Astroparticle physics - A personal outlook

Nuclear Physics B - Proceedings Supplements

Volumn 19, Issue 1, 1996, Pages 522-544

  Ellis, J ^a  

^a CERN   (Switzerland)

Author keywords

[No Author keywords available]

Indexed keywords

EID: 0009125084     PISSN: 09205632     EISSN: None     Source Type: Journal    
DOI: 10.1016/0920-5632(96)00306-4     Document Type: Review

References (193)

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15. 9. Relatively high values of (or upper limits on) the Deuterium abundance have recently been reported in Lyman α clouds at high redshifts: R.F. Cars-well et al., MNRAS 268 (1994) L1; A. Songaila et al., Nature 368 (1994) 599; M. Rugers and C.J. Hogan, astro-ph/9512004. However, there is also one report of a relatively low value of the Deuterium abundance: D. Tytler and X.M. Fan, Bull. AAAS 26 (1994) 1424, and the hope that these observations might yield measurements of the primordial Deuterium abundance is cast into doubt by indications that nuclear processing may be important already at these early times: E.J. Wampler et al., astro-ph/9512084.
16. 9. Relatively high values of (or upper limits on) the Deuterium abundance have recently been reported in Lyman α clouds at high redshifts: R.F. Cars-well et al., MNRAS 268 (1994) L1; A. Songaila et al., Nature 368 (1994) 599; M. Rugers and C.J. Hogan, astro-ph/9512004. However, there is also one report of a relatively low value of the Deuterium abundance: D. Tytler and X.M. Fan, Bull. AAAS 26 (1994) 1424, and the hope that these observations might yield measurements of the primordial Deuterium abundance is cast into doubt by indications that nuclear processing may be important already at these early times: E.J. Wampler et al., astro-ph/9512084.
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18. 9. Relatively high values of (or upper limits on) the Deuterium abundance have recently been reported in Lyman α clouds at high redshifts: R.F. Cars-well et al., MNRAS 268 (1994) L1; A. Songaila et al., Nature 368 (1994) 599; M. Rugers and C.J. Hogan, astro-ph/9512004. However, there is also one report of a relatively low value of the Deuterium abundance: D. Tytler and X.M. Fan, Bull. AAAS 26 (1994) 1424, and the hope that these observations might yield measurements of the primordial Deuterium abundance is cast into doubt by indications that nuclear processing may be important already at these early times: E.J. Wampler et al., astro-ph/9512084.
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20. 10. S. White, J. Navarro, A. Evard and C. Frenk, Nature 366 (1993) 429; J. Bartlett, A. Blanchard, J. Silk and M. Turner, Fermilab preprint 94/173-A (1994).
21. 11. R.W. Strickland and D.N. Schramm, astro-ph/9511111.
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28. 16. E. Masso, talk at this meeting, Barcelona preprint UAB-FT-380 (1995).
29. 17. The MACHO Collaboration has recently announced (http://wwwmacho.anu.edu.au/) additional microlensing events with longer time scales, indicating that a significant further fraction of our galactic halo may be composed of larger-mass objects: see also D. Bennett et al., astro-ph/9510104. Since such objects have not been seen in direct optical searches, they are likely to be white dwarfs or neutron stars, whose progenitors must have weighed ≃ 2 or more solar masses in order to have burnt out already: see also F.C. Adams and G. Laughlin, astro-ph/9602006. However, in this case, one would expect to see also a population of visible objects with masses between 0.1 and 2 solar masses. Even taking these new MACHO results at face value, there is still expected to be a substantial local density of non-baryonic cold dark matter particles: see, e.g., M.S. Turner, E.I. Gates and G. Gyuk, astro-ph/9601168.
