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The non-thermal emission from the colliding-wind binary Apep

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The recently discovered massive binary system Apep is the most powerful synchrotron emitter among the known Galactic colliding-wind binaries. This makes this particular system of great interest to investigate stellar winds and the non-thermal processes associated with their shocks. This source was detected at various radio bands, and in addition the wind-collision region was resolved by means of very-long baseline interferometric observations. We use a non-thermal emission model for colliding-wind binaries to derive physical properties of this system. The observed morphology in the resolved maps allows us to estimate the system projection angle on the sky to be ψ≈85∘. The observed radio flux densities also allow us to characterise both the intrinsic synchrotron spectrum of the source and its modifications due to free--free absorption in the stellar winds at low frequencies; from this we derive mass-loss rates of the stars of M˙WN≈4×10−5 M⊙ yr−1 and M˙WC≈2.9×10−5 M⊙ yr−1. Finally, the broadband spectral energy distribution is calculated for different combinations of the remaining free parameters, namely the intensity of the magnetic field and the injected power in non-thermal particles. We show that the degeneracy of these two parameters can be solved with observations in the high-energy domain, most likely in the hard X-rays but also possibly in γ-rays under favourable conditions.

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Versió postprint del document publicat a:

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Publications of the Astronomical Society of Australia, 2022, vol. 39, p. 4

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(c) Astronomical Society of Australia, 2022

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Articles publicats en revistes (Física Quàntica i Astrofísica)

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The non-thermal emission from the colliding-wind binary Apep