Volume 417, Number 3, April III 2004
|Page(s)||1075 - 1081|
|Section||Stellar structure and evolution|
|Published online||26 March 2004|
A numerical model for the γ-ray emission of the microquasar LS 5039
Departament d'Astronomia i Meteorologia, Universitat de Barcelona, Av. Diagonal 647, 08028 Barcelona, Spain e-mail: email@example.com,firstname.lastname@example.org
Corresponding author: V. Bosch-Ramon, email@example.com
Accepted: 6 January 2004
The possible association between the microquasar LS 5039 and the EGRET source 3EG J1824-1514 suggests that microquasars could also be sources of high-energy γ-rays. In this paper, we explore, with a detailed numerical model, if this system can produce the emission detected by EGRET (>100 MeV) through inverse Compton (IC) scattering. Our numerical approach considers a population of relativistic electrons entrained in a cylindrical inhomogeneous jet, interacting with both the radiation and the magnetic fields, taking into account the Thomson and Klein-Nishina regimes of interaction. The computed spectrum reproduces the observed spectral characteristics at very high energy.
Key words: X-rays: binaries / stars: individual: LS 5039 / gamma-rays: observations / gamma-rays: theory
© ESO, 2004
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