30. 17. The MACHO Collaboration has recently announced (http://wwwmacho.anu.edu.au/) additional microlensing events with longer time scales, indicating that a significant further fraction of our galactic halo may be composed of larger-mass objects: see also D. Bennett et al., astro-ph/9510104. Since such objects have not been seen in direct optical searches, they are likely to be white dwarfs or neutron stars, whose progenitors must have weighed ≃ 2 or more solar masses in order to have burnt out already: see also F.C. Adams and G. Laughlin, astro-ph/9602006. However, in this case, one would expect to see also a population of visible objects with masses between 0.1 and 2 solar masses. Even taking these new MACHO results at face value, there is still expected to be a substantial local density of non-baryonic cold dark matter particles: see, e.g., M.S. Turner, E.I. Gates and G. Gyuk, astro-ph/9601168.
31. 17. The MACHO Collaboration has recently announced (http://wwwmacho.anu.edu.au/) additional microlensing events with longer time scales, indicating that a significant further fraction of our galactic halo may be composed of larger-mass objects: see also D. Bennett et al., astro-ph/9510104. Since such objects have not been seen in direct optical searches, they are likely to be white dwarfs or neutron stars, whose progenitors must have weighed ≃ 2 or more solar masses in order to have burnt out already: see also F.C. Adams and G. Laughlin, astro-ph/9602006. However, in this case, one would expect to see also a population of visible objects with masses between 0.1 and 2 solar masses. Even taking these new MACHO results at face value, there is still expected to be a substantial local density of non-baryonic cold dark matter particles: see, e.g., M.S. Turner, E.I. Gates and G. Gyuk, astro-ph/9601168.
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36. 22. See, e.g., C.J. Copi and D.N. Schramm, astro-ph/9504026; M. Bolte and C.J. Hogan, Nature 376 (1995) 399.
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38. 23. M. Rowan-Robinson, Les Houches lectures (1993) and CERN Colloquium (1995).
39. 23. M. Rowan-Robinson, Les Houches lectures (1993) and CERN Colloquium (1995).
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58. 33. G. Hinshaw et al., COBE preprint 96-04, astro-ph/9601058; E.L. Wright et al., astro-ph/9601059.
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61. 35. J. Ellis, D.V. Nanopoulos, K.A. Olive and S.-J. Key, CERN preprint TH/95-88 (1995), to be published in Astropartide Physics, and references therein.
62. 36. See, e.g., A.R. Liddle and D.H. Lyth, Phys. Rep. 231 (1993) 1; M.S. Turner and M. White, Fermilab preprint Pub-95/405-A (1995).
63. 36. See, e.g., A.R. Liddle and D.H. Lyth, Phys. Rep. 231 (1993) 1; M.S. Turner and M. White, Fermilab preprint Pub-95/405-A (1995).
64. 37. M. Tegmark, astro-ph/9601077.
65. 38. A. Kogut and S. Minshaw, astro-ph/9601179.
66. 39. M.S. Turner and N. Vittorio, talks at this meeting.
67. 40. R.K. Schaefer and Q. Shafi, Nature 359 (1992) 119; M. Davis, F.J. Summers and D. Schlegel, Nature 359 (1992) 393; A.N. Taylor and M. Rowan-Robinson, Nature 359 (1992) 396.
68. 40. R.K. Schaefer and Q. Shafi, Nature 359 (1992) 119; M. Davis, F.J. Summers and D. Schlegel, Nature 359 (1992) 393; A.N. Taylor and M. Rowan-Robinson, Nature 359 (1992) 396.
69. 40. R.K. Schaefer and Q. Shafi, Nature 359 (1992) 119; M. Davis, F.J. Summers and D. Schlegel, Nature 359 (1992) 393; A.N. Taylor and M. Rowan-Robinson, Nature 359 (1992) 396.
70. 41. J.R. Primack, J. Holtzman, A. Klypin and D. Caldwell, U.C. Santa Cruz preprint SCIPP 94/28 (1994); D. Caldwell, talk at this meeting.
71. 41. J.R. Primack, J. Holtzman, A. Klypin and D. Caldwell, U.C. Santa Cruz preprint SCIPP 94/28 (1994); D. Caldwell, talk at this meeting.
72. 42. LSND Collaboration, C. Athanassopoulos et al., Phys. Rev. Lett. 75 (1995) 2650.
