Very high energy gamma-ray production inside the massive binary system Cyg X-1/HDE 226868

Free access article

Issue		A&A Volume 464, Number 2, March III 2007


Page(s)		437 - 445
Section		Astrophysical processes
DOI		http://dx.doi.org/10.1051/0004-6361:20065945

A&A 464, 437-445 (2007)
DOI: 10.1051/0004-6361:20065945

Very high energy gamma-ray production inside the massive binary system Cyg X-1/HDE 226868

W. Bednarek¹ and F. Giovannelli²

¹ Department of Experimental Physics, University of Lódz, 90-236 Lódz, ul. Pomorska 149/153, Poland
e-mail: bednar@fizwe4.fic.uni.lodz.pl
² INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica, Sezione di Roma, Area di Ricerca CNR di Roma-2, via Fosso del Cavaliere 100, 00133 Roma, Italy
e-mail: franco.giovannelli@iasf-roma.inaf.it

(Received 30 June 2006 / Accepted 6 December 2006)

Abstract
TeV $\gamma$ -ray emission has recently been discovered by Cherenkov telescopes from two microquasars, LS 5039 and LS I +61 $^{\rm o}$ 303. This emission is likely to be produced inside the binary system since in both cases variability with the orbital period of the binary has been discovered. In fact, such emission features have recently been predicted by the inverse Compton (IC) e $^\pm$ pair cascade model. In this model, electrons accelerated in the jet develop a cascade in the anisotropic radiation of the massive star. The $\gamma$ -ray spectra emerging from the cascade strongly depends on the location of the observer with respect to the orbital plane of the binary. Here we apply this model to investigate the possible $\gamma$ -ray emission features from another compact massive binary of the microquasar type, Cyg X-1. We conclude that the observational constraints at lower energies (from MeV to GeV) suggest that the spectrum of electrons injected in the jet is likely steeper than in other TeV $\gamma$ -ray microquasars. The cascade $\gamma$ -ray spectrum produced by electrons with such a spectrum in Cyg X-1 should be below the sensitivities of the MAGIC and VERITAS class Cherenkov telescopes. However, if the electron spectrum is flatter, then the highest TeV $\gamma$ -ray fluxes are predicted at ~7 h before and after the phase when the compact object is in front of the massive star. We suggest that Cherenkov telescopes should concentrate on these ranges of phases since the TeV flux can vary by a factor of ~20 with the period of the Cyg X-1 binary system. Moreover, the model predicts clear anticorrelation of the GeV and TeV $\gamma$ -ray emission. This feature can be tested by the future multiwavelength observations with the AGILE and GLAST telescopes in the GeV energy range and the MAGIC and VERITAS telescopes in the TeV energy range.

Key words: gamma-rays: theory -- radiation mechanisms: non-thermal -- stars: binaries: close -- stars: individual: Cyg X-1

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