| Item | Title | Authors | Source | Publ. Yr. | Abstract | Preprint#/Link |
| 1 | A model of the primary cosmic ray spectra | Adams-JH-Jr; Lee-J | Radiation-Measurements. vol.26, no.3; May 1996; p.467-70 | 1996 | The authors have collected published experimental measurements of the Galactic cosmic ray spectra of the primary elements, H, He, C, O, Ne, Mg, Si and Fe in the energy range from 45 MeV/nucleon to 1 TeV/nucleon in the years 1963-1987. They have fit these data with a solution to the spherically symmetric diffusion equation using boundary spectra which are a solution of the cosmic ray propagation equation in the leaky-box model. In the present work, they show how the energy spectra of these elements at 1 AU are represented by this model. | |
| 2 | A NEW EXPERIMENTAL SETUP TO STUDY UHE COSMIC RAY BASED ON MEASUREMENT OF ARRIVAL TIME SPREAD OF SECONDARY PARTICLES FROM EAS | T. Bezboruah, K. Boruah, P.K. Boruah (Gauhati U.) | Nucl. Instrum. Meth. A410, 206-212 (1998) | 1998 | ?? | |
| 3 | A new technique for the observation of EeV and ZeV cosmic rays | Kieda-DB | Astroparticle-Physics. vol.4, no.2; Dec. 1995; p.133-50 | 1995 | Describes a new technique for the detection of EeV (10/sup 18/ eV) and ZeV (10/sup 21/ eV) cosmic rays in the atmosphere. The technique uses the fact that the Cerenkov light emitted by atmospheric extensive showers generated by primaries in this energy range is brighter than the fluctuations in the ambient light of the night sky, even with a full Moon present. The Cerenkov light is also brighter than fluctuations in the twilight sky, and can even be of similar size as fluctuations in direct sunlight. For the highest energy cosmic rays (E>1 ZeV), this may allow optical detection with on-time efficiency limited only by the weather. The energy, angular, and X/sub max/ resolution of the technique is examined as a function of the background day and night sky conditions. Using a "shadowing" method for determining the direction of the original cosmic ray primary, angular resolution between 0.3 degrees to approximately=3 degrees is possible, depending upon the zenith angle and energy of the primary, and the amou | |
| 4 | About the most energetic cosmic rays | Cocconi-G | Astroparticle-Physics. vol.4, no.3; Feb. 1996; p.281-3 | 1996 | Consequences of the observed anisotropy of energetic cosmic rays are discussed. The author considers arrival directions, energies, origins, high energy proton propagation. | |
| 5 | Acceleration and Interaction of Ultra High Energy Cosmic Rays | R.J. Protheroe | Chapter in "Topics in cosmic-ray astrophysics" | 1998 | astro-ph/9812055 | |
| 6 | Acceleration of UHE Cosmic Ray Particles at Relativistic Jets in Extragalactic Radio Sources | M. Ostrowski (Jagellonian U.) | Submitted to Astron.Astrophys | 1998 | astro-ph/9803299 | |
| 7 | Angle-Time-Energy Images of Ultra-High Energy Cosmic Ray Sources | Guenter Sigl (Univ. of Chicago) | To appear in Proceedings of the Workshop on "Observing Giant Cosmic Ray Air Showers for > 10**(20) eV Particles from Space", Univ. of Maryland, Nov 13-15, 1997. | 1997 | astro-ph/9712144 | |
| 8 | Anisotropy of Ultra High Energy Cosmic Rays in the Dark Matter Halo Model | V.Berezinsky, A.Mikhailov | Phys.Lett. B449 (1999) 237-239 | 1998 | astro-ph/9810277 | |
| 9 | Arrival directions of the most energetic cosmic rays | Stanev-T; Biermann-PL; Lloyd-Evans-J; Rachen-JP; Watson-AA | Physical-Review-Letters. vol.75, no.17; 23 Oct. 1995; p.3056-9 | 1995 | Examines the arrival directions of the most energetic cosmic rays (E>2*10/sup 19/ eV) detected by several air shower experiments. The authors find that data taken by different air shower arrays show positive correlations, indicating a nonuniform arrival direction distribution. The authors also find that the events with energy >4*10/sup 19/ eV exhibit a correlation with the general direction of the supergalactic plane, where a large number of potential sources are located. If confirmed by data from other experiments the results would support models for the extragalactic origin of the highest energy cosmic rays. | |
| 10 | Arrival directions of the southern highest energy cosmic rays | Kewley-LJ; Clay-RW; Dawson-BR | Astroparticle-Physics. vol.5, no.1; June 1996; p.69-74 | 1996 | The authors have examined the arrival directions of the highest energy cosmic rays recorded by the southern hemisphere SUGAR air shower array to determine whether there exists in the south a preference for directions along the supergalactic plane as suggested by northern data. The authors have not found such an effect. | |
