Volume 432, Number 3, March IV 2005
|Page(s)||889 - 894|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||07 March 2005|
GRBs and the 511 keV emission of the Galactic bulge
Institut de Physique Nucléaire d'Orsay, IN2P3-CNRS/Université Paris-Sud, 91406 Orsay Cedex, France e-mail: firstname.lastname@example.org
2 DAPNIA/Service d'astrophysique, CEA-Saclay, 91191 Gif-sur-Yvette, France
3 Institut d'Astrophysique de Paris, 98bis Bd Arago, 75014 Paris, France
4 Fédération de Recherche, Astroparticule et Cosmologie, Univ. Paris 7, Collège de France, 75231 Paris Cedex 05, France
Accepted: 23 November 2004
We consider the phenomenology of the 511 keV emission in the Galactic bulge, as recently observed by INTEGRAL, and propose a model in which the positrons are produced by gamma-ray bursts (GRB) associated with mini-starbursts in the central molecular zone (CMZ). We show that the positrons can easily diffuse across the bulge on timescales of ∼107 yr, and that their injection rate by GRBs is compatible with the observed fluxes if the mean time between two GRBs in the bulge is ∼ yr . We also explain the low disk-to-bulge emission ratio by noting that positrons from GRBs in the Galactic disk should be annihilated on timescales of 104 yr in the dense shell of the underlying supernova remnant, after the radiative transition, while the remnants of GRBs occurring in the hot, low-density medium produced by recurrent starbursts in the CMZ become subsonic before they can form a radiative shell, allowing the positrons to escape and fill the whole Galactic bulge. If the mean time between GRBs is smaller than ~ yr, INTEGRAL should be able to detect the (localized) 511 keV emission associated with one or a few GRB explosions in the disk.
Key words: gamma rays: bursts / Galaxy: bulge
© ESO, 2005
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