Дисертації з теми "Cosmic ray direct detection"
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WANG, ZHAOMIN. "Measurements of Cosmic Ray Proton + Helium flux with the DAMPE experiment." Doctoral thesis, Gran Sasso Science Institute, 2020. http://hdl.handle.net/20.500.12571/9942.
Повний текст джерелаReichhart, Lea. "ZEPLIN-III direct dark matter search : final results and measurements in support of next generation instruments." Thesis, University of Edinburgh, 2013. http://hdl.handle.net/1842/7914.
Повний текст джерелаMertsch, Philipp. "Cosmic ray backgrounds for dark matter indirect detection." Thesis, University of Oxford, 2010. http://ora.ox.ac.uk/objects/uuid:2734b849-4d7a-4266-8538-d3dc6cab6b20.
Повний текст джерелаHalverson, Peter Georges. "Detection of high-energy cosmic ray showers by atmospheric fluorescence." Diss., The University of Arizona, 1989. http://hdl.handle.net/10150/184779.
Повний текст джерела李耀華 and Yiu-wa Lee. "Investigation of cosmic ray intensity variation at primary rigidity above 1.7 TV." Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 1986. http://hub.hku.hk/bib/B42574079.
Повний текст джерелаLorek, Ryan James. "PIERRE AUGER OBSERVATORY AND TELESCOPEARRAY JOINT COSMIC RAY DETECTION, ANDCROSS CALIBRATION." Case Western Reserve University School of Graduate Studies / OhioLINK, 2019. http://rave.ohiolink.edu/etdc/view?acc_num=case155473314851704.
Повний текст джерелаMorris, Chad Michael. "Detection Techniques of Radio Emission from Ultra High Energy Cosmic Rays." The Ohio State University, 2009. http://rave.ohiolink.edu/etdc/view?acc_num=osu1254506832.
Повний текст джерелаIntaniwet, Akarin. "Semiconducting polymers for real time direct X-ray detection." Thesis, University of Surrey, 2011. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.538028.
Повний текст джерелаBloomer, Steven David. "The search for ultra high energy gamma ray emission from Cygnus X-3 and Hercules X-1." Thesis, University of Leeds, 1990. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.238644.
Повний текст джерелаLee, Yiu-wa. "Investigation of cosmic ray intensity variation at primary rigidity above 1.7 TV." Click to view the E-thesis via HKUTO, 1986. http://sunzi.lib.hku.hk/hkuto/record/B42574079.
Повний текст джерелаEdwards, Peter J. "A study of the muon content of EAS initiated by the UHE gamma-ray emission from Cygnus X-3." Thesis, University of Nottingham, 1990. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.238238.
Повний текст джерелаViberg, Fredrik. "Advanced algorithms for Ultra-High-Energy Cosmic Ray Detection with the EUSO-TA Experiment." Thesis, Luleå tekniska universitet, Institutionen för system- och rymdteknik, 2016. http://urn.kb.se/resolve?urn=urn:nbn:se:ltu:diva-313.
Повний текст джерелаCampbell, Mariam. "Cyclic universes & direct detection of cosmic expansion by holonomy in the McVittie spacetime." Master's thesis, Faculty of Science, 2019. http://hdl.handle.net/11427/31091.
Повний текст джерелаChen, Chuxing. "Local atmospheric electricity and its possible application in high-energy cosmic ray air shower detection." Diss., The University of Arizona, 1989. http://hdl.handle.net/10150/184799.
Повний текст джерелаRaspanti, Fabio. "Organic small molecules semiconductors as direct X-ray detectors." Bachelor's thesis, Alma Mater Studiorum - Università di Bologna, 2018. http://amslaurea.unibo.it/15451/.
Повний текст джерелаGiesen, Gaelle. "Dark Matter Indirect Detection with charged cosmic rays." Thesis, Paris 11, 2015. http://www.theses.fr/2015PA112160/document.
