Using gamma-rays to probe the clumped structure of stellar winds

Conference item

Gamma-rays can be produced by the interaction of a relativistic jet and the matter of the stellar wind in the subclass of massive X-ray binaries known as "microquasars". The relativistic jet is ejected from the surroundings of the compact object and interacts with cold protons from the stellar wind, producing pions that then quickly decay into gamma-rays. Since the resulting gamma-ray emissivity depends on the target density, the detection of rapid variability in microquasars with GLAST and the new generation of Cherenkov imaging arrays could be used to probe the clumped structure of the stellar wind. In particular, we show here that the relative fluctuation in gamma rays may scale with the square root of the ratio of porosity length to binary separation, \sqrt{h/a}, implying for example a ca. 10 % variation in gamma ray emission for a quite moderate porosity, h/a ~ 0.01.

Authors: Romero, G; Owocki, S; Araudo, A; Townsend, R; Benaglia, P

• Publication status: Published
• Peer review status: Peer reviewed
• Publisher: Universitätsverlag Potsdam
• Host title: Clumping in Hot-Star Winds Proceedings of an International Workshop held in Potsdam, Germany, 18. - 22. June 2007
• Journal: Clumping in Hot-Star Winds Proceedings of an International Workshop held in Potsdam, Germany, 18. - 22. June 2007
• Pages: 191-194
• Publication date: 2008-04-01
• ISBN: 9783940793331
• Keywords: astro-ph; SBTMR