Relevant bibliographies by topics / COSMIS RAYS

Contents

  1. Journal articles
  2. Dissertations / Theses
  3. Books
  4. Book chapters
  5. Conference papers
  6. Reports

Academic literature on the topic 'COSMIS RAYS'

Author: Grafiati
Published: 4 June 2021
Last updated: 1 February 2022

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Journal articles on the topic "COSMIS RAYS"

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Zreda, M., W. J. Shuttleworth, X. Zeng, C. Zweck, D. Desilets, T. Franz, and R. Rosolem. "COSMOS: the COsmic-ray Soil Moisture Observing System." Hydrology and Earth System Sciences 16, no. 11 (November 7, 2012): 4079–99. http://dx.doi.org/10.5194/hess-16-4079-2012.

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Abstract. The newly-developed cosmic-ray method for measuring area-average soil moisture at the hectometer horizontal scale is being implemented in the COsmic-ray Soil Moisture Observing System (or the COSMOS). The stationary cosmic-ray soil moisture probe measures the neutrons that are generated by cosmic rays within air and soil and other materials, moderated by mainly hydrogen atoms located primarily in soil water, and emitted to the atmosphere where they mix instantaneously at a scale of hundreds of meters and whose density is inversely correlated with soil moisture. The COSMOS has already deployed more than 50 of the eventual 500 cosmic-ray probes, distributed mainly in the USA, each generating a time series of average soil moisture over its horizontal footprint, with similar networks coming into existence around the world. This paper is written to serve a community need to better understand this novel method and the COSMOS project. We describe the cosmic-ray soil moisture measurement method, the instrument and its calibration, the design, data processing and dissemination used in the COSMOS project, and give example time series of soil moisture obtained from COSMOS probes.
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Zreda, M., W. J. Shuttleworth, X. Zeng, C. Zweck, D. Desilets, T. Franz, R. Rosolem, and T. P. A. Ferre. "COSMOS: The COsmic-ray Soil Moisture Observing System." Hydrology and Earth System Sciences Discussions 9, no. 4 (April 4, 2012): 4505–51. http://dx.doi.org/10.5194/hessd-9-4505-2012.

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Abstract. Area-average soil moisture at the sub-kilometer scale is needed but until the advent of the cosmic-ray method (Zreda et al., 2008), it was difficult to measure. This new method is now being implemented routinely in the COsmic-ray Soil Moisture Observing System (or COSMOS). The stationary cosmic-ray soil moisture probe (sometimes called "neutronavka") measures the neutrons that are generated by cosmic rays within air and soil, moderated by mainly hydrogen atoms located primarily in soil water, and emitted to the atmosphere where they mix instantaneously at a scale of hundreds of meters and whose density is inversely correlated with soil moisture. COSMOS has already deployed 53 of the eventual 500 neutronavkas distributed mainly in the USA, each generating a time series of average soil moisture over its hectometer horizontal footprint, with similar networks coming into existence around the world. This paper is written to serve a community need to better understand this novel method and the COSMOS project. We describe the cosmic-ray soil moisture measurement method, the instrument and its calibration, the design, data processing and dissemination used in COSMOS, and give example time series of soil moisture obtained from COSMOS probes.
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Wolfendale, Arnold W. "Physics and the Cosmos: The Origin of Cosmic Rays of ‘Low’ and ‘Very High’ Energies." Australian Journal of Physics 50, no. 4 (1997): 723. http://dx.doi.org/10.1071/p96088.

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The subject of ‘cosmic rays’ is one that embraces a vast range of particle and photon energies and is an ideal one for examining ‘Physics and the Cosmos’. In the present work we examine the twin problems of the origin of cosmic rays of both low and very high energies and find that they are related by studies of the Magellanic Clouds. This remarkable result comes from the hypothesis that there is a Giant Halo surrounding the Galaxy, support coming from Magellanic Cloud observations. Also examined is the flux of extragalactic gamma rays and its relevance to the question of the asymmetry between matter and anti-matter in the Universe.
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Герасимова, Сардаана, Sardaana Gerasimova, Петр Гололобов, Peter Gololobov, Владислав Григорьев, Vladislav Grigoryev, Прокопий Кривошапкин, et al. "Heliospheric modulation of cosmic rays: model and observation." Solar-Terrestrial Physics 3, no. 1 (May 5, 2017): 78–102. http://dx.doi.org/10.12737/article_58f970f2455545.93154609.