Повний текст джерелаOverwhelming evidence for the existence of Dark Matter (DM), in the form of an unknownparticle filling the galactic halos, originates from many observations in astrophysics and cosmology: its gravitational effects are apparent on galactic rotations, in galaxy clusters and in shaping the large scale structure of the Universe. On the other hand, a non-gravitational manifestation of its presence is yet to be unveiled. One of the most promising techniques is the one of indirect detection, aimed at identifying excesses in cosmic ray fluxes which could possibly be produced by DM annihilations or decays in the Milky Way halo. The current experimental efforts mainly focus in the GeV to TeV energy range, which is also where signals from WIMPs (Weakly Interacting Massive Particles) are expected. Focussing on charged cosmic rays, in particular antiprotons, electrons and positrons, as well as their secondary emissions, an analysis of current and forseen cosmic ray measurements and improvements on astrophysical models are presented. Antiproton data from PAMELA imposes contraints on annihilating and decaying DM which are similar to (or even slightly stronger than) the most stringent bounds from gamma ray experiments, even when kinetic energies below 10 GeV are discarded. However, choosing different sets of astrophysical parameters, in the form of propagation models and halo profiles, allows the contraints to span over one or two orders of magnitude. In order to exploit fully the power of antiprotons to constrain or discover DM, effects which were previously perceived as subleading turn out to be relevant especially for the analysis of the newly released AMS-02 data. In fact, including energy losses, diffusive reaccelleration and solar modulation can somewhat modify the current bounds, even at large DM masses. A wrong interpretation of the data may arise if they are not taken into account. Finally, using the updated proton and helium fluxes just released by the AMS-02 experiment, the astrophysical antiproton to proton ratio and its uncertainties are reevaluated and compared to the preliminarly reported AMS-02 measurements. No unambiguous evidence for a significant excess with respect to expectations is found. Yet, some preference for thicker halos and a flatter energy dependence of the diffusion coefficient starts to emerge. New stringed constraints on DM annihilation and decay are derived. Secondary emissions from electrons and positrons can also be used to constrain DM annihilation or decay in the galactic halo. The radio signal due to synchrotron radiation of electrons and positrons on the galactic magnetic field, gamma rays from bremsstrahlung processes on the galactic gas densities and from Inverse Compton scattering processes on the interstellar radiation field are considered. With several magnetic field configurations, propagation scenarios and improved gas density maps and interstellar radiation field, state-of-art tools allowing the computaion of synchrotron and bremssttrahlung radiation for any WIMP DM model are provided. All numerical results for DM are incorporated in the release of the Poor Particle Physicist Coookbook for DM Indirect Detection (PPPC4DMID). Finally, the possible GeV gamma-ray excess identified in the Fermi-LAT data from the Galactic Center in terms of DM annihilation, either in hadronic or leptonic channels is studied. In order to test this tantalizing interprestation, a multi-messenger approach is used: first, the computation of secondary emisison from DM with respect to previous works confirms it to be relevant for determining the DM spectrum in leptonic channels. Second, limits from antiprotons severely constrain the DM interpretation of the excess in the hadronic channel, for standard assumptions on the Galactic propagation parameters and solar modulation. However, they considerably relax if more conservative choices are adopted
Holt, Ewa Marlen [Verfasser], J. [Akademischer Betreuer] Blümer, and A. [Akademischer Betreuer] Etchegoyen. "Combined Detection of Muons and Radio Emission of Cosmic-Ray Air Showers / Ewa Marlen Holt ; Betreuer: J. Blümer , A. Etchegoyen." Karlsruhe : KIT-Bibliothek, 2018. http://d-nb.info/116100873X/34.
Повний текст джерелаAllison, Patrick S. "Design, calibration, and early results of a surface array for detection of ultrahigh energy cosmic rays." Columbus, Ohio : Ohio State University, 2007. http://rave.ohiolink.edu/etdc/view?acc%5Fnum=osu1179849363.
Повний текст джерелаShrestha, Shreetu [Verfasser], Christoph J. [Akademischer Betreuer] Brabec, and Rainer [Gutachter] Hock. "Methylammonium Lead Iodide Perovskite for Direct X-ray Detection / Shreetu Shrestha ; Gutachter: Rainer Hock ; Betreuer: Christoph J. Brabec." Erlangen : Friedrich-Alexander-Universität Erlangen-Nürnberg (FAU), 2018. http://d-nb.info/1172972362/34.
