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2005

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Si us plau utilitzeu sempre aquest identificador per citar o enllaçar aquest document: https://hdl.handle.net/2445/45337

High mass microquasars and low latitude gamma-ray sources

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Recurs relacionat

http://dx.doi.org/10.1051/0004-6361:20041194

Resum

Population studies of unidentified EGRET sources suggest that there exist at least three different populations of galactic gamma-ray sources. One of these populations is formed by young objects distributed along the galactic plane with a strong concentration toward the inner spiral arms of the Galaxy. Variability, spectral and correlation analysis indicate that this population is not homogeneous. In particular, there is a subgroup of sources that display clear variability in their gamma-ray fluxes on timescales from days to months. Following the proposal by Kaufman Bernad\'o et al. (2002), we suggest that this group of sources might be high-mass microquasars, i.e. accreting black holes or neutron stars with relativistic jets and early-type stellar companions. We present detailed inhomogeneous models for the gamma-ray emission of these systems that include both external and synchrotron self-Compton interactions. We have included effects of interactions between the jet and all external photon fields to which it is exposed: companion star, accretion disk, and hot corona. We make broadband calculations to predict the spectral energy distribution of these objects from radio up to GeV energies. The results and predictions can be tested by present and future gamma-ray instruments like INTEGRAL, AGILE, and GLAST.

Matèries

Estels binaris de raigs X, Estels, Vents, Raigs gamma, Astrofísica

Matèries (anglès)

X-ray binaries, Stars, Winds, Gamma rays, Astrophysics

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Articles publicats en revistes (Física Quàntica i Astrofísica)

Citació

BOSCH I RAMON, Valentí, ROMERO, Gustavo e., PAREDES I POY, Josep maria. High mass microquasars and low latitude gamma-ray sources. _Astronomy and Astrophysics_. 2005. Vol. 429, núm. 1, pàgs. 267-276. [consulta: 24 de gener de 2026]. ISSN: 0004-6361. [Disponible a: https://hdl.handle.net/2445/45337]

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