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This paper presents the basic model of cosmic ray modulation in the heliosphere, developed in Yu.G. Shafer Institute of Cosmophysical Research and Aeronomy of the Siberian Branch of RAS. The model has only one free modulation parameter: the ratio of the regular magnetic field to the turbulent one. It may also be applied to the description of cosmic ray intensity variations in a wide energy range from 100 MeV to 100 GeV. Possible mechanisms of generation of the mentioned turbulence field are considered. The primary assumption about the electrical neutrality of the heliosphere appears to be wrong, and the zero potential needed to match the model with observations in the plane of the solar equator can be achieved if the frontal point of the heliosphere, which is flowed around by interstellar gas, lies near the mentioned plane. We have revealed that the abnormal rise of cosmic ray intensity at the end of solar cycle 23 is related to the residual modulation produced by the subsonic solar wind behind the front of a standing shock wave. The model is used to describe features of cosmic ray intensity variations in several solar activity cycles.
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Guertzen, G. P., A. M. Marenny, and R. A. Nymmik. "Studies of low-energy HZE cosmic rays on cosmos satellites." International Journal of Radiation Applications and Instrumentation. Part D. Nuclear Tracks and Radiation Measurements 16, no. 1 (January 1989): 53–56. http://dx.doi.org/10.1016/1359-0189(89)90011-3.

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Mishra, R. K., and R. A. Mishra. "Modulation of Cosmic Rays Along with Solar and Heliospheric Anomalies." Kosmìčna nauka ì tehnologìâ 13, no. 6 (November 30, 2007): 99–108. http://dx.doi.org/10.15407/knit2007.06.099.

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ISRAEL, M. H. "ISOTOPIC COMPOSITION OF COSMIC RAYS: RESULTS FROM THE COSMIC RAY ISOTOPE SPECTROMETER ON THE ACE SPACECRAFT." International Journal of Modern Physics A 20, no. 29 (November 20, 2005): 6633. http://dx.doi.org/10.1142/s0217751x05029666.

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Over the past seven years the Cosmic Ray Isotope Spectrometer (CRIS) on the ACE spacecraft has returned data with an unprecedented combination of excellent mass resolution and high statistics, describing the isotopic composition of elements from lithium through nickel in the energy interval ~ 50 to 500 MeV/nucleon. These data have demonstrated: * The time between nucleosynthesis and acceleration of the cosmic-ray nuclei is at least 105 years. The supernova in which nucleosynthesis takes place is thus not the same supernova that accelerates a heavy nucleus to cosmic-ray energy. * The mean confinement time of cosmic rays in the Galaxy is 15 Myr. * The isotopic composition of the cosmic-ray source is remarkably similar to that of solar system. The deviations that are observed, particularly at 22 Ne and 58 Fe , are consistent with a model in which the cosmic-ray source is OB associations in which the interstellar medium has solar-system composition enriched by roughly 20% admixture of ejecta from Wolf-Rayet stars and supernovae. * Cosmic-ray secondaries that decay only by electron capture provide direct evidence for energy loss of cosmic rays as they penetrate the solar system. This invited overview paper at ECRS 19 was largely the same as an invited paper presented a month earlier at the 8th Nuclei in the Cosmos Conference in Vancouver. The proceedings of that conference will be published shortly by Elsevier as a special edition of Nuclear Physics A. For further summary of results from CRIS, the reader is referred to URL 〈〉 and links on that page to CRIS and to Science News.
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Annila, A. "Cosmic Rays Report from the Structure of Space." Advances in Astronomy 2015 (2015): 1–11. http://dx.doi.org/10.1155/2015/135025.

