- Physical Review Journals
All JournalsPhysics Magazine
Access Provided by Xinjiang University

Physical Review D

Export citation

Export citation

Choose format for download:

Download Citation
  • Access by Xinjiang University

Destruction of Be7 in big bang nucleosynthesis via long-lived sub-strongly interacting massive particles as a solution to the Li problem

Masahiro Kawasaki1,2 and Motohiko Kusakabe1,*

  • 1Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
  • 2Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Chiba 277-8582, Japan

  • *kusakabe@icrr.u-tokyo.ac.jp
PDF

Phys. Rev. D 83, 055011 – Published 18 March, 2011

DOI: https://doi.org/10.1103/PhysRevD.83.055011

Abstract

We identify reactions which destroy Be7 and Li7 during big bang nucleosynthesis (BBN) in the scenario of BBN catalyzed by a long-lived sub-strongly-interacting massive particle (sub-SIMP or X particle). The destruction associated with nonradiative X captures of the nuclei can be realized only if the interaction strength between an X particle and a nucleon is properly weaker than that between two nucleons to a degree depending on the mass of X. Binding energies of nuclei to an X particle are estimated taking the mass and the interaction strength to nuclei of the X as input parameters. Nuclear reaction rates associated with the X are estimated naively and adopted in calculating evolutions of nuclear abundances. We suggest that the Li7 problem, which might be associated with as-yet-unrecognized particle processes operating during BBN, can be solved if the X particle interacts with nuclei strongly enough to drive Be7 destruction but not strongly enough to form a bound state with He4 of relative angular momentum L=1. Justifications of this scenario by rigorous calculations of reaction rates using quantum mechanical many-body models are highly desirable since this result involves many significant uncertainties.

View figure in article

Article Text

References (134)

