Built on

See, for example, P.-f. Yin, Q. Yuan, J. Liu, J. Zhang, X.-j. Bi, S.-h. Zhu and X. Zhang, arXiv:0811.0176 [hep-ph]; C.-R. Chen, M. M. Nojiri, F. Takahashi and T. T. Yanagida, arXiv:0811.3357 [astro-ph]; E. Nardi, F. Sannino and A. Strumia, arXiv:0811.4153 [hep-ph]; K. Ishiwata, S. Matsumoto and T. Moroi, arXiv:0811.4492 [astro-ph]; arXiv:0811.0250 [hep-ph]; A. Arvanitaki, S. Dimopoulos, S. Dubovsky, P. W. Graham, R. Harnik and S. Rajendran, arXiv:0812.2075 [hep-ph]; K. Hamaguchi, S. Shirai and T. T. Yanagida, arXiv:0812.2374 [hep-ph]; F. Takahashi and E. Komatsu, arXiv:0901.1915 [astro-ph]
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J. N. Bahcall and R. M. Soneira, Astrophys. J. Suppl. 44
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J. Hisano, S. Matsumoto, O. Saito and M. Senami, Phys. Rev. D 73

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2009

Dark Matter Signals from Cascade Annihilations

Mardon, Jeremy, Nomura, Yasunori, Stolarski, Daniel et al.

Understand

A leading interpretation of the electron/positron excesses seen by PAMELA and ATIC is dark matter annihilation in the galactic halo.

Depending on the annihilation channel, the electron/positron signal could be accompanied by a galactic gamma ray or neutrino flux, and the non-detection of such fluxes constrains the couplings and halo properties of dark matter.
In this paper, we study the interplay of electron data with gamma ray and neutrino constraints in the context of cascade annihilation models, where dark matter annihilates into light degrees of freedom which in turn decay into leptons in one or more steps.
Electron and muon cascades give a reasonable fit to the PAMELA and ATIC data.

Built on

See, for example, P.-f. Yin, Q. Yuan, J. Liu, J. Zhang, X.-j. Bi, S.-h. Zhu and X. Zhang, arXiv:0811.0176 [hep-ph]; C.-R. Chen, M. M. Nojiri, F. Takahashi and T. T. Yanagida, arXiv:0811.3357 [astro-ph]; E. Nardi, F. Sannino and A. Strumia, arXiv:0811.4153 [hep-ph]; K. Ishiwata, S. Matsumoto and T. Moroi, arXiv:0811.4492 [astro-ph]; arXiv:0811.0250 [hep-ph]; A. Arvanitaki, S. Dimopoulos, S. Dubovsky, P. W. Graham, R. Harnik and S. Rajendran, arXiv:0812.2075 [hep-ph]; K. Hamaguchi, S. Shirai and T. T. Yanagida, arXiv:0812.2374 [hep-ph]; F. Takahashi and E. Komatsu, arXiv:0901.1915 [astro-ph]
Original
1915
Earlier work this paper cites.
R. D. Davies, D. Walsh and R. S. Booth, Mon. Not. Roy. Astron. Soc. 177
1976
Earlier work this paper cites.
J. N. Bahcall and R. M. Soneira, Astrophys. J. Suppl. 44
1980
Earlier work this paper cites.
Y. B. Zel’dovich, A. A. Klypin, M. Y. Khlopov and V. M. Chechetkin, Sov. J. Nucl. Phys. 31
1980
Earlier work this paper cites.
S. Ritz and D. Seckel, Nucl. Phys. B 304
1988
Earlier work this paper cites.
G. G. Raffelt, Phys. Rept. 198
Original
1990
Earlier work this paper cites.
J. F. Navarro, C. S. Frenk and S. D. M. White, Astrophys. J. 490
1997
Earlier work this paper cites.
I. V. Moskalenko and A. W. Strong, Astrophys. J. 493
1999
Earlier work this paper cites.
H. L. Lai et al
2000
Earlier work this paper cites.
Y. Kuno and Y. Okada, Rev. Mod. Phys. 73
2001
Earlier work this paper cites.
D. Merritt, M. Milosavljević, L. Verde and R. Jimenez, Phys. Rev. Lett. 88
2002
Earlier work this paper cites.
S. Fukuda et al
2003
Earlier work this paper cites.

Similar

S. Desai et al
2004
Cited alongside, same era.
T. G. Guzik et al
2004
Cited alongside, same era.
J. F. Navarro et al
2004
Cited alongside, same era.
N. W. Evans, F. Ferrer and S. Sarkar, Phys. Rev. D 69
2004
Cited alongside, same era.
J. Ahrens et al
2004
Cited alongside, same era.
F. Aharonian et al
2006
Cited alongside, same era.
F. Aharonian et al
2006
Cited alongside, same era.
J. Hisano, S. Matsumoto, O. Saito and M. Senami, Phys. Rev. D 73