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Spectrum of cosmic rays follows a broken power law over twelve orders of magnitude. Since ubiquitous power laws are manifestations of the principle of least action, we interpret the spectrum accordingly. Our analysis complies with understanding that low-energy particles originate mostly from rapidly receding sources throughout the cosmos. The flux peaks about proton rest energy whereafter it decreases because fewer and fewer receding sources are energetic enough to provide particles with high enough velocities to compensate for the recessional velocities. Above 1015.6 eV the flux from the expanding Universe diminishes below the flux from the nearby nonexpanding part of the Universe. In this spectral feature, known as the “knee,” we relate to a distance of about 1.3 Mpc where the gravitational potential tallies the energy density of free space. At higher energies particles decelerate in a dissipative manner to attain thermodynamic balance with the vacuum. At about 1017.2 eV a distinct dissipative mechanism opens up for protons to slow down by electron-positron pair production. At about 1019.6 eV a more effective mechanism opens up via pion production. All in all, the universal principle discloses that the broad spectrum of cosmic rays probes the structure of space from cosmic distances down to microscopic details.
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Peregudov, Dmitriy, Anatoly Soloviev, Igor Yashin, and Victor Shutenko. "GALACTIC COSMIC RAY ANISOTROPY MODELLING." Solar-Terrestrial Physics 6, no. 1 (April 1, 2020): 29–34. http://dx.doi.org/10.12737/stp-61202003.

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We calculate the angular distribution of cosmic rays at a given point of the heliosphere under the assumption that the incoming flux from outer space is isotropic. The static magnetic field is shown to cause no anisotropy provided that the observation point is situated out of the trapped particle area. We consider a coronal ejection model in the form of a static cylinder with an axial homogeneous magnetic field inside. We calculate angular distribution samples in the trapped particle area (inside the cylinder) and show that there is a certain cone of directions with a reduced flux. For the same model with the moving cylinder, the angular distribution samples are calculated for different positions of the observation point outside the cylinder. Anisotropy of order of the ejection to light velocity ratio is shown to arise. The calculated samples are in qualitative agreement with URAGAN muon hodoscope data.
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Marenny, A. M., R. A. Nymmik, I. Hunyadi, I. Csige, F. Spurný, J. Charvát, and G. P. Guertzen. "Low-energy heavy ions of cosmic rays measured on cosmos-2044 biosatellite." International Journal of Radiation Applications and Instrumentation. Part D. Nuclear Tracks and Radiation Measurements 19, no. 1-4 (January 1991): 697–702. http://dx.doi.org/10.1016/1359-0189(91)90296-t.

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Dissertations / Theses on the topic "COSMIS RAYS"

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Ardashev, Khamit. "Asymmetry and Cross Section Measurements of Neutral Pion Photo-Production in the Range 240-405 MeV." Ohio University / OhioLINK, 2002. http://rave.ohiolink.edu/etdc/view?acc_num=ohiou1020689523.

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張增 and Tsang Cheung. "Primary cosmic ray composition at 10 [to the power] 15--10 [to the power] 17eV studied from extensive air shower simulations." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 1985. http://hub.hku.hk/bib/B31230593.

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Cheung, Tsang. "Primary cosmic ray composition at 10 [to the power] 15--10 [to the power] 17eV studied from extensive air shower simulations /." [Hong Kong : University of Hong Kong], 1985. http://sunzi.lib.hku.hk/hkuto/record.jsp?B12266176.

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Gabici, Stefano. "Gamma ray astronomy and the origin of galactic cosmic rays." Habilitation à diriger des recherches, Université Paris-Diderot - Paris VII, 2011. http://tel.archives-ouvertes.fr/tel-00719791.

