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19 April 2024
 
  » arxiv » astro-ph/0411656

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GRBs and the 511 keV emission of the Galactic bulge
E. Parizot ; M. Cassé ; R. Lehoucq ; J. Paul (1- IPN Orsay ; 2- DAPNIA/SAp ; 3- IAP ; 4- APC ;
Date 24 Nov 2004
Subject astro-ph
Affiliation2,3), R. Lehoucq and J. Paul (2,4) (1- IPN Orsay (CNRS/Univ. Paris-Sud); 2- DAPNIA/SAp (CEA-Saclay); 3- IAP (CNRS); 4- APC (CNRS/Univ. Paris 7)
AbstractWe consider the phenomenology of the 511 keV emission in the Galactic bulge, as recently observed by INTEGRAL, and propose a model is 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 about 10^7 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 about 8 10^4 yr x E_GRB_51. We also explain the low disk-to-bulge emission ratio by noting that positrons from GRBs in the Galactic disk should annihilate on timescales of < 10^4 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 10^4 E_51 yr, INTEGRAL should be able to detect the (localized) 511 keV emission associated with one or a few GRB explosions in the disk.
Source arXiv, astro-ph/0411656
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