Skip to Main Content

Access Provided by Xinjiang University

Physical Review D

Access by Xinjiang University

Heavy wino-like neutralino dark matter annihilation into antiparticles

Junji Hisano¹, Shigeki Matsumoto², Osamu Saito¹, and Masato Senami¹

¹ICRR, University of Tokyo, Kashiwa 277-8582, Japan
²Theory Group, KEK, Oho 1-1 Tsukuba, Ibaraki 305-0801, Japan

Phys. Rev. D 73, 055004 – Published 13 March, 2006

DOI: https://doi.org/10.1103/PhysRevD.73.055004

Abstract

The lightest neutralino is a viable dark matter (DM) candidate. In this paper we study indirect detection of the wino-like neutralino DM using positrons and antiprotons from the annihilation in the galactic halo. When the mass is around 2 TeV, which is favored from the thermal relic abundance, the nonperturbation effect significantly enhances the annihilation cross sections into positrons and antiprotons. We find that the positron and antiproton fluxes with energies larger than 100 GeV may become larger than the expected backgrounds. Since the positron flux is less sensitive to the astrophysical parameters, the detection may be promising in the upcoming experiments such as PAMELA and AMS-02. We also find the wino-like neutralino DM with mass around 2 TeV is compatible with the HEAT anomaly.

Article Text

References (44)

D. N. Spergel et al. (WMAP Collaboration), Astrophys. J. Suppl. Ser. 148, 175 (2003).
C. L. Bennett et al., Astrophys. J. Suppl. Ser. 148, 1 (2003).
G. Jungman, M. Kamionkowski, and K. Griest, Phys. Rep. 267, 195 (1996); L. Bergstrom, Rep. Prog. Phys. 63, 793 (2000); G. Bertone, D. Hooper, and J. Silk, Phys. Rep. 405, 279 (2005); C. Munoz, Int. J. Mod. Phys. A 19, 3093 (2004).
H. P. Nilles, Phys. Rep. 110, 1 (1984); H. E. Haber and G. L. Kane, 117, 75 (1985).
L. Randall and R. Sundrum, Nucl. Phys. B557, 79 (1999); G. F. Giudice, M. A. Luty, H. Murayama, and R. Rattazzi, J. High Energy Phys. 12 (1998) 027.
M. W. Goodman and E. Witten, Phys. Rev. D 31, 3059 (1985).
J. Hisano, S. Matsumoto, and M. M. Nojiri, Phys. Rev. Lett. 92, 031303 (2004).
J. Hisano, S. Matsumoto, M. M. Nojiri, and O. Saito, Phys. Rev. D 71, 063528 (2005).
S. Profumo and C. E. Yaguna, Phys. Rev. D 70, 095004 (2004).
M. Boezio et al., Nucl. Phys. B, Proc. Suppl. 134, 39 (2004).
F. Barao (AMS-02 Collaboration), Nucl. Instrum. Methods Phys. Res., Sect. A 535, 134 (2004).
S. W. Barwick et al. (HEAT Collaboration), Astrophys. J. 482, L191 (1997).
J. Hisano, S. Matsumoto, and M. M. Nojiri, Phys. Rev. D 67, 075014 (2003).
T. Moroi and L. Randall, Nucl. Phys. B570, 455 (2000).
K. Kohri, M. Yamaguchi, and J. Yokoyama, Phys. Rev. D 72, 083510 (2005).
K. Yamamoto, Phys. Lett. B 161, 289 (1985); 168, 341 (1986); D. H. Lyth and E. D. Stewart, Phys. Rev. D 53, 1784 (1996).
G. Corcella et al., J. High Energy Phys. 01 (2001) 010.
S. Rudaz and F. W. Stecker, Astrophys. J. 325, 16 (1988); M. Kamionkowski and M. S. Turner, Phys. Rev. D 43, 1774 (1991).
E. A. Baltz and J. Edsjo, Phys. Rev. D 59, 023511 (1999).
W. R. Webber, M. A. Lee, and M. Gupta, Astrophys. J. 390, 96 (1992).
M. S. Longair, High-energy Astrophysics (Cambridge University Press, Cambridge, England, 1994), Vol. 2.
A. Barrau, G. Boudoul, F. Donato, D. Maurin, P. Salati, and R. Taillet, Astron. Astrophys.. 388, 676 (2002).
I. V. Moskalenko and A. W. Strong, Astrophys. J. 493, 694 (1998).
J. J. Beatty et al., Phys. Rev. Lett. 93, 241102 (2004).
The boost factor is discussed, for example, in Ref. [19] and the clumpy halo is discussed, for example, in Ref. [44].
D. Hooper and J. Silk, Phys. Rev. D 71, 083503 (2005).
L. Bergstrom, J. Edsjo, and P. Ullio, Astrophys. J. 526, 215 (1999).
T. Sjostrand, Comput. Phys. Commun. 82, 74 (1994).
D. Maurin, R. Taillet, F. Donato, P. Salati, A. Barrau, and G. Boudoul, astro-ph/0212111.
D. Maurin, R. Taillet, and F. Donato, Astron. Astrophys. 394, 1039 (2002).
F. Donato, N. Fornengo, D. Maurin, P. Salati, and R. Taillet, Phys. Rev. D 69, 063501 (2004).
M. Garcia-Munoz, J. A. Simpson, T. G. Guzik, J. P. Wefel, and S. H. Margolis, Astrophys. J. Suppl. Ser. 64, 269 (1987).
F. Donato, D. Maurin, P. Salati, A. Barrau, G. Boudoul, and R. Taillet, Astrophys. J. 563, 172 (2001).
L. C. Tan and L. K. Ng, J. Phys. G 9, 227 (1983).
R. J. Protheroe, Astrophys. J. 251, 387 (1981).
A. Bottino, F. Donato, N. Fornengo, and P. Salati, Phys. Rev. D 58, 123503 (1998); 72, 083518 (2005).
T. Sanuki et al., Astrophys. J. 545, 1135 (2000).
J. Alcaraz et al. (AMS Collaboration), Phys. Lett. B 472, 215 (2000).
R. P. Duperray, C. Y. Huang, K. V. Protasov, and M. Buenerd, Phys. Rev. D 68, 094017 (2003).
S. Orito et al. (BESS Collaboration), Phys. Rev. Lett. 84, 1078 (2000); T. Maeno et al. (BESS Collaboration), Astropart. Phys. 16, 121 (2001).
M. Aguilar et al. (AMS Collaboration), Phys. Rep. 366, 331 (2002); 380, 97(E) (2003).
M. Boezio et al. (WiZard/CAPRICE Collaboration), Astrophys. J. 561, 787 (2001).
J. Hisano, S. Matsumoto, M. M. Nojiri, and O. Saito, Phys. Rev. D 71, 015007 (2005).
J. Silk and A. Stebbins, Astrophys. J. 411, 439 (1993); L. Bergstrom, J. Edsjo, P. Gondolo, and P. Ullio, Phys. Rev. D 59, 043506 (1999); V. Berezinsky, V. Dokuchaev, and Y. Eroshenko, 68, 103003 (2003).