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Diffusive shock acceleration operating at expanding supernova remnant shells is by far the most popular model for the origin of galactic cosmic rays. Despite the general consensus received by the model, an unambiguous and conclusive proof of the supernova remnant hypothesis is still missing. In this context, the recent developments in gamma ray astronomy provide us with precious insights into the problem of the origin of galactic cosmic rays, since production of gamma rays is expected both during the acceleration of cosmic rays at supernova remnant shocks and during their subsequent propagation in the interstellar medium. In particular, the recent detection of a number of supernova remnants at TeV energies nicely fits with the model, but it still does not constitute a conclusive proof of it, mainly due to the difficulty of disentangling the hadronic and leptonic contributions to the observed gamma ray emission. The main goal of my research is to search for an unambiguous and conclusive observational test for proving (or disproving) the idea that supernova remnants are the sources of galactic cosmic rays with energies up to (at least) the cosmic ray knee. Our present comprehension of the mechanisms of particle acceleration at shocks and of the propagation of cosmic rays in turbulent magnetic fields encourages beliefs that such a conclusive test might come from future observations of supernova remnants and of the Galaxy in the almost unexplored domain of multi-TeV gamma rays.
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Lee, Anthony A. "Application of Monte Carlo methods to some problems in high energy astrophysics /." Title page, contents and abstract only, 1993. http://web4.library.adelaide.edu.au/theses/09PH/09phl4768.pdf.

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Guberman, Daniel Alberto. "MAGIC observations with bright Moon and their application to measuring the VHE gamma-ray spectral cut-off of the PeVatron candidate Cassiopeia A." Doctoral thesis, Universitat Autònoma de Barcelona, 2018. http://hdl.handle.net/10803/664122.

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Los rayos cósmicos son núcleos atómicos que constantemente bombardean la Tierra. Está largamente aceptado que estos núcleos con energías de hasta ~3 PeV son de origen Galáctico. Pero aún no se sabe dónde en la Galaxia ni cómo son acelerados. Durante muchos años la hipótesis más popular ha sido que son acelerados en remanentes de supernova. En esta tesis presento los detalles de una serie de observaciones de la joven remanente de supernova Cassiopeia A, uno de los candidatos más prometedores a ser un Pevatrón, un sistema capaz de acelerar rayos cósmicos hasta energías de PeV. Las observaciones fueron realizadas con los telescopios MAGIC, que observan rayos gamma de muy alta energía (VHE, E > 50 GeV), entre Diciembre de 2014 y Octubre de 2016, adquiriendo 191 horas de datos buena calidad. Acumular una gran cantidad de horas de observación era indispensable para obtener una medida precisa del espectro y fue posible gracias a la posibilidad de extender el tiempo activo de MAGIC operando los telescopios bajo una luminosidad lunar intensa. Trabajé en la optimización de las observaciones con Luna en MAGIC, tanto en el momento de operar los telescopios como en la etapa del análisis de los datos. Abordo los detalles de este desarrollo y evaluó su rendimiento. Con más del 70 % de las horas obtenidas con la Luna presente en el cielo, he podido obtener el espectro más preciso hasta ahora de Cassiopeia A en VHE. Por primera vez se encuentra evidencia de un corte a E = 3,5 (+1,6\—1,0) stat (+0,8\−0,9) sys TeV en el espectro. El modelado de dicho espectro sugiere que la mayoría de los rayos gamma emitidos pueden ser atribuidos a una población de protones de muy alta energía con un índice espectral de ~2.2 y un corte a ~10 TeV. Esto implica que, asumiendo que no hay una difusión significativa d elos rayos cósmicos en el entorno de la supernova, Cassiopeia A no puede ser un PeVatrón en este momento.
Cosmic rays are atomic nuclei that are constantly bombarding the Earth. It is widely accepted that these nuclei with energies up to ~3 PeV are of Galactic origin. But the question about where in the Galaxy and how they are accelerated still remains unanswered. For several years the most popular hypothesis has been that they are accelerated in supernova remnants. In this thesis I present the details of a deep observation campaign on the young supernova remnant Cassiopeia A, one of the most promising candidates to be a PeVatron, a system capable of accelerating cosmic rays up to PeV energies. The observations were performed with the MAGIC telescopes, that observe very high energy (VHE, E > 50 GeV) gamma rays, between December 2014 and October 2016, acquiring 191 hours of good-quality data. Accumulating a large amount of observation hours was indispensable to obtain a precise measurement of the spectrum and it was possible thanks to the possibility of extending the MAGIC duty cycle by operating the telescopes under bright moonlight. I worked in the optimization of moonlight observations with MAGIC, both during the operation of the telescopes and at the data analysis stage. I discuss the details of these developments and the resulting performance. With more than 70% of the data obtained under moonlight, I was able to obtain the most precise spectrum of Cassiopeia A to date at VHE. The obtained spectrum shows for the rst time 4:9 evidence of a cut-o at E = 3,5 (+1,6\—1,0) stat (+0,8\−0,9) sys TeV. The modelling of the spectrum suggests that the bulk of the gamma-rays emitted can be attributed to a population of high-energy protons with spectral index ~2.2 and energy cuto at ~10 TeV. This implies that, assuming there is no signicant cosmic-ray diusion, Cassiopeia A cannot be a PeVatron at its present age.
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Pinzke, Anders. "Gamma-Ray Emission from Galaxy Clusters : DARK MATTER AND COSMIC-RAYS." Doctoral thesis, Stockholms universitet, Fysikum, 2010. http://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-42453.