Повний текст джерелаFont, i. Serra Joan. "A journey of Ultra Heavy Cosmic Ray Nuclei with Z≥65: From their detection near the Earth neighborhood back to their nucleosynthesis sites." Doctoral thesis, Universitat Autònoma de Barcelona, 2004. http://hdl.handle.net/10803/3358.
Повний текст джерелаPrecisament el llegat d'aquests primers observadors del cel ha estat la curiositat per l'espai extraterrestre per buscar-hi respostes a diferents preguntes. Algunes d'aquestes preguntes, que han estat formulades per diversos científics, varen consistir en les llavors per a una nova disciplina cultivada en el camp de la ciència física: La física dels Raigs Còsmics.
Actualment, la física dels Raigs Còsmics consisteix en una disciplina que aixopluga diferents tòpics de l'astrofísica i la física com ara la nucleosíntesi dels raigs còsmics, el procés de injecció, els mecanismes d'acceleració, el procés de propagació i la detecció prop de la Terra dels raigs còsmics.
Durant els anys 80, es van planejar un conjunt d'experiències a bord de satèl·lits amb la finalitat d'estudiar la component hadrònica de la radiació còsmica, en concret, els ions ultrapesants amb càrrega superior a la del Ferro. El present treball està unit a un d'aquest experiments: l'UHCRE (Ultra Heavy Cosmic Ray Experiment). Varis apilaments de detectors sòlids de traces nuclears van ser usats en l'UHCRE. Aquests apilaments han estat analitzats i mesurats en el nostre grup, reconeixent un total de 205 traces originades per ions ultrapesants de la radiació còsmica. La identificació d'aquests ions en l'UHCRE ha estat la primera motivació d'aquest treball, així la primera meitat (capítols 1 i 2) d'aquesta tesi tracta aquest problema. D'altra banda, els capítols 3 i 4, concerneix el procés de propagació de l'abundància d'aquests ions cap a les seves fonts mitjançant el model de Leaky Box.
En el capítol 1, es presenta un mètode d'identificació conegut com Gradient Fraccional de la velocitat d'atac reduïda i es realitza un estudi detallat del seu rang d'aplicabilitat. Finalment, s'efectua la determinació de l'abundància dels raigs còsmics ultrapesants amb Z > 65 vistos per l'UHCRE.
En el capítol 2, s'utilitza un model alternatiu de formació de traça latent basat en el model de pèrdua d'energia restringida en el qual s'inclouen la possible contribució de les diferents correccions per col·lisions properes en l'equació de Bethe-Bloch. Un estudi prenent els resultats de l'UHCRE permet establir relacions entre els paràmetres que intervenen en el procés d'identificació. Finalment, s'obté una estimació d'aquests paràmetres usant dades experimentals d'accelerador.
En el capítol 3, es dedueix l'equació de transport pel model de Leaky Box (MLB) que descriu la variació de la composició química de la radiació còsmica durant el seu viatge a través de la galàxia. L'abundància en les fonts que es dedueix dels resultats de l'UHCRE és estimada resolent les equacions de transport per a tots els elements amb càrrega entre 65 i 92 mitjançant un mètode numèric que cal entendre'l com una primera aproximació al problema.
En el darrer capítol, les equacions del MLB es resolen numèricament usant la Weighted Slab Technique. Es presenta un estudi de la resposta d'aquest model quan es varien les expressions dels diferents paràmetres de propagació que es requereixen. Optimitzant el paràmetre estadístic χ² entre l'abundància calculada la qual és afectada per una indeterminació en la càrrega i l'abundància experimental, ah estat possible determinar aquella combinació de totes les expressions disponibles dels paràmetres de propagació que millor reprodueix l'abundància experimental de l'UHCRE.
Since ancient times, from the beginning of humankind, human beings have shown a great curiosity and attraction for what they saw when looking up. For one reason or another, the quest for explanations of mystical nature (maybe justifications) for what surrounded human life as well as its destiny was searched outside the Earth. This mystical interest encouraged the observation of the night sky which, in time, together with other social and philosophical changes, lead to a rational interpretation of what they observed and, hence the formulation of the first cosmogonical models and then cosmological models.
