Did something decay, evaporate, or annihilate during big bang nucleosynthesis?

Physical Review D - Particles, Fields, Gravitation and Cosmology

Volumn 70, Issue 6, 2004, Pages

  Jedamzik, Karsten ^a  

^a CNRS   (France)

Author keywords

[No Author keywords available]

Indexed keywords

HYDROGEN; LITHIUM ION;

ARTICLE; BARYON; COSMOLOGICAL PHENOMENA; DECOMPOSITION; DENSITY; DESTRUCTION; ELEMENTARY PARTICLE; ENERGY TRANSFER; EVAPORATION; HADRON; NUCLEON;

EID: 84927724412     PISSN: 05562821     EISSN: None     Source Type: Journal    
DOI: 10.1103/PhysRevD.70.063524     Document Type: Article

References (61)

1. R. A. Malaney and G. J. Mathews, Phys. Rep. 229, 145 (1993); S. Sarkar, Rep. Prog. Phys. 59, 1493 (1996).
2. R. A. Malaney and G. J. Mathews, Phys. Rep. 229, 145 (1993); S. Sarkar, Rep. Prog. Phys. 59, 1493 (1996).
3. D. N. Spergel et al., Astrophys. J. Suppl. Ser. 148, 175 (2003).
4. D. Kirkman, D. Tytler, N. Suzuki, J. M. O'Meara, and D. Lubin, Astrophys. J. Suppl. Ser. 149, 1 (2003).
5. If not stated otherwise, quoted error bars are 1σ.
6. For example, for the same Ωbh2 Ref. [6] obtained 4.67 × 10-10, to be compared to the lower 3.82 × 10-10 by Ref. [7] and 4.15 × 10-10 by Ref. [8] at even higher Ωbh2 = 0.0224, as well as 4.9 × 10-10 by Ref. [9] at Ωbh2 = 0.023, indicating approximate uncertainties in the predictions.
7. S. Burles, K. M. Nollett, and M. S. Turner, Astrophys. J. 552, L1 (2001).
8. R. H. Cyburt, B. D. Fields, and K. A. Olive, Phys. Rev. D 69, 123519 (2004).
9. A. Coc, E. Vangioni-Flam, P. Descouvemont, A. Adahchour, and C. Angulo, astro-ph/0401008.
10. A. Cuoco, F. Iocco, G. Mangano, G. Miele, O. Pisanti, and P. D. Serpico, astro-ph/0307213.
11. S. G. Ryan, T. C. Beers, K. A. Olive, B. D. Fields, and J. E. Norris, Astrophys. J. Lett. 530, L57 (2000).
12. P. Bonifacio et al., Astron. Astrophys. 390, 91 (2002).
13. M. Asplund, M. Carlsson, and A. V. Botnen, Astron. Astrophys. 399, L31 (2003).
14. M. Lemoine, D. N. Schramm, J. W. Truran, and C. J. Copi, Astrophys. J. 478, 554 (1997).
15. E. Vangioni-Flam et al., New Astron. 4, 245 (1999).
16. M. Salaris and A. Weiss, Astron. Astrophys. 376, 955 (2001).
17. S. Theado and S. Vauclair, Astron. Astrophys. 375, 70 (2001).
18. M. H. Pinsonneault, G. Steigman, T. P. Walker, K. Narayanans, and V. K. Narayanan, Astrophys. J. 574, 398 (2002).
19. V. Luridiana, A. Peimbert, M. Peimbert, and M. Cervino, Astrophys. J. 592, 846 (2003).
20. Y. I. Izotov and T. X. Thuan, Astrophys. J. 602, 200 (2004).
21. K. Jedamzik, G. M. Fuller, and G. J. Mathews, Astrophys. J. 423, 50 (1994).
22. M. H. Reno and D. Seckel, Phys. Rev. D 37, 3441 (1988).
23. K. Kohri, Phys. Rev. D 64, 043515 (2001).
24. S. Dimopoulos, R. Esmailzadeh, L. J. Hall, and G. D. Starkman, Astrophys. J. 330, 545 (1988).
25. Y. L. Levitan, I. M. Sobol, M. Y. Khlopov, and V. M. Chechetkin, Sov. J. Nucl. Phys. 47, 109 (1988); E. V. Sedelnikov, S. S. Filippov, and M. Y. Khlopov, Phys. At. Nucl. 58, 235 (1995).
26. Y. L. Levitan, I. M. Sobol, M. Y. Khlopov, and V. M. Chechetkin, Sov. J. Nucl. Phys. 47, 109 (1988); E. V. Sedelnikov, S. S. Filippov, and M. Y. Khlopov, Phys. At. Nucl. 58, 235 (1995).