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The quest for the first detection of a galaxy cluster in the high energy gamma-ray regime is ongoing, and even though clusters are observed in several other wave-bands, there is still no firm detection in gamma-rays. To complement the observational efforts we estimate the gamma-ray contributions from both annihilating dark matter and cosmic-ray (CR) proton as well as CR electron induced emission. Using high-resolution simulations of galaxy clusters, we find a universal concave shaped CR proton spectrum independent of the simulated galaxy cluster. Specifically, the gamma-ray spectra from decaying neutral pions, which are produced by CR protons, dominate the cluster emission. Furthermore, based on our derived flux and luminosity functions, we identify the galaxy clusters with the brightest galaxy clusters in gamma-rays. While this emission is challenging to detect using the Fermi satellite, major observations with Cherenkov telescopes in the near future may put important constraints on the CR physics in clusters. To extend these predictions, we use a dark matter model that fits the recent electron and positron data from Fermi, PAMELA, and H.E.S.S. with remarkable precision, and make predictions about the expected gamma-ray flux from nearby clusters. In order to remain consistent with the EGRET upper limit on the gamma-ray emission from Virgo, we constrain the minimum mass of substructures for cold dark matter halos. In addition, we find comparable levels of gamma-ray emission from CR interactions and dark matter annihilations without Sommerfeld enhancement.
At the time of the doctoral defense, the following papers were unpublished and had a status as follows: Paper 2: Accepted.
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Wilkinson, Christopher Richard. "The application of high precision timing in the high resolution fly's eye cosmic ray detector." Title page, contents and abstract only, 1998. http://hdl.handle.net/2440/37715.

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This thesis represents work performed by the author on the development of the High Resolution Fly's Eye (HiRes) detector for the study of extremely high energy (>10 [superscript 18] eV) cosmic rays. Chapter 1 begins with an review of this field. This chapter details the development of the field, the physics questions we seek to answer, and our current understanding based on experimental and theoretical results. It provides the basis for understanding why detectors such as HiRes are being constructed. This review leads into chapter 2, which discuses the development of cosmic ray induced extensive air showers (EAS) and the techniques used to study them. Particular emphasis is placed upon the air fluorescence technique utilised by HiRes. The two site HiRes prototype detector is then discussed in detail in chapter 3. This covers the different components that form the detector, together with details of the calibration performed to extract useful information from the data. Chapter 4 discusses the installation and subsequent testing of GPS based clock systems for the two sites that make up the HiRes prototype detector. The entire timing system was checked, and some previously hidden bugs fixed. This chapter concludes with work performed on the time to digital converter calibration for the second HiRes site. The high relative timing accuracy provided by the GPS clocks allowed the use of timing information in programs to reconstruct the arrival directions of cosmic rays. Chapter 5 covers the development of a program to use geometrical and timing information to reconstruct EAS viewed by both HiRes sites. This chapter concludes with an evaluation of the likely reconstruction accuracy of the new HiRes (stage1) detector. A well reconstructed EAS trajectory is the first step in the determination of more interesting parameters such as primary particle energy. Chapter 6 covers the collation and analysis of EAS viewed by the both sites of the prototype detector. This includes an evaluation of effects such as the atmosphere, and an estimation of the performance of the new (stage 1) HiRes detector based on results with the prototype detector. Finally the conclusions from this thesis are summarised and sugestions made for further follow up work.
Thesis (Ph.D.)--Department of Physics and Mathematical Physics, 1998.
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Chadwick, Mary Paula. "Very high energy cosmic gamma rays from radio and X-ray pulsars." Thesis, Durham University, 1987. http://etheses.dur.ac.uk/6720/.