Precisely, the legacy of these first sky observers, has been the curiosity for the extraterrestial space in search of answers to many different questions. Some of these questions formulated by several scientists, were the seeds for a new discipline sowed in the field of physics science: Cosmic Ray Physics.
Nowadays, Cosmic Ray Physics consist on a discipline allowing to gather several different topics of astrophysics and physics such as the nucleosynthesis of cosmic rays, the injection process, the acceleration mechanisms, the propagation process and the detection of cosmic rays near the Earth.
During the 80's, a set of experiences on board of satellites were planned and carried out with the aim of studying the hadronic component of cosmic rays, specifically ultra heavy ions with charge higher than Iron. The present work is, therefore, linked to one of such experiences; the UHCRE (Ultra Heavy Cosmic Ray Experiment). Several stacks of sheets of solid state nuclear track detectors used in the UHCRE have been analysed and measured by our group, recognizing a total of 205 tracks as originated by ultra heavy cosmic ray ions. The identification of cosmic ray ions recorded in UHCRE has been the first motivation of this work, so the first half (chapter 1 and 2) of the present thesis deals with this problem. On the other hand, chapters 3 and 4 concern to the propagation process of the abundances of such ions back to their sources using the Leaky Box model.
In chapter one, an identification method, known as Reduced Etch Rate Fractional Gradient (RERFG) is presented and a detailed study of its range of applicability is performed. The determination of the abundances of ultra heavy cosmic ray with Z > 65 seen by the UHCRE is realized.
In the second chapter, an alternative track formation model based on a modification of the Restricted Energy Loss model is taken into consideration by introducing the contribution of the close collisions corrections in the Bethe-Bloch formula. A study taking the UHCRE measurements allows to establish relationships between the parameters involved in the identification process. Finally, an estimation of these parameters is made using experimental data from accelerator.
In chapter three, the transport equation for the Leaky Box Model (LBM) which describes the variation of the chemical composition of cosmic rays during their travel through the Galaxy is deduced. The source abundances inferred from the UHCRE results are estimated solving the transport equations, corresponding to all elements with charge 65 < Z < 92, with a numerical method that has to be understood as a first approximation to the problem.
In the last chapter, the LBM transport equations are numerically solved using the Weighted Slab Technique. A study of the response of the LBM is presented when different expressions of the required propagation parameters are taken. By optimizing the χ² statistical parameter between calculated abundances which are effected by a charge uncertainty and experimental abundances, it has been possible to determine which combination of all available expressions of the propagation parameters better reproduces the experimental abunadances of UHCRE.
Porelli, Andrea. "TAIGA-HiSCORE: a new wide-angle air Cherenkov detector for multi-TeV gamma-astronomy and cosmic ray physics." Doctoral thesis, Humboldt-Universität zu Berlin, 2020. http://dx.doi.org/10.18452/21610.
Повний текст джерелаThe TAIGA (Tunka Advanced Instrument for cosmic ray physics and Gamma Astronomy) detector is a new ground-based Cherenkov detection technology for gamma-astronomy from 10TeV up to several PeV, and cosmic rays (CR) above 100TeV. The main topic of this work is TAIGA-HiSCORE, the wide-aperture air Cherenkov timing array. The focus is on precision extensive air shower (EAS) arrival direction reconstruction, achieved by (1) sub-nsec time-synchronization between the array stations, and (2) a newly developed array time calibration procedure. The performance is verified using simulated and experimental data from EAS, dedicated LED calibration, and a LIDAR laser beam from the International Space Station (ISS). The analysis of the HiSCORE 9 data (2013-14), collected with a data acquisition system (DAQ) based on the White Rabbit (WR) timing system, allows to verify the sub-nsec time synchronization between the array stations. The analysis of HiSCORE 28 data (2015-2018) addresses the problem of achieving an easy-to-perform time calibration for large area ground-based Cherenkov array. A new "hybrid" calibration method is developed, which makes use of EAS data, and requires direct LED calibration of only a few array stations. The "chessboard" method is applied on the reconstructed data to obtain a MC-independent estimation of the detector angular resolution, found to be 0.4° at threshold (~50TeV) and <= 0.2° above 100TeV. A serendipitous discovery was made in this work: a signal from the CATS-LIDAR on-board the ISS was found in the HiSCORE 28 data. These "ISS-events" are used to verify the detector performance, in particular the absolute angular pointing (<= 0.1°), particularly important since a strong gamma point source has not yet been detected by the TAIGA-HiSCORE. The final part of the work presents a first preliminary approach to a wide aperture point source analysis, developed for the TAIGA-HiSCORE in stand-alone operation.
