Instabilities in colliding winds

Theoretical considerations on colliding clumped winds

First attempts are made to derive astrophysical implications of the collision of clumped stellar winds from order of magnitude estimates and preliminary numerical simulations. Compared to colliding smooth winds, we find that the most significant differences occur in widely separated systems like WR 140. Clumped winds de-stabilize the wind-wind interaction zone of such systems. Highly compressed...

Radio Emission Models of Colliding - Winds Binariess

Radio observations of colliding winds in massive stars

This brief review describes radio observations of colliding winds in massive stars starting with the first direct observational support for the colliding-wind model advanced in the early 1990’s to explain non-thermal radio and thermal X-ray emission in some massive stars. Studies of the well-studied and highly-eccentric WR+O star systemWR140 are described along with recent observations of O-sta...

3-D SPH simulations of colliding winds in η Carinae

We study colliding winds in the superluminous binary η Carinae by performing threedimensional, Smoothed Particle Hydrodynamics (SPH) simulations. For simplicity, we assume both winds to be isothermal. We also assume that wind particles coast without any net external forces. We find that the lower density, faster wind from the secondary carves out a spiral cavity in the higher density, slower wi...

Particle Acceleration in the Colliding Winds Binary Wr 140

RESUMEN Favor de proporcionar un resumen en español. If you cannot provide a spanish abstract, the editors will do this. Massive WR+O star systems produce high-temperature, shock-heated plasma where the wind of the WR star and that of its binary companion collide-the wind-collision region (WCR). The WCR is a source of thermal (e.g. hard X-rays) and non-thermal (e.g. synchrotron) emission, the l...