73. 43. B. Fields, K. Kainulainen and K.A. Olive, CERN preprint TH/95-355 (1995) and references therein.
74. 44. J. Valle, talk at this meeting.
75. 45. T. Yanagida, Proc. Workshop on the Unified Theory and the Baryon Number in the Universe (KEK, Japan, 1979); R. Slansky, Talk at Sanibel Symposium, Caltech preprint CALT-68-709 (1979).
76. 45. T. Yanagida, Proc. Workshop on the Unified Theory and the Baryon Number in the Universe (KEK, Japan, 1979); R. Slansky, Talk at Sanibel Symposium, Caltech preprint CALT-68-709 (1979).
77. 46. B.T. Cleveland et al., Nucl. Phys. Proc. Supp. B38 (1995) 47; R. Davis, Prog. Part. Nucl. Phys. 32 (1994) 13 and talk at this meeting; Kamiokande Collaboration, Y. Suzuki, Nucl. Phys. Proc. Supp. B38 (1994) 54 and talk by Y. Totsuka at this meeting; SAGE Collaboration, J.N. Abdurashitov et al., Phys. Lett. B328 (1994) 234 and talk by V.N. Gavrin at this meeting; GALLEX Collaboration, P. Anselmann et al., Phys. Lett. B327 (1994) 377 and B342 (1995) 440 and talk by R. Bernabei at this meeting.
78. 46. B.T. Cleveland et al., Nucl. Phys. Proc. Supp. B38 (1995) 47; R. Davis, Prog. Part. Nucl. Phys. 32 (1994) 13 and talk at this meeting; Kamiokande Collaboration, Y. Suzuki, Nucl. Phys. Proc. Supp. B38 (1994) 54 and talk by Y. Totsuka at this meeting; SAGE Collaboration, J.N. Abdurashitov et al., Phys. Lett. B328 (1994) 234 and talk by V.N. Gavrin at this meeting; GALLEX Collaboration, P. Anselmann et al., Phys. Lett. B327 (1994) 377 and B342 (1995) 440 and talk by R. Bernabei at this meeting.
79. 46. B.T. Cleveland et al., Nucl. Phys. Proc. Supp. B38 (1995) 47; R. Davis, Prog. Part. Nucl. Phys. 32 (1994) 13 and talk at this meeting; Kamiokande Collaboration, Y. Suzuki, Nucl. Phys. Proc. Supp. B38 (1994) 54 and talk by Y. Totsuka at this meeting; SAGE Collaboration, J.N. Abdurashitov et al., Phys. Lett. B328 (1994) 234 and talk by V.N. Gavrin at this meeting; GALLEX Collaboration, P. Anselmann et al., Phys. Lett. B327 (1994) 377 and B342 (1995) 440 and talk by R. Bernabei at this meeting.
80. 46. B.T. Cleveland et al., Nucl. Phys. Proc. Supp. B38 (1995) 47; R. Davis, Prog. Part. Nucl. Phys. 32 (1994) 13 and talk at this meeting; Kamiokande Collaboration, Y. Suzuki, Nucl. Phys. Proc. Supp. B38 (1994) 54 and talk by Y. Totsuka at this meeting; SAGE Collaboration, J.N. Abdurashitov et al., Phys. Lett. B328 (1994) 234 and talk by V.N. Gavrin at this meeting; GALLEX Collaboration, P. Anselmann et al., Phys. Lett. B327 (1994) 377 and B342 (1995) 440 and talk by R. Bernabei at this meeting.
81. 46. B.T. Cleveland et al., Nucl. Phys. Proc. Supp. B38 (1995) 47; R. Davis, Prog. Part. Nucl. Phys. 32 (1994) 13 and talk at this meeting; Kamiokande Collaboration, Y. Suzuki, Nucl. Phys. Proc. Supp. B38 (1994) 54 and talk by Y. Totsuka at this meeting; SAGE Collaboration, J.N. Abdurashitov et al., Phys. Lett. B328 (1994) 234 and talk by V.N. Gavrin at this meeting; GALLEX Collaboration, P. Anselmann et al., Phys. Lett. B327 (1994) 377 and B342 (1995) 440 and talk by R. Bernabei at this meeting.
82. 46. B.T. Cleveland et al., Nucl. Phys. Proc. Supp. B38 (1995) 47; R. Davis, Prog. Part. Nucl. Phys. 32 (1994) 13 and talk at this meeting; Kamiokande Collaboration, Y. Suzuki, Nucl. Phys. Proc. Supp. B38 (1994) 54 and talk by Y. Totsuka at this meeting; SAGE Collaboration, J.N. Abdurashitov et al., Phys. Lett. B328 (1994) 234 and talk by V.N. Gavrin at this meeting; GALLEX Collaboration, P. Anselmann et al., Phys. Lett. B327 (1994) 377 and B342 (1995) 440 and talk by R. Bernabei at this meeting.
83. 47. J.N. Bahcall and M. Pinsonneault, Rev. Mod. Phys. 67 (1995) 1; J.N. Bahcall and P.I. Krastev, Princeton Institute for Advanced Study preprint IASSNS-AST 95/56 (1995) and references therein; J.N. Bahcall, Princeton Institute for Advanced Studies preprint IASSNS-AST 95/54 (1995) and talk at this meeting; S. Turck-Chièze, talk at this meeting.