  1. D. A. Dicus and V. L. Teplitz, Phys. Rev. Lett. 44, 218 (1980).
  2. R. Plaga, Phys. Rev. D 51, 6504 (1995).
  3. R. N. Mohapatra and V. L. Teplitz, Phys. Rev. Lett. 81, 3079 (1998).
  4. M. Kusakabe, T. Kajino, T. Yoshida, and G. J. Mathews, Phys. Rev. D 80, 103501 (2009).
  5. M. Pospelov, Phys. Rev. Lett. 98, 231301 (2007).
  6. K. Kohri and F. Takayama, Phys. Rev. D 76, 063507 (2007).
  7. R. H. Cyburt, J. R. Ellis, B. D. Fields, K. A. Olive, and V. C. Spanos, J. Cosmol. Astropart. Phys. 11 (2006) 014.
  8. K. Hamaguchi, T. Hatsuda, M. Kamimura, Y. Kino, and T. T. Yanagida, Phys. Lett. B 650, 268 (2007).
  9. C. Bird, K. Koopmans, and M. Pospelov, Phys. Rev. D 78, 083010 (2008).
  10. M. Kusakabe, T. Kajino, R. N. Boyd, T. Yoshida, and G. J. Mathews, Phys. Rev. D 76, 121302 (2007).
  11. M. Kusakabe, T. Kajino, R. N. Boyd, T. Yoshida, and G. J. Mathews, Astrophys. J. 680, 846 (2008).
  12. M. Kusakabe, T. Kajino, T. Yoshida, and G. J. Mathews, Phys. Rev. D 81, 083521 (2010).
  13. K. Jedamzik, Phys. Rev. D 77, 063524 (2008).
  14. K. Jedamzik, J. Cosmol. Astropart. Phys. 03 (2008) 008.
  15. M. Kamimura, Y. Kino, and E. Hiyama, Prog. Theor. Phys. 121, 1059 (2009).
  16. M. Pospelov, arXiv:0712.0647.
  17. M. Kawasaki, K. Kohri, and T. Moroi, Phys. Lett. B 649, 436 (2007).
  18. T. Jittoh et al., Phys. Rev. D 76, 125023 (2007).
  19. T. Jittoh et al., Phys. Rev. D 78, 055007 (2008).
  20. T. Jittoh et al., Phys. Rev. D 82, 115030 (2010).
  21. M. Pospelov, J. Pradler, and F. D. Steffen, J. Cosmol. Astropart. Phys. 11 (2008) 020.
  22. M. Y. Khlopov and C. Kouvaris, Phys. Rev. D 77, 065002 (2008).
  23. J. R. Ellis, D. V. Nanopoulos, and S. Sarkar, Nucl. Phys. B259, 175 (1985).
  24. R. H. Cyburt, J. R. Ellis, B. D. Fields, and K. A. Olive, Phys. Rev. D 67, 103521 (2003).
  25. J. R. Ellis, K. A. Olive, and E. Vangioni, Phys. Lett. B 619, 30 (2005).
  26. N. Terasawa, M. Kawasaki, and K. Sato, Nucl. Phys. B302, 697 (1988).
  27. M. Kawasaki et al., Nucl. Phys. B419, 105 (1994).
  28. M. Kawasaki and T. Moroi, Prog. Theor. Phys. 93, 879 (1995).
  29. E. Holtmann, M. Kawasaki, and T. Moroi, Phys. Rev. Lett. 77, 3712 (1996).
  30. M. Kawasaki, K. Kohri, and T. Moroi, Phys. Rev. D 63, 103502 (2001).
  31. M. Kawasaki, K. Kohri, and T. Moroi, Phys. Lett. B 625, 7 (2005).
  32. M. Kawasaki, K. Kohri, and T. Moroi, Phys. Rev. D 71, 083502 (2005).
  33. T. Kanzaki, M. Kawasaki, K. Kohri, and T. Moroi, Phys. Rev. D 75, 025011 (2007).
  34. M. Kawasaki, K. Kohri, T. Moroi, and A. Yotsuyanagi, Phys. Rev. D 78, 065011 (2008).
  35. D. Cumberbatch et al., Phys. Rev. D 76, 123005 (2007).
  36. M. H. Reno and D. Seckel, Phys. Rev. D 37, 3441 (1988).
  37. S. Dimopoulos, R. Esmailzadeh, L. J. Hall, and G. D. Starkman, Astrophys. J. 330, 545 (1988).
  38. S. Dimopoulos, R. Esmailzadeh, L. J. Hall, and G. D. Starkman, Phys. Rev. Lett. 60, 7 (1988).
  39. S. Dimopoulos, R. Esmailzadeh, L. J. Hall, and G. D. Starkman, Nucl. Phys. B311, 699 (1989).
  40. M. Y. Khlopov, Y. L. Levitan, E. V. Sedelnikov, and I. M. Sobol, Phys. At. Nucl. 57, 1393 (1994).
  41. E. V. Sedelnikov, S. S. Filippov, and M. Y. Khlopov, Phys. At. Nucl. 58, 235 (1995).
  42. K. Jedamzik, Phys. Rev. Lett. 84, 3248 (2000).
  43. K. Jedamzik, Phys. Rev. D 70, 063524 (2004).
  44. K. Jedamzik, Phys. Rev. D 70, 083510 (2004).
  45. K. Jedamzik, K.-Y. Choi, L. Roszkowski, and R. Ruiz de Austri, J. Cosmol. Astropart. Phys. 07 (2006) 007.
  46. K. Jedamzik, Phys. Rev. D 74, 103509 (2006).
  47. M. Kusakabe, T. Kajino, and G. J. Mathews, Phys. Rev. D 74, 023526 (2006).
  48. M. Kusakabe et al., Phys. Rev. D 79, 123513 (2009).
  49. M. Pospelov and J. Pradler, Phys. Rev. D 82, 103514 (2010).
  50. M. Pospelov and J. Pradler, arXiv:1010.4079.
  51. J. Melendez and I. Ramirez, Astrophys. J. 615, L33 (2004).
  52. M. Asplund, D. L. Lambert, P. E. Nissen, F. Primas, and V. V. Smith, Astrophys. J. 644, 229 (2006).
  53. F. Spite and M. Spite, Astron. Astrophys. 115, 357 (1982).
  54. S. G. Ryan, T. C. Beers, K. A. Olive, B. D. Fields, and J. E. Norris, Astrophys. J. 530, L57 (2000).
  55. P. Bonifacio, P. Molaro, T. Sivarani, R. Cayrel, M. Spite, F. Spite, B. Plez, J. Andersen, B. Barbuy, T. C. Beers et al., Astron. Astrophys. 462, 851 (2007).
  56. J. R. Shi, T. Gehren, H. W. Zhang, J. L. Zeng, and G. Zhao, Astron. Astrophys. 465, 587 (2007).
  57. W. Aoki et al., Astrophys. J. 698, 1803 (2009).
  58. R. H. Cyburt, B. D. Fields, and K. A. Olive, J. Cosmol. Astropart. Phys. 11 (2008) 012.
  59. D. Larson et al., Astrophys. J. Suppl. Ser. 192, 16 (2011).
  60. O. Richard, G. Michaud, and J. Richer, Astrophys. J. 619, 538 (2005).
  61. A. J. Korn et al., Nature (London) 442, 657 (2006).
  62. K. Lind, F. Primas, C. Charbonnel, F. Grundahl, and M. Asplund, Astron. Astrophys. 503, 545 (2009).

  63. Recently, a new measurement of the cross section of radiative capture by deuteron and the Li6 abundance predicted based upon the result have been reported [64].

