We investigate if the gamma ray halo, for which recent evidence has been found in EGRET data, can be explained by neutralino annihilations in a clumpy halo. We find that the measured excess gamma ray flux can be explained through a moderate amount of clumping in the halo. The required amount of clumping implies also a measurable excess of antiprotons at low energies, which may be suggested by recent measurements by the BESS Collaboration. The predicted antiproton fluxes resulting from neutralino annihilations in a clumpy halo are high enough to give an excess over cosmic-ray produced antiprotons also at moderately high energies (above a few GeV). This prediction, as well as that of one or two sharp gamma lines coming from annihilations into gamma gamma or Z gamma, can be tested in upcoming space-home experiments such as AMS and GLAST.

Possible indications of a clumpy dark matter halo / Bergström, L.; Edsjö, J.; Ullio, P.. - In: PHYSICAL REVIEW D. - ISSN 0556-2821. - 58:8(1998), pp. 083507.1-083507.5. [10.1103/PhysRevD.58.083507]

Possible indications of a clumpy dark matter halo

Ullio, P.
1998-01-01

Abstract

We investigate if the gamma ray halo, for which recent evidence has been found in EGRET data, can be explained by neutralino annihilations in a clumpy halo. We find that the measured excess gamma ray flux can be explained through a moderate amount of clumping in the halo. The required amount of clumping implies also a measurable excess of antiprotons at low energies, which may be suggested by recent measurements by the BESS Collaboration. The predicted antiproton fluxes resulting from neutralino annihilations in a clumpy halo are high enough to give an excess over cosmic-ray produced antiprotons also at moderately high energies (above a few GeV). This prediction, as well as that of one or two sharp gamma lines coming from annihilations into gamma gamma or Z gamma, can be tested in upcoming space-home experiments such as AMS and GLAST.
1998
58
8
1
5
083507
https://doi.org/10.1103/PhysRevD.58.083507
https://arxiv.org/abs/astro-ph/9804050
Bergström, L.; Edsjö, J.; Ullio, P.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/20.500.11767/13377
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