Catalogue of particle-accelerating colliding-wind binaries

Becker, M. De; Raucq, Françoise

doi:10.1051/0004-6361/201322074

Cited by 115 publications

(149 citation statements)

References 161 publications

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“…Radio observations indicate that the particle energy distribution of electrons that emit at 3-10 GHz has a power-law index of p ∼ 3.2. The corresponding electron energy distribution seems particularly soft when compared with the observed spectral indices in other NT CWBs (De Becker & Raucq 2013), and considering that the expected index for DSA in a strong shock is p = 2. This type of soft energy distribution of the radio-emitting particles might be related to the wide nature of the orbit, which could imply a stronger toroidal magnetic field component that may soften the particle distribution by quickly dragging the particles away from the shock, at least at low energies.…”

Section: Particle Distributionmentioning

confidence: 71%

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A model for the non-thermal emission of the very massive colliding-wind binary HD 93129A

Palacio

Bosch‐Ramon

Romero

et al. 2016

A&A

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Context. Recently, the colliding-wind region of the binary stellar system HD 93129A was resolved for the first time using Very Large Baseline Interferometry. This system, one of the most massive known binaries in our Galaxy, presents non-thermal emission in the radio band, which can be used to infer the physical conditions in the system, and make predictions for the high-energy band. Aims. We intend to constrain some of the unknown parameters of HD 93129A through modeling the non-thermal emitter. We also aim to analyse the detectability of this source in hard X-rays and γ-rays. Finally, we want to predict how the non-thermal emission will evolve in the future, when the stars approach periastron. Methods. A broadband radiative model for the wind-collision region (WCR) has been developed taking into account the evolution of the accelerated particles streaming along the shocked region, the emission by different radiative processes, and the attenuation of the emission propagating through the local matter and radiation fields. We reproduce the available radio data, and make predictions of the emission in hard X-rays and γ-rays under different assumptions.Results. From the analysis of the radio emission, we find that the binary HD 93129A is more likely to have a low inclination and a high eccentricity, with the more massive star being currently closer to the observer. The minimum energy of the non-thermal electrons seems to be between ∼20-100 MeV, depending on the intensity of the magnetic field in the WCR. The latter can be in the range ∼20-1500 mG. Conclusions. Our model is able to reproduce the observed radio emission, and predicts that the non-thermal radiation from HD 93129A will increase in the near future. With instruments such as NuSTAR, Fermi, and CTA, it will be possible to constrain the relativistic particle content of the source, and other parameters such as the magnetic field strength in the WCR which, in turn, can be used to obtain upper-limits of the magnetic field on the surface of the very massive stars, thereby inferring whether magnetic field amplification is taking place in the particle acceleration region.

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Section: Particle Distributionmentioning

confidence: 71%

“…These systems, therefore, occupy a quite large region in the parameter space. In this work we focus on the subgroup of CWBs capable of accelerating relativistic particles (particle-accelerating colliding-wind binaries or PACWBs; De Becker & Raucq 2013).…”

Section: Introductionmentioning

confidence: 99%

A model for the non-thermal emission of the very massive colliding-wind binary HD 93129A

Palacio

Bosch‐Ramon

Romero

et al. 2016

A&A

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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

114

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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“…As well as by the synchrotron emission, these systems can be revealed by exceptionally large radio fluxes, a spectral index significantly lower than the thermal value, and an orbital modulation of the radio flux. De Becker & Raucq (2013) recently provided the latest catalogue of such systems.…”

Section: Introductionmentioning

confidence: 99%

“…However, it has become increasingly clear over the past few years that PACWB cover a very wide range of parameters (mass loss, wind velocity, orbital period, etc. ), and the fundamental difference between the PACWB and "normal" CWB is unknown (De Becker & Raucq 2013).…”

Section: Introductionmentioning

confidence: 99%

Search for magnetic fields in particle-accelerating colliding-wind binaries

Neiner

Grunhut

Leroy

et al. 2015

A&A

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Context. Some colliding-wind massive binaries, called particle-accelerating colliding-wind binaries (PACWB), exhibit synchrotron radio emission, which is assumed to be generated by a stellar magnetic field. However, no measurement of magnetic fields in these stars has ever been performed. Aims. We aim at quantifying the possible stellar magnetic fields present in PACWB to provide constraints for models. Methods. We gathered 21 high-resolution spectropolarimetric observations of 9 PACWB available in the ESPaDOnS, Narval and HarpsPol archives. We analysed these observations with the least squares deconvolution method. We separated the binary spectral components when possible. Results. No magnetic signature is detected in any of the 9 PACWB stars and all longitudinal field measurements are compatible with 0 G. We derived the upper field strength of a possible field that could have remained hidden in the noise of the data. While the data are not very constraining for some stars, for several stars we could derive an upper limit of the polar field strength of the order of 200 G. Conclusions. We can therefore exclude the presence of strong or moderate stellar magnetic fields in PACWB, typical of the ones present in magnetic massive stars. Weak magnetic fields could however be present in these objects. These observational results provide the first quantitative constraints for future models of PACWB.

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Catalogue of particle-accelerating colliding-wind binaries

Cited by 115 publications

References 161 publications

A model for the non-thermal emission of the very massive colliding-wind binary HD 93129A

A model for the non-thermal emission of the very massive colliding-wind binary HD 93129A

Nonthermal particles and photons in starburst regions and superbubbles

Search for magnetic fields in particle-accelerating colliding-wind binaries

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