Neutrinos as the source of ultrahigh energy cosmic rays in extra dimensions

Ashok Goyal; Abhinav Gupta; Namit Mahajan

doi:10.1103/PhysRevD.63.043003

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Neutrinos as the source of ultrahigh energy cosmic rays in extra dimensions

Ashok Goyal^*, Abhinav Gupta^†, and Namit Mahajan^‡

Department of Physics and Astrophysics, University of Delhi, Delhi 110 007, India

^*Email address: agoyal@ducos.ernet.in
^†Email address: abh@ducos.ernet.in, abhinav@physics.du.ac.in
^‡Email address: nm@ducos.ernet.in, nmahajan@physics.du.ac.in

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Phys. Rev. D 63, 043003 – Published 23 January, 2001

DOI: https://doi.org/10.1103/PhysRevD.63.043003

Abstract

If neutrinos are to be identified with the primary source of ultrahigh energy cosmic rays (UHECR), their interaction on relic neutrinos is of great importance in understanding their long intergalactic journey. In theories with large compact dimensions, the exchange of a tower of massive spin-2 gravitons (Kaluza-Klein excitations) gives an extra contribution to $ν \bar{ν} \to f \bar{f}$ and $γ γ$ processes along with the opening of a new channel for the neutrinos to annihilate with the relic cosmic neutrino background $ν \bar{ν} \to G_{kk}$ to produce bulk gravitons in the extra dimensions. This will affect their attenuation. We compute the contribution of these Kaluza-Klein excitations to the above processes and find that for parameters of the theory constrained by supernova cooling, the contribution does indeed become the dominant contribution above $\sqrt{s} ≃ 300 GeV .$

References (18)

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See also the discussion in C. Tyler, A. V. Olinto, and G. Sigl, hep-ph/0002257, wherein they have proposed that from the measurements of horizontal air showers, one can put bounds on the UHE neutrino flux striking the earth. This, in turn, can be used for putting bounds on UHE neutrino interactions with matter beyond the standard model. Thus, the modification in neutrino propagation in theories with large extra dimensions can, in principle, be tested.

[c1] M. Takeda et al., Phys. Rev. Lett. 81, 1163 (1998); S. Yoshida et al., Astropart. Phys. 3, 105 (1995); N. Hayashida et al., Phys. Rev. Lett. 73, 3491 (1994); M. A. Lawrence, R. J. Reid, and A. A. Watson, J. Phys. G 17, 733 (1991); Fly’s Eye Collaboration, D. J. Bird et al., Phys. Rev. Lett. 71, 3401 (1993); D. J. BirdAstrophys. J. 424, 491 (1994).

[c2] K. Greisen, Phys. Rev. Lett. 16, 748 (1966); G. T. Zatsepin and V. A. Kuzmin, Zh. Éksp. Teor. Fiz. 4, 114 (1966) [JETP Lett. 4, 78 (1966)].

[c3] See, for example, P. L. Biermann, J. Phys. G 23, 1 (1997), and references cited therein.

[c4] V. S. Berezinskii et al., Astrophysics of Cosmic Rays (North-Holland, Amsterdam, 1990); M. S. Langair, High Energy Astrophysics, 2nd ed. (Cambridge University Press, Cambridge, England, 1994).

[c5] T. Weiler, Astropart. Phys. 11, 303 (1999).

[c6] G. Gelmini and A. Kusenko, Phys. Rev. Lett. 84, 1378 (2000).

[c7] R. Gandhi, C. Quigg, M. H. Reno, and I. Sarcevic, Astropart. Phys. 5, 81 (1996); Phys. Rev. D 58, 093009 (1998).

[c8] N. Arkani-Hamed, S. Dimopoulos, and G. Dvali, Phys. Lett. B 429, 263 (1998); Phys. Rev. D 59, 086004 (1999); I. Antoniadis, N. Arkani-Hamed, S. Dimopoulos, and G. Dvali, Phys. Lett. B 436, 257 (1998).

[c9] S. Nussinov and R. Shrock, Phys. Rev. D 59, 105002 (1999); P. Jain, D. W. Makay, S. Panda, and J. P. Ralstan, Phys. Lett. B 484, 267 (2000).

[c10] S. Cullen and M. Pereslstein, Phys. Rev. Lett. 83, 268 (1999); V. Barger, T. Han, C. Kao, and R. J. Zhang, Phys. Lett. B 461, 34 (1999).

[c11] M. Gell-Mann, Phys. Rev. Lett. 6, 70 (1961); C. N. Yang, Phys. Rev. 77, 242 (1950); V. K. Cung and M. Yoshimura, Nuovo Cimento A 29, 557 (1975).

[c12] T. Han, J. D. Lykken, and R. J. Zhang, Phys. Rev. D 59, 105006 (1999); G. F. Giudice, R. Rattazi, and J. D. Wells, Nucl. Phys. B544, 3 (1999).

[c13] M. Bando, T. Kugo, T. Noguchi, and K. Yoshioka, Phys. Rev. Lett. 83, 3601 (1999).

[c14] M. Kachelriess and M. Plumacher, Phys. Rev. D 62, 103006 (2000).

[c15] D. A. Dicus, C. Kao, and W. W. Repko, Phys. Rev. D 59, 013005 (1998).

[c16] I. S. Gradshteyn and I. M. Ryzhik, Table of Integrals, Series, and Products (Academic Press, New York, 1994).

[c17] See, for example, J. Adams and S. Sarkar, ICTP Workshop on Physics of the Relic Neutrinos, Trieste, Italy, 1996; J. Lesgourgnes and S. Pastov, Phys. Rev. D 60, 103521 (1999).

[c18] See also the discussion in C. Tyler, A. V. Olinto, and G. Sigl, hep-ph/0002257, wherein they have proposed that from the measurements of horizontal air showers, one can put bounds on the UHE neutrino flux striking the earth. This, in turn, can be used for putting bounds on UHE neutrino interactions with matter beyond the standard model. Thus, the modification in neutrino propagation in theories with large extra dimensions can, in principle, be tested.

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Neutrinos as the source of ultrahigh energy cosmic rays in extra dimensions

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