Colliding winds from early-type stars in binary systems

Stevens, I. R.; Blondin, John M.; Pollock, A. M. T.

doi:10.1086/171013

Cited by 578 publications

(879 citation statements)

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“…From the HS wind parameters, one sees that the shocked HS plasma will be adiabatic. This is indicated by the values of either of dimensionless parameters χ (Stevens et al 1992) and Γ f f (Myasnikov & Zhekov 1993)…”

Section: Csw Model Spectramentioning

confidence: 99%

Recent X-ray observations of the symbiotic star AG Peg: do they signify colliding stellar winds?

Zhekov

Tomov

2016

Mon. Not. R. Astron. Soc.

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We present an analysis of recent X-ray observations of the symbiotic star AG Peg. The X-ray emission of AG Peg as observed with Swift in 2015 shows considerable variability on time scale of days as variability on shorter time scales might be present as well. Analysis of the X-ray spectra obtained in 2013 and 2015 confirms that AG Peg is an X-ray source of class β of the X-ray sources amongst the symbiotic stars. The X-ray emission of AG Peg as observed with ROSAT (1993 June) might well originate from colliding stellar winds (CSW) in binary system. On the other hand, the characteristics of the X-ray emission of AG Peg in 2013 and 2015 (Swift ) are hard to accommodate in the framework of the CSW picture. Analysis of the light curves in 2015 shows that the power spectrum of the X-ray variability in AG Peg resembles that of the flicker noise (or flickering) being typical for accretion processes in astronomical objects. This is a sign that CSWs did not play a key role for the X-ray emission from AG Peg in 2013-2015 and a different mechanism (probably accretion) is also getting into play.

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Section: Csw Model Spectramentioning

confidence: 99%

Recent X-ray observations of the symbiotic star AG Peg: do they signify colliding stellar winds?

Zhekov

Tomov

2016

Mon. Not. R. Astron. Soc.

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“…The wind structure, position and shape of the contact discontinuity between the stars, double-shock structures, as well as the post-shock flows were examined by Stevens et al (1992) and later by Parkin and Pittard (2008), who correspondingly used 2D and 3D hydrodynamic codes with an account for radiative cooling and some instabilities. The models were aimed to describe the symbiotic systems and gamma-ray binaries, and also binary systems with O-type and Wolf-Rayet stars including the enigmatic object in η-Carinae.…”

Section: Colliding Wind Binariesmentioning

confidence: 99%

Nonthermal particles and photons in starburst regions and superbubbles

Bykov

2014

Astron Astrophys Rev

113

102

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Starforming factories in galaxies produce compact clusters and loose associations of young massive stars. Fast radiation-driven winds and supernovae input their huge kinetic power into the interstellar medium in the form of highly supersonic and superalfvenic outflows. Apart from gas heating, collisionless relaxation of fast plasma outflows results in fluctuating magnetic fields and energetic particles. The energetic particles comprise a long-lived component which may contain a sizeable fraction of the kinetic energy released by the winds and supernova ejecta and thus modify the magnetohydrodynamic flows in the systems. We present a concise review of observational data and models of nonthermal emission from starburst galaxies, superbubbles, and compact clusters of massive stars. Efficient mechanisms of particle acceleration and amplification of fluctuating magnetic fields with a wide dynamical range in starburst regions are discussed. Sources of cosmic rays, neutrinos and multi-wavelength nonthermal emission associated with starburst regions including potential galactic "PeVatrons" are reviewed in the global galactic ecology context.

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“…However, we can suggest the following scenario already from the present results. Due to thermal instabilities (e.g., Stevens et al 1992), dense large blobs are formed in the post-shock primary's wind region near the stagnation point. These blobs are pulled to the secondary as periastron is approached.…”

Section: Accretion Near Periastron Passagementioning

confidence: 99%

Accretion by the Secondary in η Carinae During the Spectroscopic Event. I. Flow Parameters

Soker

2005

ApJ

120

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We examine the influence of the gravity of the companion (the secondary) to the massive primary star Carinae on the winds blown by the primary and the secondary. The two winds collide with each other after passing through two respective shock waves, and escape the system while strongly emitting in the X-ray band. While during most of the 5.5 yr orbital period the companion's gravity has a negligible effect on the winds, we find that near periastron the companion's gravity may significantly influence the flow, and the companion might accrete from the primary's wind under certain circumstances. Near periastron passage, the collision region of the two winds may collapse onto the secondary star, a process that could substantially reduce the X-ray luminosity. We suggest that such an accretion process produces the long, almost flat, X-ray minimum in Car.

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Colliding winds from early-type stars in binary systems

Cited by 578 publications

References 0 publications

Recent X-ray observations of the symbiotic star AG Peg: do they signify colliding stellar winds?

Recent X-ray observations of the symbiotic star AG Peg: do they signify colliding stellar winds?

Nonthermal particles and photons in starburst regions and superbubbles

Accretion by the Secondary in η Carinae During the Spectroscopic Event. I. Flow Parameters

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