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This thesis is concerned with the detection of very high energy cosmic gamma-rays from isolated pulsars and X-ray binary sources using the atmospheric Cerenkov technique. A general introduction to gamma ray detection techniques is followed by adscription of the properties of atmospheric Cerenkov radiation and a discussion of the principles of the atmospheric Cerenkov technique. The Mark I and Mark II gamma-ray telescopes operated in Dugway, Utah by the University of Durham between 1981 and 1984 are briefly described. There follows a discussion of the results from observations at many different wavelengths of Cygnus X-3. This object was observed by the Durham group between 1981 and 1983 in Dugway Utah and also in Durham during autumn 1985. The detection in the Dugway data of the 4.8 hr X-ray period and the possible detection of a19.2 day intensity variation are considered. The discovery of a 12.59 ms pulsar in data taken on Cygnus X-3 in 1983 is described. Evidence is presented which suggests this periodicity is also present at a weaker level in earlier data and also in the data taken in Durham in 1985.Results from observations of PSR1937+21 , PSR1953+29and six radio pulsars , are presented. The design and construction of the Mark III telescope, now operating in Narrabri , N.S.W. , is described in detail. Preliminary results from observations with the Mark III telescope of three objects, LMC X-4, the Vela pulsar and CentaurusX-3, are presented, with particular reference to periodicities inherent in the sources. An observation of the supernova in the Large Magellanic Cloud is discussed. A brief discussion of the mechanisms by which V.H.E. gamma-rays may be produced in isolated pulsars and X-ray binary pulsars is given, followed by a description of the future prospects for the Mark III and Mark IV telescopes.
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Richardson, K. M. "Gamma rays, cosmic rays and local molecular clouds." Thesis, Durham University, 1988. http://etheses.dur.ac.uk/942/.

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Books on the topic "COSMIS RAYS"

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Friedlander, Michael W. Cosmic rays. Cambridge, Mass: Harvard University Press, 1989.

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W, Friedlander Michael. Cosmic rays. Cambridge: Harvard Univ Press, 1990.

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Otaola, Javier A. Los Rayos cósmicos: Mensajeros de las estrellas. Mexico: Fondo de Cultura Economica, 1994.

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Solar cosmic rays. Dordrecht: Kluwer Academic Publishers, 2001.

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Miroshnichenko, Leonty. Solar Cosmic Rays. Cham: Springer International Publishing, 2015. http://dx.doi.org/10.1007/978-3-319-09429-8.

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Miroshnichenko, Leonty I. Solar Cosmic Rays. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-015-9646-6.

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High energy cosmic rays. 2nd ed. Berlin: Springer, 2010.

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Stanev, Todor. High Energy Cosmic Rays. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-540-85148-6.

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Bieber, J. W., E. Eroshenko, P. Evenson, E. O. Flückiger, and R. Kallenbach, eds. Cosmic Rays and Earth. Dordrecht: Springer Netherlands, 2000. http://dx.doi.org/10.1007/978-94-017-1187-6.

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Stanev, Todor. High Energy Cosmic Rays. Cham: Springer International Publishing, 2021. http://dx.doi.org/10.1007/978-3-030-71567-0.

