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Radio Jets and UHE Gamma-ray Emission in Cyg X-3

Published online by Cambridge University Press:  25 April 2016

R.K. Manchanda ,
L.E. Waldron  and
R.K. Sood
R.K. Manchanda
Affiliation:
Tata Institute of Fundamental Research, Bombay 400–005, India
L.E. Waldron
Affiliation:
Dept of Physics, University College, University of New South Wales, ADFA, Canberra ACT 2600
R.K. Sood
Affiliation:
Dept of Physics, University College, University of New South Wales, ADFA, Canberra ACT 2600
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Abstract

The low-mass X-ray binary source Cyg X–3 has been extensively observed from radio to ultra-high-energy (UHE) gamma-ray energies (i.e., energies >1015eV). In the radio, Cyg X–3 exhibits intense non-thermal outbursts (flares) and a double-sided relativistic jet morphology. Interestingly, at energies above 1 TeV (1012eV), the gamma-ray emission is highly variable and possibly correlated with the radio outbursts. This emission results primarily from the radiative decay of π°-mesons generated in inelastic collisions between relativistic nuclei (predominantly protons) and the surrounding matter. The observed flux of UHE gamma-rays from Cyg X–3 implies that Cyg X–3 is a localised accelerator of such particles.

We propose a model of Cyg X–3 wherein particles expelled by the source are accelerated by Shockwaves in the relativistically expanding jets. Intense flaring episodes then lead to time variations in the ambient particle flux which account for the observed features at UHE energies.

Type
High Energy Astrophysics
Information
Publications of the Astronomical Society of Australia , Volume 10 , Issue 3 , 1993 , pp. 208 - 210
Copyright
Copyright © Astronomical Society of Australia 1993

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