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Bibliografias temáticas / Cosmic-ray theory

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Literatura científica selecionada sobre o tema "Cosmic-ray theory"

Autor: Grafiati

Publicado: 14 de março de 2023

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Artigos de revistas sobre o assunto "Cosmic-ray theory"

1

Hand, Eric. "Cosmic-ray theory unravels". Nature 463, n.º 7284 (fevereiro de 2010): 1011. http://dx.doi.org/10.1038/4631011a.

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Ferreira, Stefan E. S. "Theory of cosmic ray modulation". Proceedings of the International Astronomical Union 4, S257 (setembro de 2008): 429–38. http://dx.doi.org/10.1017/s1743921309029664.

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AbstractThis work aims to give a brief overview on the topic of cosmic ray modulation in the heliosphere. The heliosphere, heliospheric magnetic field, transport parameters and the transport equation together with modulation models, which solve this equation in various degree of complexity, are briefly discussed. Results from these models are then presented where first it is shown how cosmic rays are globally distributed in an asymmetrical heliosphere which results from the relative motion between the local interstellar medium and the Sun. Next the focus shifts to low-energy Jovian electrons. The intensities of these electrons, which originate from a point source in the inner heliosphere, exhibit a unique three-dimensional spiral structure where most of the particles are transported along the magnetic field lines. Time-dependent modulation is also discussed where it is shown how drift effects together with propagating diffusion barriers are responsible for modulation over a solar cycle.

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Dorman, L. I., e I. V. Dorman. "Cosmic-ray atmospheric electric field effects". Canadian Journal of Physics 73, n.º 7-8 (1 de julho de 1995): 440–43. http://dx.doi.org/10.1139/p95-063.

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Experimental data on the atmospheric electric field effect in the cosmic-ray muon component are discussed on the basis of the general theory of cosmic-ray meteorological effects. In this framework, we develop the theory of atmospheric electric field effects in the hard- and soft-muons of secondary cosmic rays and in the neutron-monitor counting rates as well. We show that the experimental results can be understood on the basis of this theory. We also show that a sufficient atmospheric electric field effect in the cosmic-ray neutron component is to be expected because the neutron monitors work as analyzers of soft muons and really detect only negative muons as well as neutrons.

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Ivlev, Alexei V., Kedron Silsbee, Marco Padovani e Daniele Galli. "Rigorous Theory for Secondary Cosmic-Ray Ionization". Astrophysical Journal 909, n.º 2 (1 de março de 2021): 107. http://dx.doi.org/10.3847/1538-4357/abdc27.

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Starodubtsev, Sergei. "Shape of spectrum of galactic cosmic ray intensity fluctuations". Solar-Terrestrial Physics 8, n.º 2 (30 de junho de 2022): 71–75. http://dx.doi.org/10.12737/stp-82202211.

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The impact of solar wind plasma on fluxes of galactic cosmic rays (CR) penetrating from the outside into the heliosphere with energies above ~1 GeV leads to temporal variations in the CR intensity in a wide frequency range. Cosmic rays being charged particles, their modulation occurs mainly under impacts of the interplanetary magnetic field. It is well known that the observed spectrum of interplanetary magnetic field (IMF) fluctuations in a wide frequency range ν from ~10–7 to ~10 Hz has a pronounced falling character and consists of three sections: energy, inertial, and dissipative. Each of them is described by the power law PIMF(ν)~ν–α, while the IMF spectrum index α increases with increasing frequency. The IMF fluctuations in each of these sections are also characterized by properties that depend on their nature. Also known are established links between fluctuation spectra of the interplanetary magnetic field and galactic cosmic rays in the case of modulation of the latter by Alfvén or fast magnetosonic waves. The theory predicts that fluctuation spectra of cosmic rays should also be described by the power law PCR(ν)~ν–γ. However, the results of many years of SHICRA SB RAS research into the nature and properties of cosmic ray intensity fluctuations based on data from neutron monitors at stations with different geomagnetic cut-offs RC from 0.5 to 6.3 GV show that the observed spectrum of fluctuations in galactic cosmic ray intensity in the frequency range above 10–4 Hz becomes flat, i.e. it is similar to white noise. This fact needs to be realized and explained. This paper reports the results of research into the shape of the spectrum of galactic cosmic ray intensity fluctuations within a frequency range ν from ~10–6 to ~1 Hz and compares them with model calculations of white noise spectra, using measurement data from the neutron monitor of the Apatity station. A possible physical explanation has been given for the observed shape of the cosmic ray fluctuation spectrum on the basis of the known mechanisms of their modulation in the heliosphere.

