering · Physics and Astronomy · #Astrophysics (astro-ph) #Cyclone Separators and Fluid Dynamics #FOS: Physical sciences #Fluid Dynamics and Vibration Analysis #Particle Dynamics in Fluid Flows #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9405067
10 pages of TEX, Invited talk at the IAU Symposium No. 163 "Wolf-Rayet Stars: Binaries, Colliding Winds, Evolution", Elba, Italy, 2-6 May 1994
arxiv created 1994/05/29 · openalex publication_date 1994/05/29 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
One of the main properties of Wolf-Rayet (WR) stars is a very intense outflow of gas. No less than 40% of WR stars belong to binary systems. Young massive O and B stars are the secondary components of such systems. OB stars also have an intense stellar wind. If the intensities of the stellar winds of WR and OB stars are more or less comparable or if the distance between the components of the binary is large enough, the winds flowing out of WR and OB stars can collide and the shock waves are formed. In the shock the gas is heated to temperature ∼ 107 K and generates X-ray emission. Stellar wind collision may be responsible not only for the X-ray emission of WR + OB binaries and for their radio, IR and γ-ray emision as well. Stellar wind collision, gas heating, particle acceleration, and generation of X-ray, γ-ray, radio and IR emission in WR + OB binaries are discussed.