| 11 | Can Ultra High Energy Cosmic Rays be Evidence for New Particle Physics? | Glennys R. Farrar | Invited talk at the Workshop on "Observing the Highest Energy Particles (> 10^{20} eV) from Space", College Park, MD, Nov. 13-15 1997 | 1998 | astro-ph/9801020 | |
| 12 | Correlation between Compact Radio Quasars and Ultra-High Energy Cosmic Rays | Glennys R. Farrar (Rutgers Univ.), Peter L. Biermann (Max Planck Institute for Radio Astronomy, Bonn) | Phys.Rev.Lett. 81 (1998) 3579-3582 | 1998 | astro-ph/9806242 | |
| 13 | Cosmic ray astrophysics (history and general review) | Ginzburg-VI | Physics-Uspekhi. vol.39, no.2; Feb. 1996; p.155-68. Translated from: Uspekhi-Fizicheskii-Nauk. vol.166, no.2; Feb. 1996; p.169-83 | 1996 | The history of the discovery and investigation of cosmic rays prior to the advent of the cosmic ray astrophysics is presented. Some data about cosmic rays near the Earth and in the Universe are given. The main part of cosmic rays observed near the Earth is generated in our Galaxy by supernova explosions. The most important problem yet to be solved in cosmic ray astrophysics is the origin of cosmic rays of superhigh energy. | |
| 14 | Cosmic rays from primordial black holes and constraints on the early universe | Carr-BJ; MacGibbon-JH | Physics-Reports. vol.307, no.1-4; Dec. 1998; p.141-54 | 1998 | The constraints on the number of evaporating primordial black holes imposed by observations of the cosmological gamma-ray background do not exclude their making a significant contribution to the Galactic flux of cosmic ray photons, electrons, positrons and antiprotons. Even if this contribution is small, cosmic ray data place important limits on the number of evaporating black holes and thereby on models of the early Universe. Evaporating black holes are unlikely to be detectable in their final explosive phase unless new physics is invoked at the QCD phase transition. | |
| 15 | Cosmic rays: the most energetic particles in the universe | Cronin-JW | Reviews-of-Modern-Physics. vol.71, no.2; Feb. 1999; p.S165-72 | 1999 | Cosmic rays are an ever present aspect of nature. The birth of the field of elementary-particle physics can be traced to studies of cosmic rays. Now advances in technology and new instrumentation are changing the nature of cosmic-ray research. New forms of astronomy are being created. Ground-based instruments, spawned by cosmic-ray techniques, permit the observation of astrophysical objects emitting radiation in very-high-energy gamma rays, (>or=100 GeV), high-energy neutrinos (>or=1 TeV), and the most energetic particles found in the cosmic radiation (>or=5*10/sup 19/ eV). At these energies the galactic and intergalactic magnetic fields deflect the cosmic-ray protons by only a few degrees. The interaction of these cosmic rays with the cosmic background radiation limits the possible sources to redshifts far less than unity. The origin of these highest-energy cosmic rays is not understood. The present status of knowledge of these cosmic rays and the prospects for solving the mystery concerning their origin are | |
| 16 | Cosmic Strings - Dead Again? | Mark Hindmarsh (Sussex) | talk given at Cosmo 97, Ambleside, England, Sept 97 | 1998 | hep-ph/9806469 | |
| 17 | Cosmological origin for cosmic rays above 10/sup 19/ eV | Waxman-E | Astrophysical-Journal,-Letters. vol.452, no.1, pt.2; 10 Oct. 1995; p.L1-4 | 1995 | The cosmic-ray spectrum at 10/sup 19/-10/sup 20/ eV, reported by the Fly's Eye and the AGASA experiments, is shown to be consistent with a cosmological distribution of sources of protons, with a power-law generation spectrum dlnN/dlnE=-2.3+or-0.5 and energy production rate of 4.5+or-1.5*10/sup 44/ ergs Mpc/sup -3/ yr/sup -1/. The two events measured above 10/sup 20/ eV are not inconsistent with this model. Verifying the existence of a "blackbody cutoff", observed with low significance, would require approximately 30 observation years with existing experiments, but only approximately 1 year with the proposed approximately 5000 km/sup 2/ detectors. For a cosmological source distribution, no anisotropy is expected in the angular distribution of events with energies up to approximately 5*10/sup 19/ eV. | |
| 18 | Cryptons: a stringy form of decaying superheavy dark matter, as a source of the ultra high energy cosmic rays | D.V. Nanopoulos | Talk given at the R. Arnowitt Fest: A Symposium on Supersymmetry and Gravitation, College Station, TX 5-7 April 1998. | 1998 | hep-ph/9809546 | |