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Wentzel, Donat G. "Self-Confined Cosmic Rays". Symposium - International Astronomical Union 107 (1985): 341–54. http://dx.doi.org/10.1017/s007418090007580x.

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Cosmic rays do not stream freely through the galaxy, contrary to earlier expectations. Streaming cosmic rays are slowed down by the emission of resonant Alfven waves that scatter the cosmic rays. The theory of self-confinement explains the isotropy of the bulk of the cosmic rays but not of cosmic rays above 103 Gev; it has been a stimulus to the theory for cosmic-ray acceleration at supernova shocks; and, on inclusion of diffusion in a galactic wind, it may explain the uniform cosmic-ray density out to 18 kpc in our galaxy. Rapidly streaming electrons in clusters of galaxies, in supernova remnants, and near solar flares are accomodated by the theory when it is expanded to include the effects of hot plasmas and other wave modes. A “resonance gap” may prevent the turning backwards of streaming particles and thus allow streaming near the particle speed.

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Shalchi, A. "Second-order quasilinear theory of cosmic ray transport". Physics of Plasmas 12, n.º 5 (maio de 2005): 052905. http://dx.doi.org/10.1063/1.1895805.

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KUSENKO, ALEXANDER. "COSMIC CONNECTIONS: FROM COSMIC RAYS TO GAMMA RAYS, COSMIC BACKGROUNDS AND MAGNETIC FIELDS". Modern Physics Letters A 28, n.º 02 (20 de janeiro de 2013): 1340001. http://dx.doi.org/10.1142/s0217732313400014.

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Combined data from gamma-ray telescopes and cosmic-ray detectors have produced some new surprising insights regarding intergalactic and galactic magnetic fields, as well as extragalactic background light. We review some recent advances, including a theory explaining the hard spectra of distant blazars and the measurements of intergalactic magnetic fields based on the spectra of distant sources. Furthermore, we discuss the possible contribution of transient galactic sources, such as past gamma-ray bursts and hypernova explosions in the Milky Way, to the observed flux of ultrahigh-energy cosmic-rays nuclei. The need for a holistic treatment of gamma rays, cosmic rays, and magnetic fields serves as a unifying theme for these seemingly unrelated phenomena.

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Krennrich, Frank. "TeV GAMMA RAYS: OBSERVATIONS VERSUS EXPECTATIONS & THEORY". Acta Polytechnica 53, A (18 de dezembro de 2013): 635–40. http://dx.doi.org/10.14311/ap.2013.53.0635.

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The scope of this paper is to discuss two important questions relevant for TeV γ-ray astronomy; the pursuit to reveal the origin of cosmic rays in our galaxy, and the opacity of the universe in γ-rays. The origin of cosmic rays stipulated the field of TeV astronomy in the first place, and led to the development of the atmospheric Cherenkov technique; significant progress has been made in the last decade through the detection of several supernova remnants, the primary suspects for harboring the acceleration sites of cosmic rays. TeV γ-rays propagate mostly unhindered through the galactic plane, making them excellent probes of processes in SNRs and other galactic sources. Key results related to the SNR origin of cosmic rays are discussed. TeV γ-ray spectra from extragalactic sources experience significant absorption when traversing cosmological distances. The opacity of the universe to γ-rays above 10 GeV progressively increases with energy and redshift; the reason lies in their pair production with ambient soft photons from the extragalactic background light (EBL). While this limits the γ-ray horizon, it offers the opportunity to gain information about cosmology, i.e. the EBL intensity, physical conditions in intergalactic space, and potentially new interaction processes. Results and implications pertaining to the EBL are given.

