Relevant bibliographies by topics / Cosmic-ray transport

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  1. Dissertations / Theses

Academic literature on the topic 'Cosmic-ray transport'

Author: Grafiati
Published: 14 March 2023

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Dissertations / Theses on the topic "Cosmic-ray transport"

1

RECCHIA, SARAH. "Non linear cosmic ray transport and cosmic ray driven galactic winds." Doctoral thesis, Gran Sasso Science Institute, 2016. http://hdl.handle.net/20.500.12571/13501.

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The bulk of Cosmic Rays (CRs) reaching our planet is likely of Galactic origin and is thought to be accelerated in sources located in the Galactic disk (mainly Supernova remnants (SNRs)). The energy density of Galactic CRs, ∼ 1 eV/cm3, can be accounted for if one assumes that 3-10% of the mechanical energy injected by SNe in the Galaxy is channeled into accelerated particles. The observed large residence time of CRs in the Galaxy (compared to the time required for ballistic propagation of relativistic particles on Galactic distances) suggests that Galactic CRs are well coupled to the interste
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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 obser
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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 st
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4

Andreasen, Mie, Karsten H. Jensen, Marek Zreda, Darin Desilets, Heye Bogena, and Majken C. Looms. "Modeling cosmic ray neutron field measurements." AMER GEOPHYSICAL UNION, 2016. http://hdl.handle.net/10150/621996.

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The cosmic ray neutron method was developed for intermediate-scale soil moisture detection, but may potentially be used for other hydrological applications. The neutron signal of different hydrogen pools is poorly understood and separating them is difficult based on neutron measurements alone. Including neutron transport modeling may accommodate this shortcoming. However, measured and modeled neutrons are not directly comparable. Neither the scale nor energy ranges are equivalent, and the exact neutron energy sensitivity of the detectors is unknown. Here a methodology to enable comparability o
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5

Snyman, Jasper Lodewyk. "Modelling of the heliosphere and cosmic ray transport / Jasper L. Snyman." Thesis, North-West University, 2007. http://hdl.handle.net/10394/1814.

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Nkosi, Godfrey Sibusiso. "A study of cosmic ray anisotropies in the heliosphere / Godfrey Sibusiso Nkosi." Thesis, North-West University, 2006. http://hdl.handle.net/10394/1627.

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Nndanganeni, Rendani Rejoyce. "Modelling of galactic cosmic ray electrons in the heliosphere / Nndanganeni, R.R." Thesis, North-West University, 2012. http://hdl.handle.net/10394/7034.

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The Voyager 1 spacecraft is now about 25 AU beyond the heliospheric termination shock and soon it should encounter the outer boundary of the heliosphere, the heliopause. This is set to be at 120 AU in the modulation model used for this study. This implies that Voyager 1, and soon afterwards also Voyager 2, should be able to measure the heliopause spectrum, to be interpreted as the lowest possible local interstellar spectrum, for low energy galactic electrons (1 MeV to 120 MeV). This could give an answer to a long outstanding question about the spectral shape (energy dependence) of the galactic
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8

Tolksdorf, Tobias René [Verfasser], Reinhard [Gutachter] Schlickeiser, and Horst [Gutachter] Fichtner. "Cosmic ray transport in superbubbles / Tobias René Tolksdorf ; Gutachter: Reinhard Schlickeiser, Horst Fichtner ; Fakultät für Physik und Astronomie." Bochum : Ruhr-Universität Bochum, 2021. http://d-nb.info/1226429041/34.

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9

Ngobeni, Mabedle Donald. "Aspects of the modulation of cosmic rays in the outer heliosphere / by Mabedle Donald Ngobeni." Thesis, North-West University, 2006. http://hdl.handle.net/10394/97.

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A time-dependent two-dimensional (2D) modulation model including drifts, the solar wind tennination shock (TS) with diffusive shock acceleration and a heliosheath based on the Parker (1965) transport equation is used to study the modulation of galactic cosmic rays (GCRs) and the anomalous component of cosmic rays (ACRs) in the heliosphere. In particular, the latitude dependence of the TS compression ratio and injection efficiency of the ACRs (source strength) based on the hydrodynamic modeling results of Scherer et al. (2006) is used for the first time in a modulation model. The subsequent eff
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10

Cohet, Romain. "Transport des rayons cosmiques en turbulence magnétohydrodynamique." Thesis, Montpellier, 2015. http://www.theses.fr/2015MONTS051/document.

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Dans cette thèse, nous étudions les propriétés du transport de particules chargées de haute énergie dans des champs électromagnétiques turbulents.Ces champs ont été générés en utilisant le code magnétohydrodynamique (MHD) RAMSES, résolvant les équations de la MHD idéales compressibles. Nous avons développé un module pour générer la turbulence MHD, en utilisant une technique de forçage à grande échelle. Les propriétés des équations de la MHD font cascader l'énergie des grandes échelles vers les petites, développant un spectre en énergie suivant une loi de puissance, appelée zone inertielle. Nou
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