-
2
-
-
0347416177
-
-
I. Antoniadis, N. Arkani-Hamed, S. Dimopoulos, and G. Dvali, ibid. 436, 257 (1998).
-
(1998)
Phys. Lett. B
, vol.436
, pp. 257
-
-
Antoniadis, I.1
Arkani-Hamed, N.2
Dimopoulos, S.3
Dvali, G.4
-
7
-
-
0033525985
-
-
See, for instance, G. F. Giudice, R. Rattazzi, and J. D. Wells, Nucl. Phys. B544, 3 (1999),
-
(1999)
Nucl. Phys.
, vol.B544
, pp. 3
-
-
Giudice, G.F.1
Rattazzi, R.2
Wells, J.D.3
-
10
-
-
0000804427
-
-
T. G. Rizzo, hep-ph/9910255
-
E. A. Mirabelli, M. Perelstein, and M. E. Peskin, ibid. 82, 2236 (1999); T. G. Rizzo, hep-ph/9910255;
-
(1999)
Phys. Rev. Lett.
, vol.82
, pp. 2236
-
-
Mirabelli, E.A.1
Perelstein, M.2
Peskin, M.E.3
-
14
-
-
0008138888
-
-
See, for instance, C. Csâki, M. Graesser, C. Kolda, and J. Terning, Phys. Lett. B 462, 34 (1999);
-
(1999)
Phys. Lett. B
, vol.462
, pp. 34
-
-
Csâki, C.1
Graesser, M.2
Kolda, C.3
Terning, J.4
-
16
-
-
17044366079
-
-
C. Csaki, M. Graesser, L. Randall, and J. Terning, Phys. Rev. D 62, 045015 (2000);
-
(2000)
Phys. Rev. D
, vol.62
, pp. 045015
-
-
Csaki, C.1
Graesser, M.2
Randall, L.3
Terning, J.4
-
21
-
-
0011323708
-
-
N. Arkani-Hamed, S. Dimopoulos, G. Dvali, and N. Kaloper, J. High Energy Phys. 12, 010 (2000);
-
(2000)
J. High Energy Phys.
, vol.12
, pp. 010
-
-
Arkani-Hamed, N.1
Dimopoulos, S.2
Dvali, G.3
Kaloper, N.4
-
22
-
-
0002269325
-
-
V. Barger, T. Han, C. Kao, and R. J. Zhang, Phys. Lett. B 461, 34 (1999);
-
(1999)
Phys. Lett. B
, vol.461
, pp. 34
-
-
Barger, V.1
Han, T.2
Kao, C.3
Zhang, R.J.4
-
24
-
-
0034713138
-
-
S. Cassisi, V. Castellani, S. Degl'Innocenti, G. Fiorentini, and B. Ricci, ibid. 481, 323 (2000).
-
(2000)
Phys. Lett. B
, vol.481
, pp. 323
-
-
Cassisi, S.1
Castellani, V.2
Degl'Innocenti, S.3
Fiorentini, G.4
Ricci, B.5
-
33
-
-
0000341976
-
-
L3 Collaboration, M. Acciarri et al. Phys. Lett. B 470, 281 (1999);
-
(1999)
Phys. Lett. B
, vol.470
, pp. 281
-
-
Acciarri, M.1
-
34
-
-
0034720088
-
-
H1 Collaboration, C. Adloff et al. ibid. 479, 358 (2000);
-
(2000)
Phys. Lett. B
, vol.479
, pp. 358
-
-
Adloff, C.1
-
35
-
-
10944224909
-
-
DO Collaboration, B. Abbott et ai, Phys. Rev. Lett. 86, 1156(2001).
-
(2001)
Phys. Rev. Lett.
, vol.86
, pp. 1156
-
-
Abbott, B.1
-
38
-
-
0034164989
-
-
For a comprehensive review on the origin of the highest energy cosmic rays the reader is referred to P. Bhattacharjee and G. Sigl, Phys. Rep. 327, 109 (2000).
-
(2000)
Phys. Rep.
, vol.327
, pp. 109
-
-
Bhattacharjee, P.1
Sigl, G.2
-
41
-
-
0001828155
-
-
[JETP Lett. 4, 78 (1966)].
-
(1966)
JETP Lett.
, vol.4
, pp. 78
-
-
-
42
-
-
33750665864
-
-
E.-J. Ahn, G. Medina-Tanco, P. L. Biermann, and T. Stanev, astro-ph/9911123; G. Farrar and T. Piran, astro-ph/0010370
-
The observed near-isotropy of the distribution can be explained, within a single-source hypothesis, postulating a galactic wind or a large extragalactic magnetic field. E.-J. Ahn, G. Medina-Tanco, P. L. Biermann, and T. Stanev, astro-ph/9911123; G. Farrar and T. Piran, astro-ph/0010370.
-
-
-
-
43
-
-
4243810300
-
-
None of these models, however, could explain directional clustering as discussed by AGASA Collaboration, N. Hayashida et ai, Phys. Rev. Lett. 77, 1000 (1996);
-
(1996)
Phys. Rev. Lett.
, vol.77
, pp. 1000
-
-
Hayashida, N.1
-
44
-
-
0033192151
-
-
astro-ph/9902239
-
M. Takeda et al, Astrophys. J. 522, 225 (1999); astro-ph/9902239;
-
(1999)
Astrophys. J.
, vol.522
, pp. 225
-
-
Takeda, M.1
-
45
-
-
0001628425
-
-
For a recent analytic analysis, see H. Goldberg and T. J. Weiler, astro-ph/0009378
-
Y. Uchihori et al., Astropart. Phys. 13, 151 (2000). For a recent analytic analysis, see H. Goldberg and T. J. Weiler, astro-ph/0009378.