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Schlickeiser, Reinhard. "Cosmic-Ray Transport and Acceleration". International Astronomical Union Colloquium 142 (1994): 926–36. http://dx.doi.org/10.1017/s0252921100078337.

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AbstractWe review the transport and acceleration of cosmic rays concentrating on the origin of galactic cosmic rays. Quasi-linear theory for the acceleration rates and propagation parameters of charged test particles combined with the plasma wave viewpoint of modeling weak cosmic electromagnetic turbulence provides a qualitatively and quantitatively correct description of key observations. Incorporating finite frequency effects, dispersion, and damping of the plasma waves are essential in overcoming classical discrepancies with observations as the Kfit - Kql discrepancy of solar particle events. We show that the diffusion-convection transport equation in its general form contains spatial convection and diffusion terms as well as momentum convection and diffusion terms. In particular, the latter momentum diffusion term plays a decisive role in the acceleration of cosmic rays at super-Alfvénic supernova shock fronts, and in the acceleration of ultra-high-energy cosmic rays by distributed acceleration in our own galaxy.Subject headings: acceleration of particles — convection — cosmic rays — diffusion — shock waves

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Mais fontes

Teses / dissertações sobre o assunto "Cosmic-ray theory"

1

Gieseler, Jan [Verfasser]. "Understanding Galactic Cosmic Ray Modulation: Observations and Theory / Jan Gieseler". Kiel : Universitätsbibliothek Kiel, 2018. http://d-nb.info/1155760816/34.

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Fornieri, Ottavio. "Cosmic-ray transport in the Milky Way and related phenomenology". Doctoral thesis, Università di Siena, 2021. http://hdl.handle.net/11365/1143115.

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In this thesis, we aim at studying some of the open questions regarding the origin of the "Cosmic Rays" (CRs), as well as their transport properties. The exceptional quality of the experimentally measured cosmic-ray observables, especially at the recently-achieved energies in the range ~O(100 GeV - 1 TeV), started to question the standard picture, based on a "Supernova Remnant"-(SNR)-only origin of the CRs and a diffusive propagation inspired by the "Quasi-Linear Theory" (QLT) of pitch-angle interaction against alfvénic turbulence. First, we reproduce the most relevant cosmic-ray observables to tune the propagation setup, numerically solving the transport equation with the DRAGON code. On top of this, to account for the rising of the e^+ above ~10 GeV, we fit a primary population of positrons originating in Pulsar Wind Nebulae, in a model-independent setup that considers the uncertainties in the pulsar injections mechanism. Since the all-lepton spectrum is still not reproduced above ~50 GeV --- and in particular the ~TeV break --- we consider the contribution from a nearby source of e^-, and conclude that an old t_{age} ~ 10^5 yr SNR, located between ~600 pc and ~1 kpc, is probably missing from the Catalogues. Within the hypothesis of such old remnant in its radiative phase contributing to the e^+ + e^-, we search for its signature in the proton flux as well. To do this, we consider a phenomenological propagation setup that reproduces the hadronic spectral hardening at ~200 GeV as a diffusive feature D(E) ~ E^delta(E), and adopt it consistently for the large-scale background and for the nearby source. Within this framework, we account for the all-lepton spectrum, the proton spectrum and the cosmic-ray dipole anisotropy with the same old (t_{age} = 2*10^5 yr), nearby (d = 300 pc) remnant. We highlight that the progressively hardening diffusion coefficient is a crucial ingredient, since, in a single-power-law diffusion scenario, the dipole anisotropy data would be overshot by, at least, one order of magnitude. Finally, we explore the phenomenological implications of a change of paradigm in the standard cosmic-ray diffusion --- based on wave-particle interaction with Alfvén fluctuations --- considering a non-linear extension of the QLT that enhances the efficiency of CR-scattering with the other "Magneto-Hydro-Dynamic" (MHD) modes. Indeed, assuming the anisotropy of the alfvénic cascade, its scattering rate at all energies below ~100 TeV is not able to confine charged cosmic rays, and the fast magnetosonic modes alone shape the diffusion coefficient that particles experience in the Galaxy. Within such picture, we implement the resulting D(E) in DRAGON2, where two independent zones differently affect the evolution of the MHD cascade: the Halo (L_{Halo} ~ 5-6 kpc) and the Warm Ionized Medium (L_{WIM} ~ 1 kpc). We find that, with a reasonable choice of selected quantities, representing the physics of the environments, we can reproduce the hadronic fluxes, as well as the boron-over-carbon ratio, from ~200 GeV above. We assign to the rising of the "streaming instabilities" the cosmic-ray transport below this energy.

