Fe xxv line profiles in colliding wind binaries
arXiv:1508.04965 · doi:10.1016/j.newast.2015.08.002
Abstract
Strong wind-wind collisions in massive binaries generate a very hot plasma that frequently produces a moderately strong iron line. The morphology of this line depends upon the properties of the wind interaction zone and its orientation with respect to the line of sight. As the binary components revolve around their common centre of mass, the line profiles are thus expected to vary. With the advent of the next generation of X-ray observatories (Astro-H, Athena) that will offer high-resolution spectroscopy above 6 keV, it will become possible to exploit these changes as the most sensitive probe of the inner parts of the colliding wind interaction. Using a simple prescription of the wind-wind interaction in an early-type binary, we have generated synthetic line profiles for a number of configurations and orbital phases. These profiles can help constrain the properties of the stellar winds in such binary systems.
Accepted for publication in New Astronomy
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- Modeling the Optical to Ultraviolet Polarimetric Variability from Thomson Scattering in Colliding Wind Binaries
- The long-period massive binary HD~54662 revisited
- X-ray emission of massive stars and their winds
- UV Spectropolarimetry with Polstar: Massive Star Binary Colliding Winds
- LIFELINE: The program for the simulation of the X-ray line profiles in massive colliding wind binaries