Particle acceleration and nonthermal radio emission in binaries of early-type stars

Eichler, David; Усов, В. В.

doi:10.1086/172130

Cited by 351 publications

(492 citation statements)

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“…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. The colliding wind binaries were long known to be sources of non-thermal radio emission Eichler and Usov (1993), Dougherty et al (2005), Pittard and Dougherty (2006), De Becker (2007) and the catalog of colliding wind binaries with non-thermal particle acceleration compiled by De Becker and Raucq (2013) contains 43 objects.…”

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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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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“…For Cyg OB2 #8A, we adopted a radial dependence of the magnetic field (Eichler & Usov, 1993). The collision zone is indeed closer to the stars than in the case considered by Benaglia et al (2001).…”

Section: Cyg Ob2 #8a In the Context Of This Scenariomentioning

confidence: 99%

“…The acceleration of relativistic electrons responsible for non-thermal emission (radio, X-rays, γ-rays) is believed to occur within the interaction zone of the colliding winds of the binary system (Eichler & Usov, 1993). The IC scattering of UV photons of Cyg OB2 #8A is expected to account for 8-10 % of the γ-ray luminosity of the unidentified EGRET source 3EG J2033+4118.…”

Section: Prospects and Conclusionmentioning

confidence: 99%

On the Multiplicity of the O-Star Cyg OB2 #8a and its Contribution to the γ-ray Source 3EG J2033+4118

Becker

Rauw

Swings

2005

Astrophys Space Sci

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Abstract. We present the results of an intensive spectroscopic campaign in the optical waveband revealing that Cyg OB2 #8A is an O6 + O5.5 binary system with a period of about 21.9 d. Cyg OB2 #8A is a bright X-ray source, as well as a nonthermal radio emitter. We discuss the binarity of this star in the framework of a campaign devoted to the study of non-thermal emitters, from the radio waveband to γ-rays. In this context, we attribute the non-thermal radio emission from this star to a population of relativistic electrons, accelerated by the shock of the windwind collision. These relativistic electrons could also be responsible for a putative γ-ray emission through inverse Compton scattering of photospheric UV photons, thus contributing to the yet unidentified EGRET source 3EG J2033+4118.

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“…With momentum ratio η ∼ 10, the opening angle of the cone-like shock is ∼ 50 − 60 • (c.f. Eichler & Usov 1993;Canto et al 1996), which corresponds to ∼ 0.15 orbital phase. Because the emission is concentrated in the forward direction of the flow, therefore, we expect that double peaks due to the Doppler effect appear at ∼ 0.15 phase before and after the phase of radio eclipse, which is consistent with the observation.…”

Section: Discussionmentioning

confidence: 99%

X-ray studies of the black widow pulsar PSR B1957+20

Huang¹,

Kong²,

Takata

et al. 2012

Proc. IAU

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We report on Chandra observations of the black widow pulsar, PSR B1957+20. Evidence for a binary-phase dependence of the X-ray emission from the pulsar is found with a deep observation. The binary-phase resolved spectral analysis reveals non-thermal X-ray emission of PSR B1957+20, confirming the results of previous studies. This suggests that the X-rays are mostly due to intra-binary shock emission which is strongest when the pulsar wind interacts with the ablated material from the companion star. The geometry of the peak emission is determined in our study. The marginal softening of the spectrum of the non-thermal X-ray tail may indicate that particles injected at the termination shock is dominated by synchrotron cooling.

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Particle acceleration and nonthermal radio emission in binaries of early-type stars

Cited by 351 publications

References 0 publications

Nonthermal particles and photons in starburst regions and superbubbles

Nonthermal particles and photons in starburst regions and superbubbles

On the Multiplicity of the O-Star Cyg OB2 #8a and its Contribution to the γ-ray Source 3EG J2033+4118

X-ray studies of the black widow pulsar PSR B1957+20

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