-
(2000)
Astropart. Phys.
, vol.13
, pp. 151
-
-
Uchihori, Y.1
-
46
-
-
33750676220
-
-
H. Davoudiasl, J. L. Hewett, and T. G. Rizzo, hep-ph/0010066.
-
In considering the exchange of gravitons (KK modes), one should distinguish the following two scenarios: (i) In the ca-nonical example of [1], KK gravitons couple extremely weakly, and the observational effects arise because of the very large multiplicity of states due to their fine splittings, (ii) In the anti-de Sitter bulk scenario (see Randall-Sundrum in Ref. [3]), each exited state coupling is o(E/TeV), and thus single KK modes could be detected via their decay products. Future cosmic ray data could play an important role in testing the latter. H. Davoudiasl, J. L. Hewett, and T. G. Rizzo, hep-ph/0010066.
-
-
-
-
47
-
-
0035862248
-
-
The influence of the extra-dimensional scenario on monopole induced showers was reported elsewhere. L. A. Anchordoqui, T. P. McCauley, S. Reucroft, and J. Swain, Phys. Rev. D 63, 027303 (2001).
-
(2001)
Phys. Rev. D
, vol.63
, pp. 027303
-
-
Anchordoqui, L.A.1
McCauley, T.P.2
Reucroft, S.3
Swain, J.4
-
49
-
-
4143053149
-
-
A remarkable correlation between the arrival direction of cosmic rays above 10"° eV and high redshift compact radio quasars seems to support the neutrino hypothesis. Such a correlation, however, diminishes when considering only the highest energy events (£>8X1019 eV at 1-standard deviation) that have no contamination from the expected proton pile-up around the photopion production threshold. G. R. Farrar and P. Biermann, Phys. Rev. Lett. 81, 3579 (1998);
-
(1998)
Phys. Rev. Lett.
, vol.81
, pp. 3579
-
-
Farrar, G.R.1
Biermann, P.2
-
50
-
-
0034894228
-
-
G. Sigl et al, Phys. Rev. D 63, 081302 (2001);
-
(2001)
Phys. Rev. D
, vol.63
, pp. 081302
-
-
Sigl, G.1
-
51
-
-
33750653250
-
-
A. Virmani et al, astro-ph/0010235
-
A. Virmani et al, astro-ph/0010235.
-
-
-
-
53
-
-
0001301336
-
-
P. Jain; D. \V. McKay, S. Panda, and J. P. Ralston, Phys. Lett. B 484, 267 (2000).
-
(2000)
Phys. Lett. B
, vol.484
, pp. 267
-
-
Jain, P.1
McKay, D.V.2
Panda, S.3
Ralston, J.P.4
-
54
-
-
33750660226
-
-
G. Domokos, S. Kovesi-Domokos, and P. T. Mikulski, hep-ph/0006328
-
G. Domokos, S. Kovesi-Domokos, and P. T. Mikulski, hep-ph/0006328.
-
-
-
-
60
-
-
0000736135
-
-
R. S. Fletcher, T. K. Gaisser, P. Lipari, and T. Stanev, Phys. Rev. D 50, 5710 (1994).
-
(1994)
Phys. Rev. D
, vol.50
, pp. 5710
-
-
Fletcher, R.S.1
Gaisser, T.K.2
Lipari, P.3
Stanev, T.4
-
62
-
-
0000363112
-
-
edited by D. Kieda, M. Salamon, and B. Dingus, Salt Lake City, Utah, astro-ph/9905185
-
S. J. Sciutto, in Proceedings of the XXVI International Cosmic Ray Conference, edited by D. Kieda, M. Salamon, and B. Dingus, Salt Lake City, Utah, 1999, Vol. 1, p. 411, astro-ph/9905185.
-
(1999)
Proceedings of the XXVI International Cosmic Ray Conference
, vol.1
, pp. 411
-
-
Sciutto, S.J.1
-
63
-
-
85037916808
-
-
See in particular Fig. 8
-
L. A. Anchordoqui, M. T. Dova, L. N. Epele, and S. J. Sciutto, Phys. Rev. D 59, 094003 (1999). See in particular Fig. 8.
-
(1999)
Phys. Rev. D
, vol.59
, pp. 094003
-
-
Anchordoqui, L.A.1
Dova, M.T.2
Epele, L.N.3
Sciutto, S.J.4
-
65
-
-
0033599926
-
-
B552, 3 (1999); B551, 549 (1999). See also [16].
-
Z. Kakushadze, Nucl. Phys. B548, 205 (1999); B552, 3 (1999); B551, 549 (1999). See also [16].
-
(1999)
Nucl. Phys.
, vol.B548
, pp. 205
-
-
Kakushadze, Z.1
-
67
-
-
33750635107
-
-
A. Jain, P. Jain, D. W. McKay, and J. P. Ralston, hep-ph/0011310
-
A. Jain, P. Jain, D. W. McKay, and J. P. Ralston, hep-ph/0011310.
-
-
-
-
68
-
-
0030079586
-
-
It is worthwhile to remark that at these energies the CMB is completely opaque to the propagation of gamma rays. See, for instance, R. J. Protheroe and P. A. Johnson, Astropart. Phys. 4, 253 (1996).
-
(1996)
Astropart. Phys.
, vol.4
, pp. 253
-
-
Protheroe, R.J.1
Johnson, P.A.2
|