| 19 | Dark matter halos and the anisotropy of ultra-high energy cosmic rays | Gustavo Medina Tanco (Inst.Astron.e Geof.-USP-Brasil), Alan A. Watson (Univ.of Leeds-UK) | Astroparticle Physics (accepted for publication) | 1999 | astro-ph/9903182 | |
| 20 | Deflection of ultra high energy cosmic rays by the galactic magnetic field: from the sources to the detector | Gustavo A. Medina Tanco (IAG/RGO), Elisabete M. de Gouveia Dal Pino (IAG), Jorge E. Horvath (IAG) | ?? | 1997 | astro-ph/9707041 | |
| 21 | Differences between gamma-ray and hadronic showers | Hillas-AM | Space-Science-Reviews. vol.75, no.1-2; Jan. 1996; p.17-30 | 1996 | Cosmic gamma-ray sources may be sought if high-energy gamma-rays may be detected without confusion from the very intense isotropic background of hadronic cosmic rays. Ground-based methods are needed at energies above tens of GeV, using air showers, and at energies below tens of TeV, the detection of muons in showers is not the most efficient way to reject hadronic showers. The shape and orientation of Cerenkov images can reject far more than 99% of the background. The way in which Cerenkov radiation is distributed in showers is discussed, and the possibilities of using image shape, distribution of light on the ground, time profile, spectrum and polarization of the light are briefly discussed. Imaging alone appears to be the most powerful. Simulations suggest that the UV content of the light should not be a useful diagnostic. | |
| 22 | Exotic massive hadrons and ultra-high energy cosmic rays | Ivone F.M.Albuquerque, Glennys R.Farrar, Edward W.Kolb | Phys.Rev. D59 (1999) 015021 | 1998 | hep-ph/9805288 | |
| 23 | Galactic Anisotropy as Signature of ``Top-Down'' Mechanisms of Ultra-High Energy Cosmic Rays | S. L. Dubovsky, P. G. Tinyakov | JETP Lett. 68 (1998) 107-111 | 1998 | hep-ph/9802382 | |
| 24 | Gamma-ray bursters as sources of cosmic rays | Milgrom-M; Usov-V | Astroparticle-Physics. vol.4, no.4; April 1996; p.365-9 | 1996 | From the little that is know of the physical conditions in gamma -ray bursters, it seems that they are potentially effective in the acceleration of high-energy cosmic rays (CRs), especially if the bursters are at cosmological distances. The authors find that, with the observed statistics and fluxes of gamma -ray bursts, cosmological bursters may be an important source of cosmic rays in two regions of the observed spectrum: (1) At the very-high-energy end (E>10/sup 19/ eV), where CRs must be of extragalactic origin. (2) Around and above the spectral feature that has been described as a bump and/or a knee, which occurs around 10/sup 15/ eV. The occasional bursters that occur inside the Galaxy-about once in a few hundred thousand years if burst emission is isotropic; more often, if it is beamed-could maintain the density of galactic cosmic rays at the observed level in this range. These two energy ranges might correspond to two typical CR energy scales characteristic of bursters: one pertinent to CR acceler | |
| 25 | Gamma-Ray Bursts, Ultra High Energy Cosmic Rays, and Cosmic Gamma-Ray Background | Tomonori Totani | Accepted by Astroparticle Physics | 1998 | astro-ph/9810207 | |
| 26 | GeV Photons from Ultra High Energy Cosmic Rays accelerated in Gamma Ray Bursts | Mario Vietri | Phys.Rev.Lett. 78 (1997) 4328-4331 | 1997 | astro-ph/9705061 | |
| 27 | Highlights on very and ultra high energy cosmic ray physics | Battistoni-G | Nuclear-Physics-B,-Proceedings-Supplements. vol.48; May 1996; p.434-40 | 1996 | A short selection out of the most interesting problems in high energy cosmic ray physics is presented, together with some recent experimental results. | |
| 28 | Limits on models of the ultrahigh energy cosmic rays based on topological defects | Protheroe-RJ; Stanev-T | Physical-Review-Letters. vol.77, no.18; 28 Oct. 1996; p.3708-11 | 1996 | Using the propagation of ultrahigh energy nucleons, photons, and electrons in the universal radiation backgrounds, the authors obtain limits on the luminosity of topological defect scenarios for the origin of the highest energy cosmic rays. The limits are set as a function of the mass of the X particles emitted by the cosmic strings or other defects, the cosmological evolution of the topological defects, and the strength of the extragalactic magnetic fields. The existing data on the cosmic ray spectrum and on the isotropic 100 MeV gamma-ray background limit significantly the parameter space in which topological defects can generate the flux of the highest energy cosmic rays, and rule out models with the standard X-particle mass of 10/sup 16/ GeV and higher. | |
