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GRBs and the 511 keV emission of the Galactic bulge

Abstract : We 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.
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Contributor : Suzanne Robert <>
Submitted on : Monday, March 1, 2021 - 4:13:34 PM
Last modification on : Monday, March 1, 2021 - 4:14:01 PM
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E. Parizot, M. Cassé, R. Lehoucq, J. Paul. GRBs and the 511 keV emission of the Galactic bulge. Astronomy and Astrophysics - A&A, EDP Sciences, 2005, 432, pp.889-894. ⟨10.1051/0004-6361:20042215⟩. ⟨in2p3-00023426⟩



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