2010
DOI: 10.1111/j.1365-2966.2010.15776.x
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3D models of radiatively driven colliding winds in massive O + O star binaries - III. Thermal X-ray emission

Abstract: The X-ray emission from the wind-wind collision in short-period massive O + O star binaries is investigated. The emission is calculated from 3D hydrodynamical models which incorporate gravity, the driving of the winds, orbital motion of the stars and radiative cooling of the shocked plasma. Changes in the amount of stellar occultation and circumstellar attenuation introduce phase-dependent X-ray variability in systems with circular orbits, while strong variations in the intrinsic emission also occur in systems… Show more

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Cited by 96 publications
(95 citation statements)
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References 81 publications
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“…Considering that massive binaries are known to be bright thermal X-ray emitters (see e.g. Stevens et al 1992;Pittard & Parkin 2010), the X-ray spectrum is expected to be dominated by thermal emission in the complete soft band (i.e. below 10 keV), which agrees with observational results obtained over the past decades.…”
Section: High-energy Investigationssupporting
confidence: 81%
See 1 more Smart Citation
“…Considering that massive binaries are known to be bright thermal X-ray emitters (see e.g. Stevens et al 1992;Pittard & Parkin 2010), the X-ray spectrum is expected to be dominated by thermal emission in the complete soft band (i.e. below 10 keV), which agrees with observational results obtained over the past decades.…”
Section: High-energy Investigationssupporting
confidence: 81%
“…below 10 keV), which agrees with observational results obtained over the past decades. In that energy band, the X-ray emission is indeed dominated by emission lines on top of a free-free continuum, as produced by an optically thin plasma that is characterized by temperatures that do not go beyond several 10 MK (for CWB with periods of at least a few weeks, where stars are able to accelerate their winds up to their terminal velocitites, see Stevens et al 1992;Pittard & Stevens 1997;Pittard & Parkin 2010). As a result, one could only expect non-thermal high energy emission to be revealed in the hard X-ray domain (above 10 keV) or even in γ-rays, where thermal X-rays are not present.…”
Section: High-energy Investigationsmentioning
confidence: 99%
“…Based on hydrodynamical simulations, Pittard & Parkin (2010) indeed predicted the existence of deviations from this behaviour. However, their simulations refer to binary systems with much shorter orbital periods than 9 Sgr.…”
Section: Discussionmentioning
confidence: 99%
“…If the system hosts a wind interaction that produces X-ray emission, we expect to observe changes in the X-ray spectra between the various phases. These changes can result from a varying line-of-sight column density or from the changing separation between the stars or from a combination of both effects (Stevens et al 1992;Pittard & Parkin 2010). Figure 4 illustrates the EPIC-pn spectra of 9 Sgr at the four epochs that were monitored.…”
Section: X-ray Spectroscopymentioning
confidence: 99%
“…Stevens et al 1992;Folini & Walder 2000;Pittard & Parkin 2010;, or dealt with only part of the stellar evolution (Stegeman 2003). Velázquez et al (2003) simulated the collision between a supernova and an expanding wind bubble, but with a simplified model that assumed the supernova progenitor had not previously created a circumstellar bubble through its own wind.…”
Section: Introductionmentioning
confidence: 99%