| 29 | Magnetic monopoles as the highest energy cosmic ray primaries | Kephart-TW; Weiler-TJ | Astroparticle-Physics. vol.4, no.3; Feb. 1996; p.271-9 | 1996 | The authors suggest that the highest energy >or approximately=10/sup 20/ eV cosmic ray primaries may be relativistic magnetic monopoles. Motivations for this hypothesis are that conventional primaries are problematic, while monopoles are naturally accelerated to E~10/sup 20/ eV by Galactic magnetic fields. By matching the cosmic monopole production mechanism to the observed highest energy cosmic ray flux the authors estimate the monopole mass to be <or approximately=10/sup 10/ GeV. | |
| 30 | Magnetized local supercluster and the origin of the highest energy cosmic rays | Blasi-P; Olinto-AV | Physical-Review-D. vol.59, no.2; 15 Jan. 1999; p.023001/1-7 | 1999 | A sufficiently magnetized local supercluster can explain the spectrum and angular distribution of ultrahigh energy cosmic rays. We show that the spectrum of extragalactic cosmic rays with energies below ~10/sup 20/ eV may be due to the diffusive propagation in the local supercluster with fields of ~10/sup -8/-10/sup -7/ G. Above ~10/sup 20/ eV, cosmic rays propagate in an almost rectilinear way which is evidenced by the change in shape of the spectrum at the highest energies. The fit to the spectrum requires that at least one source be located relatively nearby at ~10-15 Mpc away from the Milky Way. We discuss the origin of magnetic fields in the local supercluster and the observable predictions of this model. | |
| 31 | Maximum Likelihood Analysis of Clusters of Ultra-High Energy Cosmic Rays | Guenter Sigl, Martin Lemoine, Angela V. Olinto (Univ. of Chicago) | Phys.Rev. D56 (1997) 4470-4479 | 1997 | astro-ph/9704204 | |
| 32 | Measuring the UHE cosmic-ray composition with tracking detectors in air shower arrays | Bernlohr-K | Astroparticle-Physics. vol.5, no.2; Aug. 1996; p.139-46 | 1996 | Measuring the angles of muons and electrons in air showers is proposed as a method for studying the primary cosmic-ray mass composition near the knee of the cosmic-ray energy spectrum at a few 10/sup 15/ eV. Conventional tracking detectors at existing air shower arrays could serve this purpose, like the CRT detectors at the HEGRA array. When the average radial muon angles are examined as a function of shower core distance, the experimental resolution can be very well calibrated from the tangential angle distribution. The method is particularly promising for measuring changes in the average mass number of the primary cosmic rays with energy. The method is described and experimental and theoretical constraints are discussed. | astro-ph/9605177 |
| 33 | Non-Diffusive Propagation of Ultra High Energy Cosmic Rays | Gustavo A. Medina Tanco, Elisabete M. de Gouveia Dal Pino, Jorge E. Horvath | Astropart.Phys. 6 (1997) 337-342 | 1997 | astro-ph/9610172 | |
| 34 | On the acceleration of Ultra High Energy Cosmic Rays in Gamma Ray Bursts | Mario Vietri (Osservatorio Astronomico di Roma) | Astrophys.J. 453 (1995) 883-889 | 1995 | astro-ph/9506081 | |
| 35 | On the injection energy distribution of ultra-high-energy cosmic rays | Geddes-J; Quinn-TC; Wald-RM | Astrophysical-Journal. vol.459, no.1, pt.1; 1 March 1996; p.384-92 | 1996 | Investigates the injection spectrum of ultra-high-energy (>10/sup 15/ eV) cosmic rays under the hypotheses that (1) these cosmic rays are protons and (2) the sources of these cosmic rays are extragalactic and are distributed homogeneously in space, although they may have had a different strength in the past; furthermore, the authors assume that no individual sources are unusually close. The most puzzling aspect of the observed ultra-high-energy cosmic-ray spectrum is the apparent nonexistence of a "Greisen cutoff" at about 10/sup 19.8/ eV. Such a cutoff would be expected owing to rapid energy loss from photopion production caused by interactions with the microwave background. The authors show that this fact could be explained naturally if most (or all) of the cosmic rays presently observed above about 10/sup 19.6/ eV were initially injected with energy above the Greisen cutoff. However, the authors find that the injection of cosmic rays above the Greisen cutoff cannot account for the observed flux below | |