  64. F. Hammache et al., Phys. Rev. C 82, 065803 (2010).
  65. R. Cayrel et al., Astron. Astrophys. 473, L37 (2007).
  66. M. Steffen, R. Cayrel, P. Bonifacio, H. G. Ludwig, and E. Caffau, arXiv:0910.5917.
  67. N. Prantzos, Astron. Astrophys. 448, 665 (2006).

  68. [A/H]=log(A/H)−log(A/H)⊙ is the number ratio of nuclide A to H measured in a logarithmic scale normalized to the solar value.

  69. R. N. Boyd, C. R. Brune, G. M. Fuller, and C. J. Smith, Phys. Rev. D 82, 105005 (2010).
  70. R. H. Cyburt and M. Pospelov, arXiv:0906.4373.
  71. N. Chakraborty, B. D. Fields, and K. A. Olive, arXiv:1011.0722.
  72. N. Arkani-Hamed and S. Dimopoulos, J. High Energy Phys. 06 (2005) 073.
  73. N. Arkani-Hamed, S. Dimopoulos, G. F. Giudice, and A. Romanino, Nucl. Phys. B709, 3 (2005).
  74. S. Raby, Phys. Lett. B 422, 158 (1998).
  75. S. Shirai, M. Yamazaki, and K. Yonekura, J. High Energy Phys. 06 (2010) 056.
  76. L. Covi, M. Olechowski, S. Pokorski, K. Turzynski, and J. D. Wells, J. High Energy Phys. 01 (2011) 033.
  77. U. Sarid and S. D. Thomas, Phys. Rev. Lett. 85, 1178 (2000).
  78. J. Hisano, K. Nakayama, S. Sugiyama, T. Takesako, and M. Yamanaka, Phys. Lett. B 691, 46 (2010).
  79. K. Nakayama, F. Takahashi, and T. T. Yanagida, arXiv:1010.5693.
  80. J. Kang, M. A. Luty, and S. Nasri, J. High Energy Phys. 09 (2008) 086.
  81. H. Baer, K.-m. Cheung, and J. F. Gunion, Phys. Rev. D 59, 075002 (1999).
  82. E. W. Kolb and M. S. Turner, The Early Universe (Addison-Wesley, Reading, MA, 1990).
  83. S. Wolfram, Phys. Lett. B 82, 65 (1979).
  84. C. B. Dover, T. K. Gaisser, and G. Steigman, Phys. Rev. Lett. 42, 1117 (1979).
  85. G. D. Starkman, A. Gould, R. Esmailzadeh, and S. Dimopoulos, Phys. Rev. D 41, 3594 (1990).
  86. K. Nakamura and Particle Data Group, J. Phys. G 37, 075021 (2010).
  87. N. Prantzos, M. Casse, and E. Vangioni-Flam, Astrophys. J. 403, 630 (1993).
  88. R. Ramaty, B. Kozlovsky, R. E. Lingenfelter, and H. Reeves, Astrophys. J. 488, 730 (1997).
  89. M. Kusakabe, Astrophys. J. 681, 18 (2008).
  90. S. E. Woosley and T. A. Weaver, Astrophys. J. Suppl. Ser. 101, 181 (1995).
  91. T. Yoshida, T. Kajino, and D. H. Hartmann, Phys. Rev. Lett. 94, 231101 (2005).

  92. These parameters have been adjusted to fit the deuteron binding energy and low-energy triplet-even proton-neutron scattering phase shifts [93, 94].

  93. M. Yahiro, Y. Iseri, H. Kameyama, M. Kamimura, and M. Kawai, Prog. Theor. Phys. Suppl. 89, 32 (1986).
  94. N. Austern et al., Phys. Rep. 154, 125 (1987).

  95. This value is an example which leads to the binding energy of deuteron when another parameter is fixed to be v0w=−25.5  MeV.

  96. E. Hiyama, M. Kamimura, T. Motoba, T. Yamada, and Y. Yamamoto, Phys. Rev. C 66, 024007 (2002).
  97. E. Hiyama, Y. Kino, and M. Kamimura, Prog. Part. Nucl. Phys. 51, 223 (2003).
  98. J. Martorell, D. W. L. Sprung, and D. C. Zheng, Phys. Rev. C 51, 1127 (1995).
  99. A. Amroun et al., Nucl. Phys. A 579, 596 (1994).
  100. I. Tanihata et al., Phys. Lett. B 206, 592 (1988).
  101. M. Fukuda, M. Mihara, T. Fukao, S. Fukuda, M. Ishihara, S. Ito, T. Kobayashi, K. Matsuta, T. Minamisono, S. Momota et al., Nucl. Phys. A 656, 209 (1999).
  102. C. Angulo et al., Nucl. Phys. A 656, 3 (1999).
  103. R. N. Boyd, An Introduction to Nuclear Astrophysics (University of Chicago, Chicago, 2008).
  104. W. A. Fowler, G. R. Caughlan, and B. A. Zimmerman, Annu. Rev. Astron. Astrophys. 5, 525 (1967).
  105. G. R. Caughlan and W. A. Fowler, At. Data Nucl. Data Tables 40, 283 (1988).
  106. M. Sowerby, J. Nucl. Energy 24, 323 (1970).