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Book chapters on the topic "COSMIS RAYS"

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Hofmann, W., and J. A. Hinton. "Cosmic Particle Accelerators." In Particle Physics Reference Library, 827–63. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-34245-6_13.

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AbstractIn the century since the measurements of Victor Hess [1]—considered as the discovery of cosmic rays—the properties of cosmic rays, as they arrive on Earth, have been studied in remarkable detail; we know their energy spectrum, extending to 1020 eV, their elemental composition, their angular distribution, and we understand the basic energetic requirements of cosmic ray production in the Galaxy.
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Gooch, Jan W. "Cosmic Rays." In Encyclopedic Dictionary of Polymers, 174. New York, NY: Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4419-6247-8_2971.

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Schröder, Frank G. "Cosmic Rays." In Springer Theses, 5–18. Berlin, Heidelberg: Springer Berlin Heidelberg, 2012. http://dx.doi.org/10.1007/978-3-642-33660-7_2.

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Flügge, S. "Cosmic Rays." In General Index / Generalregister, 575–92. Berlin, Heidelberg: Springer Berlin Heidelberg, 1988. http://dx.doi.org/10.1007/978-3-642-82502-6_9.

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Fleischer, Robert L. "Cosmic Rays." In Tracks to Innovation, 101–31. New York, NY: Springer New York, 1998. http://dx.doi.org/10.1007/978-1-4612-4452-3_5.

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Jokipii, J. R. "Cosmic rays." In From the Sun: Auroras, Magnetic Storms, Solar Flares, Cosmic Rays, 123–31. Washington, D. C.: American Geophysical Union, 1998. http://dx.doi.org/10.1029/sp050p0123.

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Beckman, John Etienne. "Cosmic Rays? Cosmic Particles." In Astronomers' Universe, 259–83. Cham: Springer International Publishing, 2021. http://dx.doi.org/10.1007/978-3-030-68372-6_9.

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Fernández Barral, Alba. "Cosmic Rays and Gamma-Ray Astrophysics." In Extreme Particle Acceleration in Microquasar Jets and Pulsar Wind Nebulae with the MAGIC Telescopes, 3–16. Cham: Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-97538-2_1.

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Schlickeiser, Reinhard. "Galactic Cosmic Rays." In Cosmic Ray Astrophysics, 435–59. Berlin, Heidelberg: Springer Berlin Heidelberg, 2002. http://dx.doi.org/10.1007/978-3-662-04814-6_17.

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McDonald, Frank B., and Vladimir S. Ptuskin. "Galactic cosmic rays." In The Century of Space Science, 677–97. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-0320-9_29.

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Conference papers on the topic "COSMIS RAYS"

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George, J. S. "Cosmic ray source abundances and the acceleration of cosmic rays." In Acceleration and transport of energetic particles observed in the heliosphere (ACE-2000 symposium). AIP, 2000. http://dx.doi.org/10.1063/1.1324355.

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Moskalenko, Igor V. "Propagation of Cosmic Rays: Nuclear Physics in Cosmic-Ray Studies." In INTERNATIONAL CONFERENCE ON NUCLEAR DATA FOR SCIENCE AND TECHNOLOGY. AIP, 2005. http://dx.doi.org/10.1063/1.1945315.

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Lingenfelter, R. E. "Cosmic ray acceleration in superbubbles and the composition of cosmic rays." In Acceleration and transport of energetic particles observed in the heliosphere (ACE-2000 symposium). AIP, 2000. http://dx.doi.org/10.1063/1.1324342.

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Tkachev, Igor. "Cosmic Rays." In XXIst International Europhysics Conference on High Energy Physics. Trieste, Italy: Sissa Medialab, 2012. http://dx.doi.org/10.22323/1.134.0013.

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Donato, Fiorenza. "Cosmic rays and the diffuse gamma-ray emission." In 7th International Fermi Symposium. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.312.0134.