| 36 | On the problem of determining the mass composition of cosmic rays derived from air shower measurements | Erlykin-AD; Wolfendale-AW | Astroparticle-Physics. vol.9, no.3; Oct. 1998; p.213-20 | 1998 | An analysis is made of a variety of cosmic ray data from the standpoint of making a "best estimate" of the mean logarithm of the primary cosmic ray mass (<ln A>) in the energy range 10/sup 5/-10/sup 8/ GeV. Reassuringly, the values of <ln A> join on well to the results of direct measurements at lower energies. There is also some modest support for our hypothesis of there having been a local, recent supernova. A by-product is the identification from five contenders of the best model of nuclear interactions of high energy (~10/sup 6/ GeV), although much remains to be done in this area. | |
| 37 | Origin and Propagation of Ultra-High Energy Cosmic Rays | Gustavo A. Medina Tanco, Elisabete M. de Gouveia Dal Pino, Jorge E. Horvatth (Instituto Astronomico e Geofisico, University of Sao Paulo - IAG-USP) | Paper presented at the 1998 International Conference on Plasma Physics | 1999 | astro-ph/9901053 | |
| 38 | Possible clustering of the most energetic cosmic rays within a limited space angle observed by the Akeno Giant Air Shower Array | Hayashida-N; Honda-K; Honda-M; Inoue-N; Kadota-K; Kakimoto-F; Kamata-K; Kawaguchi-S; Kawasumi-N; Matsubara-Y; Murakami-K; Nagano-M; Ohoka-LH; Sakaki-N; Souma-N; Takeda-M; Teshima-M; Tsushima-I; Uchihori-Y; Yoshida-S; Yoshii-H | Physical-Review-Letters. vol.77, no.6; 5 Aug. 1996; p.1000-3 | 1996 | Accumulated data of the Akeno Giant Air Shower Array (AGASA) indicate that arrival directions of a significant fraction of extremely high energy cosmic rays (EHECR) are uniformly distributed over the observable sky. However, three pairs of showers with angular separation of less than 2.5 degrees within the pair are observed among the 36 events above 40 EeV (4*10/sup 19/ eV), corresponding to a chance probability of 2.9% from uniform distribution. It should be noted that two pairs of them are observed to be within 2.0 degrees of the supergalactic plane. | |
| 39 | Possible sources of ultrahigh-energy cosmic protons | Uryson-AV | JETP-Letters. vol.64, no.2; 25 July 1996; p.77-81.Translated from: Pis'ma-v-Zhurnal-Eksperimental'noi-i-Teoreticheskoi-Fiziki. vol.64, no.2; 25 July 1996; p.71-5 | 1996 | The arrival directions of showers with energies above 3.2*10/sup 19/ eV, recorded by the Akeno and AGASA detectors, are analyzed. Their distributions over the celestial sphere are compared with the distributions of possible sources of protons of such high energies. An analysis using three standard deviations of uncertainty in the determination of the arrival directions of the showers shows that the sources of the protons initiating the showers are nuclei of active galaxies with red shifts z<or=0.0092, i.e. their distance from us does not exceed 40 Mpc, assuming the Hubble constant is H=75 km/s.Mpc. | |
| 40 | Predictions of the Gamma-Ray Burst Model of Ultra High Energy Cosmic Rays | Eli Waxman (IAS, Princeton) | Invited talk, to appear in Proc. ICRR Symposium on Extremely High Energy Cosmic Rays, ed. M. Nagano, Tokyo 1996 | 1996 | astro-ph/9612061 | |
| 41 | Propagation of UHE cosmic rays in a structured universe | Jorg P. Rachen | Contributed Paper to the 18th Texas Symposium on Rel. Astrophysics and Cosmology, Chicago 1996 | 1997 | astro-ph/9702046 | |
| 42 | Propagation of Ultra High Energy Protons over Cosmological Distances and Implications for Topological Defect Models | R. J. Protheroe, P. A. Johnson | Astropart.Phys. 4 (1996) 253 | 1996 | astro-ph/9506119 | |
| 43 | Recent results from the CASA-MIA experiment | Matthews-J | AIP-Conference-Proceedings. no.338; 1995; p.823-7 | 1995 | Results from the CASA-MIA cosmic ray experiment are presented. The author discusses the apparatus and its performance, including new results on the identification of the shadows of the Sun and Moon used to determine the angular resolution. Limits on the emission of 100 TeV gamma -rays from the Crab Nebula are well below extrapolations from TeV observations. A search for diffuse gamma -rays from the Galactic plane give limits approaching some recent predictions. | |
| 44 | Reconstruction of Source and Cosmic Magnetic Field Characteristics from Clusters of Ultra-High Energy Cosmic Rays | Guenter Sigl (Univ. of Chicago, USA), Martin Lemoine (Univ. of Chicago, USA/DARC, CNRS, France) | Astropart.Phys. 9 (1998) 65-78 | 1998 | astro-ph/9711060 | |
