Gamma-ray absorption and the origin of the gamma-ray flare in Cygnus X-1

TL;DR

This paper models gamma-ray absorption and emission in Cygnus X-1 to explain a VHE flare, proposing jet-clump interactions as the cause, and successfully reproduces the observed spectrum.

Contribution

It introduces a detailed model of gamma-ray opacity and emission mechanisms in Cygnus X-1, highlighting jet-clump interactions as a novel explanation for the VHE flare.

Findings

Gamma-ray opacity varies along the orbit, affecting observed emission.

Jet-clump interactions can produce the observed VHE spectrum.

The model reproduces the flare spectrum with reasonable parameters.

Abstract

The high-mass microquasar Cygnus X-1, the best-established candidate for a stellar-mass black hole in the Galaxy, has been detected in a flaring state at very high energies (VHE), E > 200 GeV, by the Atmospheric Cherenkov Telescope MAGIC. The flare occurred at orbital phase 0.91, where phase 1 is the configuration with the black hole behind the companion high-mass star, when the absorption of gamma-ray photons by photon-photon annihilation with the stellar field is expected to be highest. We aim to set up a model for the high-energy emission and absorption in Cyg X-1 that can explain the nature of the observed gamma-ray flare. We study the gamma-ray opacity due to pair creation along the whole orbit, and for different locations of the emitter. Then we consider a possible mechanism for the production of the VHE emission. We present detailed calculations of the gamma-ray opacity and infer from these calculations the distance from the black hole where the emitting region was located. We suggest that the flare was the result of a jet-clump interaction where the decay products of inelastic proton-proton collisions dominate the VHE outcome. We are able to reproduce the spectrum of Cyg X-1 during the observed flare under reasonable assumptions. The flare may be the first event of jet-cloud interaction ever detected at such high energies.