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3

Singleterry, Robert Clay Jr. "Neutron transport associated with the galactic cosmic ray cascade". Diss., The University of Arizona, 1993. http://hdl.handle.net/10150/186421.

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Transport of low energy neutrons associated with the galactic cosmic ray cascade is analyzed in this dissertation. A benchmark quality analytical algorithm is demonstrated for use with B scRYNTRN, a computer program written by the High Energy Physics Division of N scASA Langley Research Center, which is used to design and analyze shielding against the radiation created by the cascade. B scRYNTRN uses numerical methods to solve the integral transport equations for baryons with the straight-ahead approximation, and numerical and empirical methods to generate the interaction probabilities. The straight-ahead approximation is adequate for charged particles, but not for neutrons. As N scASA Langley improves B scRYNTRN to include low energy neutrons, a benchmark quality solution is needed for comparison. The neutron transport algorithm demonstrated in this dissertation uses the closed-form Green's function solution to the galactic cosmic ray cascade transport equations to generate a source of neutrons. A basis function expansion for finite heterogeneous and semi-infinite homogeneous slabs with multiple energy groups and isotropic scattering is used to generate neutron fluxes resulting from the cascade. This method, called the F(N) method, is used to solve the neutral particle linear Boltzmann transport equation. As a demonstration of the algorithm coded in the programs M scGSLAB and M scGSEMI, neutron and ion fluxes are shown for a beam of fluorine ions at 1000 MeV per nucleon incident on semi-infinite and finite aluminum slabs. Also, to demonstrate that the shielding effectiveness against the radiation from the galactic cosmic ray cascade is not directly proportional to shield thickness, a graph of transmitted total neutron scalar flux versus slab thickness is shown. A simple model based on the nuclear liquid drop assumption is used to generate cross sections for the galactic cosmic ray cascade. The E scNDF/B V database is used to generate the total and scattering cross sections for neutrons in aluminum. As an external verification, the results from M scGSLAB and M scGSEMI were compared to A scNISN/P scC, a routinely used neutron transport code, showing excellent agreement. In an application to an aluminum shield, the F(N) method seems to generate reasonable results.

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4

Kuno, Yugo Mafra 1982. "Elaboração de um método global de reconstrução de chuveiros extensos utilizando teoria da informação e otimização matemática". [s.n.], 2017. http://repositorio.unicamp.br/jspui/handle/REPOSIP/330494.