| 45 | Results from the Fly's Eye experiment | Bird-DJ; Corbato-SC; Dai-HY; Dawson-BR; Elber-JW; Gaisser-TK; Green-KD; Huang-MA; Kieda-DB; Ko-S; Larsen-CG; Loh-EC; Luo-M; Salamon-MH; Smith-JD; Sokolsky-P; Sommers-P; Stanev-T; Tang-JKK; Thomas-SB; Tilav-S | AIP-Conference-Proceedings. no.338; 1995; p.839-54 | 1995 | We report recently analyzed results on the energy spectrum, and composition of cosmic rays above 0.3 EeV. We observe a break in the spectrum at 3 EeV and a changing composition. The results can be explained by a simple two component model: galactic cosmic rays dominated by heavy primaries and an extragalactic component dominated by light primaries. The observed isotropic arrival direction distribution is consistent with the predictions of this model. A 320 EeV event was also recorded. | |
| 46 | Signatures of the origin of high-energy cosmic rays in cosmological gamma-ray bursts | Miralda-Escude-J; Waxman-E | Astrophysical-Journal,-Letters. vol.462, no.2, pt.2; 10 May 1996; p.L59-62 | 1996 | We derive observational consequences for the hypothesis that cosmic rays (CRs) of energy greater than 10/sup 19/ eV originate in the same cosmological objects producing gamma-ray bursts (GRBs). Intergalactic magnetic fields >or approximately=10/sup -12/ G are required in this model to allow CRs to be observed continuously in time by producing energy-dependent delays in the CR arrival times. This results in individual CR sources having very narrow observed spectra, since at any given time only those CRs having a fixed time delay are observed. Thus, the brightest CR sources should be different at different energies. The average number of sources contributing to the total CR flux decreases with energy much more rapidly than in a model of steady CR sources, dropping to one at E/sub crit/ approximately=2*10/sup 20/ eV with very weak sensitivity to the intergalactic magnetic field strength. Below E/sub crit/, a very large number of sources is expected, consistent with observations. Above E/sub crit/, a source may b | |
| 47 | Some prospects of future ultra-high energy cosmic ray experiments | Sigl-G | Nuclear-Physics-B,-Proceedings-Supplements. vol.70; Jan. 1999; p.503-5 | 1999 | We discuss the prospects of next generation ultra-high energy cosmic ray detectors to gain information both on the sources and on large-scale magnetic fields from the distribution in arrival times, directions, and energies of charged ultra-high energy cosmic rays from discrete sources. | |
| 48 | Strongly interacting neutrinos and the highest energy cosmic rays | Domokos-G; Kovesi-Domokos-S | Physical-Review-Letters. vol.82, no.7; 15 Feb. 1999; p.1366-9 | 1999 | Cosmic rays of energies larger than the Greisen-Zatsepin-Kuzmin cutoff may be neutrinos if they acquire strong interactions due to a "precocious unification" of forces. A scenario for this to happen is outlined. There is no contradiction with precision measurements carried out at LEP and SLAC. Observable consequences at LHC and future neutrino detectors are discussed. | |
| 49 | TeV Burst of Gamma-Ray Bursts and Ultra High Energy Cosmic Rays | Tomonori Totani | to appear in ApJ Lett. | 1998 | astro-ph/9810206 | |
| 50 | The angular deviation of ultra high energy cosmic rays in intergalactic magnetic fields | Clay-RW; Cook-S; Dawson-BR; Smith-AGK; Lampard-SR | Astroparticle-Physics. vol.9, no.3; Oct. 1998; p.221-5 | 1998 | The angular deviation associated with the propagation of ultra high energy cosmic ray protons through turbulent intergalactic magnetic fields is examined including the effect of interactions with the cosmic microwave background. It is found that the deviation of the particles is consistent with diffusion ideas but the magnitude of the deviation is appreciably less than suggested by simple models for a given mean field strength and observational energy. | |
| 51 | The anisotropy of EHE cosmic rays | Lee-AA; Clay-RW | Journal-of-Physics-G-(Nuclear-and-Particle-Physics). vol.21, no.12; Dec. 1995; p.1743-57 | 1995 | The effects of magnetic field turbulence on the anisotropy of galactic cosmic rays of the highest energies are investigated. It is found that, if the cosmic ray flux at energies above 1 EeV is made up predominantly of galactic protons, neither the observed galactic magnetic field turbulence nor possible halo turbulence are sufficient for both the computed anisotropy and galactic flux gradient to agree with observation. The implication is that the origin of these cosmic rays is not within our galaxy. | |