  107. The BeX6 nucleus produced in this reaction pathway immediately p decays into HeX4 and two protons.

  108. C. A. Bertulani, Comput. Phys. Commun. 156, 123 (2003).
  109. G. G. Simon, C. Schmitt, and V. H. Walther, Nucl. Phys. A 364, 285 (1981).
  110. D. R. Tilley et al., Nucl. Phys. A 708, 3 (2002).
  111. L. Kawano, Recon Technical Report N, 92, 25163 (NASA STI Program, Hanover, MD, 1992).
  112. M. S. Smith, L. H. Kawano, and R. A. Malaney, Astrophys. J. Suppl. Ser. 85, 219 (1993).
  113. P. Descouvemont, A. Adahchour, C. Angulo, A. Coc, E. Vangioni-Flamand , At. Data Nucl. Data Tables 88, 203 (2004).
  114. G. J. Mathews, T. Kajino, and T. Shima, Phys. Rev. D 71, 021302 (2005).

  115. This reaction can be efficient since the reaction Q-value of X(Li7,t)HeX4 is very small (see Table II).

  116. http://www.tunl.duke.edu/nucldata/index.shtml.

  117. The reaction rates and related information of HeX4(d,Li6)X, HeX4(t,Li7)X and HeX4(He,3Be7)X in the case of leptonic X− particle can be found in Refs. [8, 15].

  118. M. Kusakabe, T. Kajino, and G. J. Mathews, Proceedings in the Open Access Journal of Physics: Conference Series, (IOP Publishing, Bristol, England, to be published).
  119. M. Kamimura, Y. Kino, and E. Hiyama, in American Institute of Physics Conference Series, edited by H. Susa, M. Arnould, S. Gales, T. Motobayashi, C. Scheidenberger, and H. Utsunomiya, American Institute of Physics Conference Series Vol. 1238 (American Institute of Physics, Melville, NY, 2010), pp. 139–144.
  120. E. Rollinde, E. Vangioni, and K. A. Olive, Astrophys. J. 651, 658 (2006).
  121. E. Rollinde, D. Maurin, E. Vangioni, K. A. Olive, and S. Inoue, Astrophys. J. 673, 676 (2008).
  122. R. N. Boyd and T. Kajino, Astrophys. J. 336, L55 (1989).
  123. T. Kajino and R. N. Boyd, Astrophys. J. 359, 267 (1990).
  124. T. Kajino, G. J. Mathews, and G. M. Fuller, Astrophys. J. 364, 7 (1990).
  125. A. Coc, P. Delbourgo-Salvador, F. de Oliveira, P. Aguer, S. Barhoumi, G. Bogaert, J. Kiener, A. Lafebvre, and J. P. Thibaud, Astrophys. J. 402, 62 (1993).
  126. M. Orito, T. Kajino, R. N. Boyd, and G. J. Mathews, Astrophys. J. 488, 515 (1997).
  127. M. Pettini, B. J. Zych, M. T. Murphy, A. Lewis, and C. C. Steidel Mon. Not. R. Astron. Soc. 391, 1499 (2008).
  128. T. M. Bania, R. T. Rood, and D. S. Balser, Nature (London) 415, 54 (2002).
  129. C. Chiappini, A. Renda, and F. Matteucci, Astron. Astrophys. 395, 789 (2002).
  130. E. Vangioni-Flam, K. A. Olive, B. D. Fields, and M. Casse, Astrophys. J. 585, 611 (2003).
  131. K. Lodders, Astrophys. J. 591, 1220 (2003).
  132. Y. I. Izotov and T. X. Thuan, Astrophys. J. 710, L67 (2010).
  133. E. Aver, K. A. Olive, and E. D. Skillman, J. Cosmol. Astropart. Phys. 05 (2010) 003.
  134. H. Ito, W. Aoki, S. Honda, and T. C. Beers, Astrophys. J. 698, L37 (2009).

Outline

Information

Phys. Rev. D 83, 055011– Published 18 March, 2011
  • Received 14 December 2010

© 2011 American Physical Society

Sign In to Your Journals Account

Filter

Filter

Article Lookup

Enter a citation