27. V. V. Smith, D. L. Lambert, and P. E. Nissen, Astrophys. J. 408, 262 (1993); 506, 405 (1998); L. M. Hobbs and J. A. Thorburn, Astrophys. J. 491, 772 (1997); R. Cayrel, M. Spite, F. Spite, E. Vangioni-Flam, M. Cassé, and J. Audouze, Astron. Astrophys. 343, 923 (1999); P. E. Nissen, M. Asplund, V. Hill, and S. D'Odorico, Astron. Astrophys. 357, L49 (2000).
28. V. V. Smith, D. L. Lambert, and P. E. Nissen, Astrophys. J. 408, 262 (1993); 506, 405 (1998); L. M. Hobbs and J. A. Thorburn, Astrophys. J. 491, 772 (1997); R. Cayrel, M. Spite, F. Spite, E. Vangioni-Flam, M. Cassé, and J. Audouze, Astron. Astrophys. 343, 923 (1999); P. E. Nissen, M. Asplund, V. Hill, and S. D'Odorico, Astron. Astrophys. 357, L49 (2000).
29. V. V. Smith, D. L. Lambert, and P. E. Nissen, Astrophys. J. 408, 262 (1993); 506, 405 (1998); L. M. Hobbs and J. A. Thorburn, Astrophys. J. 491, 772 (1997); R. Cayrel, M. Spite, F. Spite, E. Vangioni-Flam, M. Cassé, and J. Audouze, Astron. Astrophys. 343, 923 (1999); P. E. Nissen, M. Asplund, V. Hill, and S. D'Odorico, Astron. Astrophys. 357, L49 (2000).
30. V. V. Smith, D. L. Lambert, and P. E. Nissen, Astrophys. J. 408, 262 (1993); 506, 405 (1998); L. M. Hobbs and J. A. Thorburn, Astrophys. J. 491, 772 (1997); R. Cayrel, M. Spite, F. Spite, E. Vangioni-Flam, M. Cassé, and J. Audouze, Astron. Astrophys. 343, 923 (1999); P. E. Nissen, M. Asplund, V. Hill, and S. D'Odorico, Astron. Astrophys. 357, L49 (2000).
31. V. V. Smith, D. L. Lambert, and P. E. Nissen, Astrophys. J. 408, 262 (1993); 506, 405 (1998); L. M. Hobbs and J. A. Thorburn, Astrophys. J. 491, 772 (1997); R. Cayrel, M. Spite, F. Spite, E. Vangioni-Flam, M. Cassé, and J. Audouze, Astron. Astrophys. 343, 923 (1999); P. E. Nissen, M. Asplund, V. Hill, and S. D'Odorico, Astron. Astrophys. 357, L49 (2000).
32. P. E. Nissen, D. L. Lambert, F. Primas, and V. V. Smith, Astron. Astrophys. 348, 211 (1999).
33. It may be that this is simply a selection effect as most of these claimed detections are only around 2σ.
34. K. M. Nollett, M. Lemoine, and D. N. Schramm, Phys. Rev. C 56, 1144 (1997).
35. E. Vangioni-Flam, M. Cassé, R. Cayrel, J. Audouze, M. Spite, and F. Spite, New Astron. 4, 245 (1999); B. D. Fields and K. A. Olive, New Astron. 4, 255 (1999).
36. E. Vangioni-Flam, M. Cassé, R. Cayrel, J. Audouze, M. Spite, and F. Spite, New Astron. 4, 245 (1999); B. D. Fields and K. A. Olive, New Astron. 4, 255 (1999).
37. R. Ramaty, S. T. Scully, R. E. Lingenfelter, and B. Kozlovsky, Astrophys. J. 534, 747 (2000).
38. A. Alibés, J. Labay, and R. Canal, Astrophys. J. 571, 326 (2002).
39. T. K. Suzuki and S. Inoue, Astrophys. J. 573, 168 (2002).
40. K. Jedamzik, Phys. Rev. Lett. 84, 3248 (2000).
41. Such considerations are also very useful to derive constraints on late-decaying particles in the early Universe.