| 52 | The cosmic ray energy spectrum above 3*10/sup 18/ eV measured by the Akeno Giant Air Shower Array | Yoshida-S; Hayashida-N; Honda-K; Imaizumi-S; Inoue-N; Kadota-K; Kakimoto-F; Kamata-K; Kawaguchi-S; Kawasumi-N; Matsubara-Y; Murakami-K; Nagano-M; Ohoka-H; Teshima-M; Tsushima-L; Yoshii-H; Honda-M | Astroparticle-Physics. vol.3, no.2; March 1995; p.105-23 | 1995 | Reports the first result on the cosmic ray energy spectrum above 3*10/sup 18/ eV measured by the Akeno Giant Air Shower Array (AGASA) from July 1990 to February 1994. The analysis method and the energy resolution of the AGASA experiment are described in some detail. The flattening of the spectrum around 10/sup 19/ eV (ankle) is observed with a significance of 2.9 sigma . If the authors express the differential energy spectrum of cosmic rays of energy E (in eV) with an ankle energy E/sub a/ as J(E)= kappa (E/E/sub a/)/sup - gamma / m/sup -2/ s/sup -1/ sr/sup -1/ eV/sup -1/, gamma for 10/sup 18.5/ eV<or=E<or=E/sub a/ is in good agreement with that from the previous experiment and is 3.2+or-.1. The slope gamma above E/sub a/ depends strongly on the value E/sub a/. For the case E/sub a/=10/sup 19/ eV, kappa =(/sub -0.2//sup +0.1/)*10/sup -33/ and gamma =2.3/sub -0.3//sup +0.5/ for 10/sup 19/ eV<or=E<or=10/sup 20/ eV. If E/sub a/=10/sup 18.8/ eV, then kappa =(1.0+or-0.1)*10/sup -32/ and gamma =2.7/sub -0.4//s | |
| 53 | The energy spectrum observed by the AGASA experiment and the spatial distribution of the sources of ultra-high energy cosmic rays | Gustavo Medina Tanco (Inst.Astron.e Geof.-USP-Brasil & Univ.of Leeds-UK) | Astrophys. J. Letters (submitted) | 1998 | astro-ph/9810366 | |
| 54 | The highest energy cosmic ray | Halzen-F; Vazquez-RA; Stanev-T; Vankov-HP | Astroparticle-Physics. vol.3, no.2; March 1995; p.151-6 | 1995 | One should keep in mind that the highest energy cosmic rays may be photons or neutrinos. The authors discuss the particle assignment of the 3*10/sup 20/ eV shower recently observed by the Fly's Eye detector. They show that the event is not initiated by a photon and that the assignments of a proton and neutrino as the primary particle are, arguably, equally valid. Neither assignment is totally satisfactory. | |
| 55 | The origin of cosmic rays | Biermann-PL | Space-Science-Reviews. vol.74, no.3-4; Nov. 1995; p.385-96 | 1995 | Describes progress in our understanding of the origin of cosmic rays. The authors propose that cosmic rays originate mainly in three sites, (a) normal supernova explosions into the interstellar medium, (b) supernova explosions into stellar winds, and (c) hot spots of powerful radio galaxies. The proposal depends on an assumption about the scaling of the turbulent diffusive transport in cosmic ray mediated shock regions; the proposal also uses a specific model for the interstellar transport of cosmic rays. The model has been investigated in some detail and compared to (i) the radio data of OB stars, Wolf-Rayet stars, radio supernovae, radio supernova remnants, Gamma-ray line and continuum emission from starforming regions, and the cosmic ray electron spectrum, (ii) the Akeno air shower data over the particle energy range from 10 TeV to EeV, and (iii) the Akeno and Fly`s Eye air shower data from 0.1 EeV to above 100 EeV. | |
| 56 | The origin of cosmic rays above 10/sup 18.5/ eV | Norman-CA; Melrose-DB; Achterberg-A | Astrophysical-Journal. vol.454, no.1, pt.1; 20 Nov. 1995; p.60-8 | 1995 | Discusses the origin of ultra-high-energy cosmic rays (UHECRs) in the energy range above 10/sup 18.5/ eV where it is indicated that the spectrum becomes protonic and extends smoothly up to at least 10/sup 19.5/ eV and is consistent with a smooth extension to 10/sup 20.5/ eV. The acceleration of the 10/sup 19.5/ eV component must occur within ~1 Gpc. The authors rule out the production and escape of protons and neutrons from active galactic nuclei. Composition arguments make unlikely any origin in metal-rich environments such as rich clusters and the inner regions of galaxies. The authors dismiss the canonical extended halo models since such halos are almost never observed although diffuse halos have been seen in QSO absorption-line studies of metallic absorption lines. Large-scale shocks from explosions and winds are analyzed including those originating both recently and at earlier cosmological epochs. Large-scale shocks can work well only if they occur in microgauss fields. Hot spots and cocoons of radi | |
| 57 | The origin of high energy cosmic rays and the large scale structure of the Universe | Biermann-PL | Astrophysics-Reports. no.1; Jan. 1995; p.11-21 | 1995 | A recent theoretical proposal for the origin of cosmic rays gives quantitative predictions, which can be tested with data. Specifically, it has been suggested, that all cosmic rays can be attributed to just three source sites: 1) supernova explosions into the interstellar medium, 2) supernova explosions into a stellar wind, and 3) powerful radiogalaxies. The cosmic rays from any extragalactic source suffer from interaction with the microwave background, leading to the Greisen-Zatsepin-Kuzmin cutoff. The author discusses here possible sources, and specifically asks whether powerful radiogalaxies are suitable candidates. | |
