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Extra resources for Proceedings of the Sixth International Workshop on Relativistic Aspects of Nuclear Physics : Caraguatatuba, São Paulo, Brazil, 17-20 October 2000

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B455 (1999) 45. 24. J. Barrette et al (E877 Collaboration), Phys. Rev. C55 (1997) 1420. 25. M. A. Voloshin for the NA49 Collaboration, Nucl. Phys. A661 (1999) 341c. 26. S. Pratt, Phys. Rev. D 33, 1314 (1986); G. Bertsch, M. Gong and M. Tohyama, Phys. Rev. C 37, 1896 (1988); and G. Bertsch, Nucl. Phys. A 498, 151c (1989). 27. S. , Phys. Rev. C42 (1990) 2646. 28. D. H. Rischke, Nucl. Phys. H. Rischke and M. Gyulassy, Nucl. Phys. A608 (1996) 479. 29. M. Gyulassy and M. Pluemmer, Phys. Lett. N. Wang and M.

B444 (1998) 523. Phys. A661 (1999) 485c. 36 27. 28. 29. 30. 31. 32. , Nucl. Phys. A661 (1999) 534c. , Nucl. Phys. A498 (1989) 375c. Phys. A498 (1989) 133c. A - in print. A - in print. Lett. B - in print. Angela V. Olinto 38 The Origin of the Highest Energy Cosmic Rays A. V. edu Contrary to expectations, several cosmic ray events with energies above 10 2 0 eV have been observed. The flux of such events is well above the predicted GreisenZatsepin-Kuzmin cutoff due to the pion production (via the A resonace) of extragalactic cosmic ray protons off the cosmic microwave background.

3. M u l t i - S t r a n g e H y p e r o n s While the AGS strangeness production can be understood in terms of independent nucleon-nucleon collisions and hadronic re-interactions, this is not t h e case at the SPS [9]. T h e precise measurements of strange hyperons and their anti-particles reveal a systematic increase with respect to p + P b (A, H, fi - WA97 d a t a [30,31]) and with respect to p + p (H NA49 d a t a [25]). T h e excess is larger for particles of higher strangeness content, becoming most dramatic for fi+H (up to factor ~ 20).

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