84. 47. J.N. Bahcall and M. Pinsonneault, Rev. Mod. Phys. 67 (1995) 1; J.N. Bahcall and P.I. Krastev, Princeton Institute for Advanced Study preprint IASSNS-AST 95/56 (1995) and references therein; J.N. Bahcall, Princeton Institute for Advanced Studies preprint IASSNS-AST 95/54 (1995) and talk at this meeting; S. Turck-Chièze, talk at this meeting.
85. 47. J.N. Bahcall and M. Pinsonneault, Rev. Mod. Phys. 67 (1995) 1; J.N. Bahcall and P.I. Krastev, Princeton Institute for Advanced Study preprint IASSNS-AST 95/56 (1995) and references therein; J.N. Bahcall, Princeton Institute for Advanced Studies preprint IASSNS-AST 95/54 (1995) and talk at this meeting; S. Turck-Chièze, talk at this meeting.
86. 47. J.N. Bahcall and M. Pinsonneault, Rev. Mod. Phys. 67 (1995) 1; J.N. Bahcall and P.I. Krastev, Princeton Institute for Advanced Study preprint IASSNS-AST 95/56 (1995) and references therein; J.N. Bahcall, Princeton Institute for Advanced Studies preprint IASSNS-AST 95/54 (1995) and talk at this meeting; S. Turck-Chièze, talk at this meeting.
87. 48. See, in particular, the talks at this meeting by D.R.O. Morrison, preprint DM-95-10 (1996) and by A. Dar, astro-ph/9601109.
88. 48. See, in particular, the talks at this meeting by D.R.O. Morrison, preprint DM-95-10 (1996) and by A. Dar, astro-ph/9601109.
89. 49. V. Castellani et al., Phys. Rev. D50 (1994) 4749; N. Hata and P. Langacker, Phys. Rev. D52 (1995) 420; G. Fiorentini, talk at this meeting.
90. 49. V. Castellani et al., Phys. Rev. D50 (1994) 4749; N. Hata and P. Langacker, Phys. Rev. D52 (1995) 420; G. Fiorentini, talk at this meeting.
91. 49. V. Castellani et al., Phys. Rev. D50 (1994) 4749; N. Hata and P. Langacker, Phys. Rev. D52 (1995) 420; G. Fiorentini, talk at this meeting.
92. 50. A. Dar and G. Shaviv, astro-ph/9401043.
93. 51. J. Christensen-Dalsgaard, Nature 376 (1995) 641 and talk at this meeting.
94. 52. W. Haxton, talk at this meeting.
95. 53. Superkamiokande Collaboration, Y. Totsuka, ICCR report 227-90-20 (1990) and talk at this meeting.
96. 54. SNO Collaboration, G.T. Ewan et al., Sudbury Neutrino Observatory proposal SNO-87-12 (1987); A. McDonald, talk at this meeting.
97. 54. SNO Collaboration, G.T. Ewan et al., Sudbury Neutrino Observatory proposal SNO-87-12 (1987); A. McDonald, talk at this meeting.
98. 55. BOREXINO Collaboration, C. Arpesella et al., BOREXINO proposal (Univerity of Milano, Milano, 1992).
99. 56. HELLAZ Collaboration, G. Laurenti et al., Proc. Fifth Int. Workshop on Neutrino Telescopes, Venice 1993, ed. M. Baldo Ceolin (University of Padova, Padova, 1994) 161.
100. 57. HERON Collaboration, S.R. Bandler et al., J. Low Temp. Phys. 93 (1993) 785.
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102. 59. CHORUS Collaboration, M. de Jong et al., CERN preprints PPE/90-42 (1990) and 93-13 (1993).
103. 60. NOMAD Collaboration, L. Di Lella, Nucl. Phys. Proc. Supp. B31 (1993) 319.
104. 61. COSMOS Collaboration, P803 proposal to Fermilab (1993).
105. 62. J.J. Gomez-Cadenas, J.A. Hernando and A. Bueno, CERN preprint PPE/95-177 (1995).
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109. 66. F. Cavanna, CERN preprint PPE/95-133 (1995);
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119. 73. P. Renton, to appear in Proceedings of the Beijing International Symposium on Lepton and Photon Interaction, Oxford Preprint OUNP-95-20 (1995), and LEP Electroweak Working Group, P. Antilogus et al., CERN preprint PPE/95-172 (1995).
120. 73. P. Renton, to appear in Proceedings of the Beijing International Symposium on Lepton and Photon Interaction, Oxford Preprint OUNP-95-20 (1995), and LEP Electroweak Working Group, P. Antilogus et al., CERN preprint PPE/95-172 (1995).
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