| 58 | The Pierre Auger Project | Mantsch-PM | AIP-Conference-Proceedings. no.359; 1996; p.370-82 | 1996 | The Pierre Auger project is a broadly based international effort to make a detailed study of cosmic rays at the highest energies. Two air shower detectors are proposed, one to be placed in the Northern Hemisphere and one in the Southern Hemisphere. Each installation will consist of an array of 1600 particle detectors spread over 3000 km/sup 2/ with a solid angle acceptance of 2 sr for cosmic ray air showers. Each installation will also have an atmospheric fluorescence detector viewing the volume above the surface array. These two air shower detector techniques working together form a powerful instrument for the proposed research. The objectives of the Pierre Auger project are to measure the arrival direction, energy, and mass composition of 60 events per year above an energy of 10/sup 20/ eV and 6000 events per year above 10/sup 19/ eV. A collaboration is now being formed with the goal of having the Pierre Auger observatory in operation by 2001. | |
| 59 | Topological Defect Models of Ultra-High Energy Cosmic Rays | Guenter Sigl (Univ. of Chicago) | to appear in proceedings of the "International School of Cosmic-Ray Astrophysics", Erice, 16-23 June 1996 (World Scientific) | 1996 | astro-ph/9611190 | |
| 60 | Ultra high energy cosmic rays | Berezinsky-V | Nuclear-Physics-B,-Proceedings-Supplements. vol.70; Jan. 1999; p.419-30 | 1999 | The current status of ultra high energy cosmic rays (UHECR) is reviewed, with emphasis given to theoretical interpretation of the observed events. The Galactic and extragalactic origin, in case of astrophysical sources of UHE particles, have the problems either with acceleration to the observed energies or with the fluxes and spectra. Topological defects can naturally produce particles with energies as observed and much higher, but in most cases fail to produce the observed fluxes. Cosmic necklaces and monopole-antimonopole pairs are identified as most plausible sources, which can provide the observed flux and spectrum. The relic superheavy particles are shown to be clustering in the Galactic halo, producing UHECR without Greisen-Zatsepin-Kuz'min cutoff. The lightest supersymmetric particles are discussed as UHE carriers in the Universe. | hep-ph/9802351 |
| 61 | Ultra high energy cosmic rays and the large scale structure of the galactic magnetic field | Todor Stanev | submitted to The Astrophysical Journal | 1996 | astro-ph/9607086 | |
| 62 | Ultra high energy cosmic rays from cosmological relics | V.Berezinsky | Invited talk at 10th Int. Symposium on Very High Energy Cosmic Ray Interactions, July 12 - 17, 1998, Gran Sasso | 1998 | astro-ph/9811268 | |
| 63 | Ultra High Energy Cosmic Rays from Decaying Superheavy Particles | V.Berezinsky | ?? | 1998 | astro-ph/9801046 | |
| 64 | ULTRA HIGH ENERGY COSMIC RAYS: PHYSICS ISSUES AND POTENTIALITIES OF THE AUGER HYBRID DETECTOR | The AUGER Collaboration (P. Billoir for the collaboration) | "Jerusalem 1997, High energy physics" 1011-1014 (1997) | 1997 | ?? | |
| 65 | Ultra-High Energy Cosmic Ray Propagation in the Local Supercluster | Guenter Sigl (Univ. of Chicago, USA), Martin Lemoine (DARC, CNRS, France), Peter Biermann (MPI fuer Radioastronomie, Bonn, Germany) | to appear in Astroparticle Physics | 1998 | astro-ph/9806242 | |
| 66 | Ultra-high energy cosmic ray sources and large scale magnetic fields | Martin Lemoine, Guenter Sigl, Angela V. Olinto, David N. Schramm (Univ. of Chicago) | Astrophys.J. 486 (1997) L115-L118 | 1997 | astro-ph/9704203 | |
| 67 | Ultra-high energy cosmic rays without GZK cutoff | V. Berezinsky, M. Kachelriess, A.Vilenkin | Phys.Rev.Lett. 79 (1997) 4302-4305 | 1997 | astro-ph/9708217 | |
| 68 | Why not cosmological cosmic rays? | Sato-H | New-Astronomy-Reviews. vol.42, no.3-4; Sept. 1998; p.287-8 | 1998 | Cosmic rays were once considered to be an indication of unknown cosmological processes, but they have turned out to be a minor product of astrophysical processes. However, the puzzle of the high-energy end of the cosmic-ray flux might bring about a radical change in physics, including a discovery of violation of the principle of relativity. |
Last Updated on 4/28/99
By Jeff Wilkes