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Orientador: José Augusto Chinellato
Dissertação (mestrado) - Universidade Estadual de Campinas, Instituto de Física Gleb Wataghin
Made available in DSpace on 2018-09-02T17:59:22Z (GMT). No. of bitstreams: 1 Kuno_YugoMafra_M.pdf: 3634635 bytes, checksum: afd1f210608c9cb926532d441cade068 (MD5) Previous issue date: 2017
Resumo: O fluxo de raios cósmicos de ultra-alta energia (superiores a 10^18 eV) que chega ao topo da atmosfera é baixo, tal que torna-se necessário estudar em detalhes os chuveiros atmosféricos extensos de modo a se determinar a composição e a energia da partícula primária. Dispõe-se de algoritmos que simulam processos de QED e QCD, e descrevem a difusão das partículas na atmosfera, fornecendo o estado (x, p, id, t) de cada uma. Entretanto, é também necessário parametrizar as funções que descrevem sua distribuição ao longo da cascata atmosférica. O método da entropia máxima (MEM) permite que se parametrize a distribuição de partículas em função dos momentos estatísticos esses perfis, que são menos afetados pelo ruído. A maximização da entropia também permite que a distribuição seja inferida minimizando o enviesamento que ocorre, por exemplo, no ajuste de curvas tradicionalmente realizado. No presente trabalho foi estudada aplicação do MEM na análise do perfil longitudinal das componentes eletrônica e muônica geradas por simulação no CORSIKA, já conhecendo as características da partícula primária, de forma a avaliar os benefícios dessa metodologia no estudo de chuveiros atmosféricos
Abstract: The flux of ultra-high energy cosmic rays (above 10^18 eV) that reach the upper atmosphere is low, so that it is necessary to thoroughly study air showers in order to determine the composition and energy of the primary particle. There are algorithms that simulate QED and QCD processes, and track the particle diffusion in the atmosphere, providing the state (x, p, id, t) of each one. Still, it is also necessary to parameterize the functions that describe its distribution throughout the atmospheric cascade. The maximum entropy method (MEM) allows the parameterization of the particle distribution with the statistical moments as variables, which are less affected by noise. The maximum entropy also allows the inference of the distribution minimizing the bias, which is high in inference processes such as the traditional curve fitting. The application of MEM in the analysis of the longitudinal profile of the electronic and muonic components generated by simulation with CORSIKA was the object of study in this research work, having as a prior the characteristics of the primary particle, in order to evaluate the benefits of the method in the study of air showers
Mestrado
Física
Mestre em Física
CAPES

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5

Perassa, Eder Arnedo 1982. "Métodos de estatística bayesiana e máxima entropia aplicados na análise de dados em eventos de raios cósmicos". [s.n.], 2017. http://repositorio.unicamp.br/jspui/handle/REPOSIP/331058.

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Orientador: José Augusto Chinellato
Tese (doutorado) - Universidade Estadual de Campinas, Instituto de Física Gleb Wataghin
Made available in DSpace on 2018-09-03T07:30:39Z (GMT). No. of bitstreams: 1 Perassa_EderArnedo_D.pdf: 3556275 bytes, checksum: c4e6180df4a4a5dcbfe476b7d331bee4 (MD5) Previous issue date: 2017
Resumo: Neste trabalho, estudamos os métodos de estatística bayesiana e máxima entropia na análise de dados em eventos de raios cósmicos. Inicialmente, fizemos um resumo sobre o desenvolvimento da física de raios cósmicos em que descrevemos alguns resultados teóricos e experimentais recentes. A seguir, apresentamos uma breve revisão do método bayesiano e o aplicamos na determinação da composição em massa dos primários em eventos de raios cósmicos. Além disso, introduzimos o método de máxima entropia e propomos um método de parametrização do perfil longitudinal de chuveiros atmosféricos extensos. Em todas as aplicações, foram mostrados os algoritmos desenvolvidos e os resultados obtidos a partir de dados de eventos simulados. Os resultados indicaram que tais métodos podem ser utilizados satisfatoriamente como ferramentas na análise de dados em eventos de raios cósmicos
Abstract: In this work, we study bayesian statistics and maximum entropy methods in cosmic ray events data analysis. At first, we summarized developments in cosmic rays physics, describing some recent theoretical and experimental results. We present briefly a review of bayesian method and apply it to the problem of determining mass composition primary cosmic ray events. Moreover, we introduce the maximum entropy method and propose a method for the parametrization of the longitudinal profile of extensive air showers. In all applications, the algorithms developed and the results obtained from simulated event data were shown. The results suggested that such methods can be satisfactorily used as tools in cosmic rays events data analysis
Doutorado
Física
Doutor em Ciências
277612/2007
CAPES

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Wade, Richard Peter. "A systematics for interpreting past structures with possible cosmic references in Sub-Saharan Africa". Diss., Pretoria : [s.n.], 2009. http://upetd.up.ac.za/thesis/available/etd-05052009-174557/.

