Light relic neutralinos

Physical Review D - Particles, Fields, Gravitation and Cosmology

Volumn 67, Issue 6, 2003, Pages

  Bottino, A ^a   Fornengo, N ^a   Scopel, S ^a  

^a UNIVERSITY OF TURIN   (Italy)

Author keywords

[No Author keywords available]

Indexed keywords

ARTICLE; DENSITY; ELASTICITY; MATHEMATICAL ANALYSIS; NEUTRON;

EID: 0038408692     PISSN: 15507998     EISSN: 15502368     Source Type: Journal    
DOI: 10.1103/PhysRevD.67.063519     Document Type: Article

References (45)

1. J. Ellis, K. Enqvist, D. V. Nanopoulos, and K. Tamvakis, Phys. Lett. 155B, 381 (1985)
2. Phys. Lett.M. Drees, 158B, 409 (1985)
3. M. DreesPhys. Rev. D 33, 1468 (1986).
4. M. Drees and X. Tata, Phys. Rev. D 43, 2971 (1991).
5. K. Griest and L. Roszkowski, Phys. Rev. D 46, 3309 (1992).
6. S. Mizuta, D. Ng, and M. Yamaguchi, Phys. Lett. B 300, 96 (1993).
7. A. Gabutti, M. Olechowski, S. Cooper, S. Pokorski, and L. Stodolsky, Astropart. Phys. 6, 1 (1996).
8. G. Bélanger, F. Boudjema, F. Donato, R. Godbole, and S. Rosier-Lees, Nucl. Phys. B581, 3 (2000).
9. A. Corsetti and P. Nath, Phys. Rev. D 64, 125010 (2001).
10. R. Arnowitt, B. Dutta, and Y. Santoso, hep-ph/0010244.
11. D. G. Cerdeño, S. Khalil, and C. Muñoz, hep-ph/0105180.
12. V. A. Bednyakov and H. V. Klapdor-Kleingrothaus, Phys. Rev. D 63, 095005 (2001).
13. H. Baer, C. Balazs, A. Belyaev, R. Dermisek, A. Mafi, and A. Mustfayev, J. High Energy Phys. 05, 061 (2002).
14. V. Bertin, E. Nezri, and J. Orloff, hep-ph/0210034.
15. A. Birkedal-Hansen and B. D. Nelson, hep-ph/0211071
16. A. Birkedal-HansenB. D. NelsonPhys. Rev. D 64, 015008 (2001).
17. A. Bottino, F. Donato, N. Fornengo, and S. Scopel, Phys. Lett. B 423, 109 (1998)
18. A. BottinoF. DonatoN. FornengoS. ScopelPhys. Rev. D 59, 095003 (1999)
19. Phys. Rev. DA. BottinoF. DonatoN. FornengoS. Scopel59, 095004 (1999)
20. Phys. Rev. DA. BottinoF. DonatoN. FornengoS. Scopel62, 056006 (2000).
21. ALEPH Collaboration, A. Colaleo, talk at SUSY’01, 2001, Dubna, Russia; DELPHI Collaboration, J. Abdallah et al., DELPHI 2001-085 CONF 513, 2001.
22. T. Affolder, Phys. Rev. Lett. 86, 4472 (2001).
23. CLEO Collaboration, S. Ahmed, CONF 99/10, hep-ex/9908022
24. ALEPH Collaboration, R. Barate, Phys. Lett. B 429, 169 (1998)
25. Phys. Lett. BBelle Collaboration, K. Abe, 511, 151 (2001).
26. A. Bottino, N. Fornengo, and S. Scopel, Nucl. Phys. B608, 461 (2001).
27. A. Bottino, F. Donato, N. Fornengo, and S. Scopel, Phys. Rev. D 63, 125003 (2001).
28. S. Ambrosanio, A. Dedes, S. Heinemeyer, S. Su, and G. Weiglein, Nucl. Phys. B624, 3 (2002).
29. Muon ((Formula presented)-2) Collaboration, G. W. Bennett, Phys. Rev. Lett. 89, 101804 (2002)
30. Phys. Rev. Lett.G. W. Bennett89, 129903(E) (2002).
31. M. Davier, S. Eidelman, A. Höcker, and Z. Zhang, hep-ph/0208177.
32. K. Hagiwara, A. D. Martin, D. Nomura, and T. Teubner, hep-ph/0209187.
33. A. Bottino, F. Donato, N. Fornengo, and S. Scopel, Astropart. Phys. 13, 215 (2000).
34. A. Bottino, F. Donato, N. Fornengo, and S. Scopel, Astropart. Phys. 18, 205 (2002).
35. A. Bottino, V. de Alfaro, N. Fornengo, G. Mignola, and M. Pignone, Astropart. Phys. 2, 67 (1994).
36. For a summary on WIMP direct detection experiments, see, for instance, A. Morales, Nucl. Phys. B (Proc. Suppl.) 110, 39 (2002).
37. DAMA/NaI Collaboration, R. Bernabei, Phys. Lett. B 389, 757 (1996).
38. CDMS Collaboration, D. Abrams, Phys. Rev. D 66, 122003 (2002).
39. A. Benoit, Phys. Lett. B 545, 43 (2002).
40. P. Belli, R. Cerulli, N. Fornengo, and S. Scopel, Phys. Rev. D 66, 043503 (2002).
41. DAMA/NaI Collaboration, R. Bernabei, Phys. Lett. B 480, 23 (2000)
42. R. BernabeiEur. Phys. J. C 18, 283 (2000).
43. G. Bélanger, F. Boudjema, A. Pukhov, and S. Rosier-Lees, hep-ph/0212227.
44. D. Hooper and T. Plehn, hep-ph/0212226.
45. This is at variance with the results of Refs. 3334, where a lower limit on the neutralino mass of 12 GeV 33 and 18 GeV 34 has been deduced. Notice that the authors of Refs. 3334 consider only the limit of very large (Formula presented) which strongly suppresses processes which involve A exchange, in particular the neutralino annihilation cross section. On the contrary, we are considering also the light Higgs sector, which is effective in reducing the value of the neutralino relic abundance and therefore in allowing lighter neutralinos [see Eq. (10)].