EDP Sciences
Free Access
Volume 396, Number 1, December II 2002
Page(s) 157 - 169
Section Formation, structure and evolution of stars
DOI https://doi.org/10.1051/0004-6361:20021376
Published online 22 November 2002

A&A 396, 157-169 (2002)
DOI: 10.1051/0004-6361:20021376

Detectability and characteristics of the 2.223 MeV line emission from nearby X-ray binaries

N. Guessoum1 and P. Jean2

1  American University of Sharjah, College of Arts & Sciences, Physics Department, Sharjah, UAE
2  Centre d'Etude Spatiale des Rayonnements, CNRS/UPS, 9 avenue du colonel Roche, 31028 Toulouse, France
    e-mail: jean@cesr.fr

(Received 31 July 2002 / Accepted 16 September 2002 )

We present an application and an improvement of the model of Jean & Guessoum (2001) for the production of the 2.223 MeV line resulting from the capture of neutrons in the atmosphere of the secondary in an X-ray binary system. In this model, the neutrons are produced in the accretion disk around the compact primary star and radiated in all directions. The present treatment has fine-tuned and improved upon the previous model in several ways: (1) we have added CNONe nuclei in both the atmosphere of the secondary and the accretion disk around the compact object, making the production and interaction of the neutrons more realistic and accurate; (2) we have improved the physical modeling of the atmosphere of the secondary; and (3) we have considered the comptonization of the 2.223 MeV photons emitted and thus produced the spectrum of the emission both for the line and for the "continuum" below, down to some 100 keV of energy. We have performed a detailed investigation of the variation of the 2.223 MeV emissivity with respect to: the X-ray binary parameters (masses of the compact and secondary stars, separation, etc.), the rate and the model of accretion, and the metallicity of the accreted and atmospheric material. The mean fluxes, phasograms, and the spectra of the 2.223 MeV line have been calculated for several nearby X-ray binary sources, namely: A0620-00, XTE J1118+480, Cen X-4, GS 2000+25 and GRO J0422+32; and we have compared the results with present and future $\gamma$-ray spectrometer sensitivities (INTEGRAL's spectrometer SPI and the Compton Telescope).

Key words: X-rays: binaries -- accretion, accretion disks -- gamma-ray: theory -- lines: profiles -- nuclear reactions, nucleosynthesis, abundances

Offprint request: N. Guessoum, nguessoum@aus.ac.ae

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