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Livros sobre o assunto "Cosmic-ray theory"

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1940-, Wilson John W., e United States. National Aeronautics and Space Administration. Scientific and Technical Information Program., eds. An efficient HZETRN: (a galactic cosmic ray transport code). [Washington, DC]: National Aeronautics and Space Administration, Office of Management, Scientific and Technical Information Program, 1992.

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2

Blandford, Roger D. Particle acceleration at astrophysical shocks: A theory of cosmic ray origin. Amsterdam: North-Holland, 1987.

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3

United States. National Aeronautics and Space Administration., ed. Studies using IMP, Voyager and Pioneer cosmic ray data to determine the size of the heliosphere. [Washington, DC: National Aeronautics and Space Administration, 1996.

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United States. National Aeronautics and Space Administration., ed. Studies using IMP, Voyager and Pioneer cosmic ray data to determine the size of the heliosphere. [Washington, DC: National Aeronautics and Space Administration, 1996.

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5

Stuewer, Roger H. The Plague Spreads to Austria and Italy. Oxford University Press, 2018. http://dx.doi.org/10.1093/oso/9780198827870.003.0014.

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Hitler annexed Austria to Germany on March 15, 1938. Erwin Schrödinger, in Graz, soon regretted having applauded this and fled to Dublin. Stefan Meyer pre-emptively resigned his professorship in Vienna. Marietta Blau, discoverer of cosmic-ray disintegration “stars,” immigrated to Mexico. Polonium expert Elizabeth Rona immigrated to America. Renowned Lise Meitner escaped to Stockholm, where she received little scientific or personal support. Mussolini’s Fascist Italy adopted Nazi racial policies and enacted anti-Semitic laws in the fall of 1938. Bruno Rossi, dismissed from his professorship in Padua, immigrated with his wife to England and then to America. Emilio Segrè relinquished his professorship in Palermo and immigrated with his wife and young son to America. Enrico Fermi, his Jewish wife Laura, and their two children, went to Stockholm where he received the 1938 Nobel Prize in Physics and then immigrated to America to begin what Laura Fermi called the process of Americanization.

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Capítulos de livros sobre o assunto "Cosmic-ray theory"

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Shalchi, Andreas. "The Quasilinear Theory". In Nonlinear Cosmic Ray Diffusion Theories, 57–81. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00309-7_3.

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Shalchi, Andreas. "The Weakly Nonlinear Theory". In Nonlinear Cosmic Ray Diffusion Theories, 99–114. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00309-7_5.

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Shalchi, Andreas. "The Nonlinear Guiding Center Theory". In Nonlinear Cosmic Ray Diffusion Theories, 83–97. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00309-7_4.

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Shalchi, Andreas. "The Extended Nonlinear Guiding Center Theory". In Nonlinear Cosmic Ray Diffusion Theories, 135–53. Berlin, Heidelberg: Springer Berlin Heidelberg, 2009. http://dx.doi.org/10.1007/978-3-642-00309-7_7.

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Feinberg, Eugene L. "Particle Theory — Cosmic Rays — Accelerators Conflicts and Reconciliations". In Early History of Cosmic Ray Studies, 339–53. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5434-2_33.

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Yukawa, Hideki. "Cosmic Rays and the Beginning of the Meson Theory". In Early History of Cosmic Ray Studies, 133–35. Dordrecht: Springer Netherlands, 1985. http://dx.doi.org/10.1007/978-94-009-5434-2_12.