42. The analysis does not currently include the effects from antinucleons. An antinucleon scatters not more than 1-2 times on nucleons before an annihilation reaction occurs. Because of the small 4He/H ratio it thus has a probability of roughly 10% to annihilate on 4He, thereby 1 producing around ∼0.3 D, 3He, and 3H per annihilation. One may therefore expect ∼0.03 D (3He and 3H) per injected antinucleon. This should be compared to ∼1 D (see text below) produced per annihilation by injected energetic nucleons, since those latter may scatter of the order 10-20 times before falling below the threshold for 4He spallation.
43. M. S. Smith, L. H. Kawano, and R. A. Malaney, Astrophys. J. Suppl. Ser. 85, 219 (1993).
44. C. Angulo et al., Nucl. Phys. A656, 3 (1999).
45. T. Sjöstrand, P. Edén, C. Friberg, L. Lönnblad, G. Miu, S. Mrenna, and E. Norrbin, Comput. Phys. Commun. 135, 238 (2001); www.thep.lu.se/torbjorn/Pythia.html
46. For higher particle masses m ≳ 1 TeV, the ratio of secondary to primary neutrons is more of the order of ∼10.
47. Note here that predictions become less accurate for higher mass particles due to poor reaction rate data at high energies. Whereas the typical energy of a nucleon generated during the decay of a mx = 200 GeV particle is 8 GeV, it is 55 GeV for a mx = 4 TeV particle.
48. The decay may still be envisioned as baryon number nonviolating, as it may be associated with the injection of one n̄ p̄ pair. These latter particles predominantly annihilate on protons, thus effectively yielding the injection of one energetic np pair, and the annihilation of two thermal protons. In any case, due to the weakness of the source, the removal, or nonremoval, of thermal protons has a negligible effect on the final result. As argued above [35], cascade produced D due to antinucleon-annihilation on 4He is a subdominant ∼10% effect, which nevertheless, becomes stronger for lower energy primary nucleons.
49. K. Enqvist and A. Mazumdar, Phys. Rep. 380, 99 (2003).
50. E. Witten, Phys. Rev. D 30, 272 (1984).
51. J. L. Feng, A. Rajaraman, and F. Takayama, Phys. Rev. D 68, 063504 (2003).
52. A. Bottino, N. Fornengo, and S. Scopel, Phys. Rev. D 67, 063519 (2003).
53. For a short discussion of uncertainties in observationally inferred light-element abundances the reader is also referred to B. Fields and S. Sarkar, Phys. Lett. B 592, 1 (2004).
54. S. Burles and D. Tytler, astro-ph/9712109.
55. S. Burles and D. Tytler, Astrophys. J. 499, 699 (1998).
56. T. Moroi, H. Murayama, and M. Yamaguchi, Phys. Lett. B 303, 289 (1993); M. Bolz, A. Brandenburg, and W. Buchmuller, Nucl. Phys. B606, 518 (2001).
57. T. Moroi, H. Murayama, and M. Yamaguchi, Phys. Lett. B 303, 289 (1993); M. Bolz, A. Brandenburg, and W. Buchmuller, Nucl. Phys. B606, 518 (2001).
58. Even when the decay channel into gluons, for example, due to kinematic reasons is disallowed, decay into the U(1)Y B-gauge boson may induce the injection of nucleons, since the B is a mixture between the photon and the Z, with the latter having an appreciable branching ratio into quarks. Nevertheless, in this case a gravitino mass of the order of 8 TeV is required.
59. M. Bolz,W. Buchmuller, and M. Plumacher, Phys. Lett. B 443, 209 (1998).
60. K. Jedamzik, M. Lemoine, and G. Moultaka (to be published).
61. J. L. Feng, A. Rajaraman, and F. Takayama, Phys. Rev. Lett. 91, 011302 (2003).