The non-thermal, time-variable radio emission from Cyg OB2 # 5: A wind-collision region

Abstract

The radio emission from the well-studied massive stellar system Cyg OB2 #5 is known to fluctuate with a period of 6.7 years between a low-flux state when the emission is entirely of free-free origin, and a high-flux state when an additional non-thermal component (of hitherto unknown nature) appears. In this paper, we demonstrate that the radio flux of that non-thermal component is steady on timescales of hours, and that its morphology is arc-like. This shows that the non-thermal emission results from the collision between the strong wind driven by the known contact binary in the system, and that of an unseen companion on a somewhat eccentric orbit with a 6.7-yr period and a 5 to 10 mas semi-major axis. Together with the previously reported wind-collision region located about 0.8 arcsec to the north-east of the contact binary, Cyg OB2 #5 appears to be the only multiple system known so far to harbor two radio-imaged wind-collision regions.

Accepted for publication in The Astrophysical Journal

References in corpus (6)

• PAMELA Measurements of Cosmic-ray Proton and Helium Spectra
• Radio, X-ray, and gamma-ray Emission Models of the Colliding Winds Binary WR 140
• Non-thermal emission processes in massive binaries
• Monitoring the Large Proper Motions of Radio Sources in the Orion BN/KL Region
• A multiwavelength investigation of the massive eclipsing binary Cyg OB2 #5
• A 1.3 cm wavelength radio flare from a deeply embedded source in the Orion BN/KL region

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