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Vink, Jacco. "Cosmic-Ray Acceleration by Supernova Remnants: Introduction and Theory". In Astronomy and Astrophysics Library, 277–321. Cham: Springer International Publishing, 2020. http://dx.doi.org/10.1007/978-3-030-55231-2_11.

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Hick, P., G. Stevens e J. van Rooijen. "The Maximum Entropy Principle in Cosmic Ray Transport Theory". In Astrophysics and Space Science Library, 355–58. Dordrecht: Springer Netherlands, 1986. http://dx.doi.org/10.1007/978-94-009-4612-5_43.

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Berezhko, E. G. "Theory of Cosmic Ray and High-Energy Gamma-Ray Production in Supernova Remnants". In Astrophysical Sources of High Energy Particles and Radiation, 1–17. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-010-0560-9_1.

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Berezhko, Evgeny. "Nonlinear Kinetic Theory of Cosmic-Ray Acceleration in Supernova Remnants". In Space Sciences Series of ISSI, 295–304. Dordrecht: Springer Netherlands, 2001. http://dx.doi.org/10.1007/978-94-017-3239-0_25.

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Trabalhos de conferências sobre o assunto "Cosmic-ray theory"

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MRIA, Luke Drury. "Galactic Cosmic Rays - Theory and Interpretation". In 35th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.301.1081.

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Petukhova, Anastasia, Ivan Petukhov e Stanislav Petukhov. "Theory of Forbush Decrease in a Magnetic Cloud". In 35th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.301.0122.

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Caprioli, Damiano, Colby Haggerty e Pasquale Blasi. "The Theory of Efficient Particle Acceleration at Shocks". In 37th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2021. http://dx.doi.org/10.22323/1.395.0482.

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Mertsch, Philipp, e Markus Ahlers. "Cosmic ray small-scale anisotropies in quasi-linear theory". In 36th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2019. http://dx.doi.org/10.22323/1.358.0105.

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Yan, Huirong. "Magnetohydrodynamic turbulence and propagation of cosmic rays: theory confronted with observations". In 37th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2021. http://dx.doi.org/10.22323/1.395.0038.

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Rebel, Heinrich gerhard. "High energy cosmic ray observations". In Twenty-sixth Johns Hopkins Workshop on current problems in particle theory: high energy reactions. Trieste, Italy: Sissa Medialab, 2002. http://dx.doi.org/10.22323/1.009.0010.

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7

Bottacini, Eugenio, Markus Böttcher, Elena Pian, Werner Collmar e Dario Gasparrini. "Challenges in reconciling observations and theory of the brightest high-energy flare ever of 3C 279". In 35th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2017. http://dx.doi.org/10.22323/1.301.0642.

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8

Ruffolo, David, T. Jitsuk, T. Pianpanit, A. P. Snodin, W. H. Matthaeus e P. Chuychai. "Random ballistic interpretation of the nonlinear guiding center theory of perpendicular transport". In The 34th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2016. http://dx.doi.org/10.22323/1.236.0197.

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9

Dorman, Lev, Lev Pustilnik e Elizabeth Petrov. "Influence of atmospheric electric field over NM on CR intensity: Observations on Mt. Hermon and comparison with theory". In 36th International Cosmic Ray Conference. Trieste, Italy: Sissa Medialab, 2019. http://dx.doi.org/10.22323/1.358.1106.

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10

Olinto, Angela V. "Ultra-high energy cosmic ray theory faces observational puzzles". In CENTENARY SYMPOSIUM 2012: DISCOVERY OF COSMIC RAYS. AIP, 2013. http://dx.doi.org/10.1063/1.4792569.

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Relatórios de organizações sobre o assunto "Cosmic-ray theory"

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Desilets, Darin. Radius of influence for a cosmic-ray soil moisture probe : theory and Monte Carlo simulations. Office of Scientific and Technical Information (OSTI), fevereiro de 2011. http://dx.doi.org/10.2172/1011220.

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