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Rachen, Jörg P., and P. Mészáros. "Cosmic rays and neutrinos from gamma-ray bursts." In GAMMA-RAY BURSTS. ASCE, 1998. http://dx.doi.org/10.1063/1.55402.

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Scarsi, Livio. "Gamma ray bursts and extreme energy cosmic rays." In WORKSHOP ON OBSERVING GIANT COSMIC RAY AIR SHOWERS FROM >1020 eV Particles from Space. ASCE, 1998. http://dx.doi.org/10.1063/1.56132.

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Cherry, Michael L. "Composition and energy spectra of cosmic rays—Implications for cosmic ray origins." In INTERSECTIONS BETWEEN PARTICLE AND NUCLEAR PHYSICS. ASCE, 1997. http://dx.doi.org/10.1063/1.54237.

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Ahlers, Markus. "The cosmic triad: Cosmic rays, gamma-rays and neutrinos." In 5TH INTERNATIONAL WORKSHOP ON ACOUSTIC AND RADIO EEV NEUTRINO DETECTION ACTIVITIES: ARENA 2012. AIP, 2013. http://dx.doi.org/10.1063/1.4807556.

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Ramesh, Rashmi. "Adventures in Inflation And Cosmic Microwave Background - The future of the cosmos." In The 34th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2016. http://dx.doi.org/10.22323/1.236.0511.

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Reports on the topic "COSMIS RAYS"

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Murase, Kohta, Kunihito Ioka, Shigehiro Nagataki, and Takashi Nakamura. High Energy Neutrinos and Cosmic-Rays From Low-Luminosity Gamma-Ray Bursts? Office of Scientific and Technical Information (OSTI), July 2006. http://dx.doi.org/10.2172/886791.

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Tajima, T., and Y. Takahashi. Laboratory laser acceleration and high energy astrophysics: {gamma}-ray bursts and cosmic rays. Office of Scientific and Technical Information (OSTI), August 1998. http://dx.doi.org/10.2172/674811.

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Chapline, George F., Andrew M. Glenn, Les F. Nakae, Iwona Pawelczak, Neal J. Snyderman, Steven A. Sheets, and Ron E. Wurtz. Time-Correlated Particles Produced by Cosmic Rays. Office of Scientific and Technical Information (OSTI), May 2015. http://dx.doi.org/10.2172/1251035.

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Aguayo Navarrete, Estanislao, John L. Orrell, and Richard T. Kouzes. Monte Carlo Simulations of Cosmic Rays Hadronic Interactions. Office of Scientific and Technical Information (OSTI), April 2011. http://dx.doi.org/10.2172/1022429.

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Poirier, J. Calculation of Atmospheric Muons from Cosmic Gamma Rays. Office of Scientific and Technical Information (OSTI), April 2005. http://dx.doi.org/10.2172/839832.

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Durham, J. Matthew. Cosmic Ray Muon Tomography. Office of Scientific and Technical Information (OSTI), October 2016. http://dx.doi.org/10.2172/1329840.

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Davoudiasl, Hooman. Gravi-Burst: Super-GZK Cosmic Rays from Localized Gravity. Office of Scientific and Technical Information (OSTI), October 2000. http://dx.doi.org/10.2172/784723.

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Bloom, Elliott. THE ORIGIN OF COSMIC RAYS: WHAT CAN GLAST SAY? Office of Scientific and Technical Information (OSTI), October 2000. http://dx.doi.org/10.2172/784735.

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Guardincerri, Elena, Jeffrey Darnell Bacon, Tess Marie Daughton, J. Matthew Durham, Shelby Fellows, Olivia Ruth Johnson, Deborah Jean Morley, et al. Imaging the inside of thick structures using cosmic rays. Office of Scientific and Technical Information (OSTI), October 2015. http://dx.doi.org/10.2172/1223764.

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Plewa, Matthew I., and Justin Vandenbroucke. Detecting cosmic rays using CMOS sensors in consumer devices. Ames (Iowa): Iowa State University. Library. Digital Press, January 2015. http://dx.doi.org/10.31274/ahac.9757.

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