El, Aisati Chaimae. "Gamma-ray and Neutrino Lines from Dark Matter: multi-messenger and dedicated smoking-gun searches." Doctoral thesis, Universite Libre de Bruxelles, 2018. http://hdl.handle.net/2013/ULB-DIPOT:oai:dipot.ulb.ac.be:2013/266180.
Повний текст джерелаOption Physique du Doctorat en Sciences
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Hofmann, Florian [Verfasser], and Kirpal [Akademischer Betreuer] Nandra. "Turbulence and direct dark matter detection in the X-ray halo of galaxy clusters : implications for eROSITA / Florian Hofmann ; Betreuer: Kirpal Nandra." München : Universitätsbibliothek der Ludwig-Maximilians-Universität, 2016. http://d-nb.info/1120302129/34.
Повний текст джерелаLagage, Pierre-Olivier. "Acceleration et propagation des rayons cosmiques : production, oscillations et detection de neutrinos." Paris 7, 1987. http://www.theses.fr/1987PA077124.
Повний текст джерелаJung, Aera. "JEM-EUSO prototypes for the detection of ultra-high-energy cosmic rays (UHECRs) : from the electronics of the photo-detection module (PDM) to the operation and data analysis of two pathnders." Thesis, Sorbonne Paris Cité, 2017. http://www.theses.fr/2017USPCC108/document.
Повний текст джерелаThe JEM-EUSO (Extreme Universe Space Observatory on-board the Japanese Experiment Module) international space mission is designed to observe UHECRs by detecting the UV fluorescence light emitted by the so-called Extensive Air Shower (EAS) which develop when UHECRs interact with the Earth’s atmosphere. The showers consist of tens of billions or more secondary particles crossing the atmosphere at nearly the speed of light, which excite nitrogen molecules which then emit light in the UV range. While this so-called “fluorescence technique'” is routinely used from the ground, by operating from space, JEM-EUSO will, for the first time, provide high-statistics on these events. Operating from space, with a large Field-of-View of ±30 °, allows JEM-EUSO to observe a much larger volume of atmosphere, than possible from the ground, collecting an unprecedented number of UHECR events at the highest energies.For the four pathfinder experiments built within the collaboration, we have been developing a common set of electronics, in particular the central data acquisition system, capable of operating from the ground, high altitude balloons, and space.These pathfinder experiments all use a detector consisting of one Photo-detection Modules (PDMs) identical to the 137 that will be present on the JEM-EUSO focal surface. UV light generated by high-energy particle air showers passes the UV filter and impacts the Multi-anode Photomultiplier Tubes (MAPMT). Here UV photons are converted into electrons, which are multiplied by the MAPMTs and fed into Elementary Cell Application-Specific Integrated Circuit (EC-ASIC) boards, which perform the photon counting and charge estimation. The PDM control board interfaces with these ASIC boards, providing power and configuration parameters, collecting data and performing the level 1 trigger. I was in charge of designing, developing, integrating, and testing the PDM control board for the EUSO-TA and EUSO-Balloon missions as well as the autonomous trigger algorithm testing and I also performed some analysis of the EUSO-Balloon flight data and data from the EUSO-TA October 2015 run.In this thesis, I will give a short overview of high-energy cosmic rays, including their detection technique and the leading experiments (Chapter 1), describe JEM-EUSO and its pathfinders including a description of each instrument (Chapter 2), present the details of the design and the fabrication of the PDM (Chapter 3) and PDM control board (Chapter 4), as well as the EUSO-TA and EUSO-Balloon integration tests (Chapter 5). I will report on the EUSO-Balloon campaign (Chapter 6) and results (Chapter 7), including a specific analysis developed to search for global variations of the ground UV emissivity, and apply a similar analysis to data collected at the site of Telescope Array (Chapter 8). Finally, I will present the implementation and testing of the first-level trigger (L1) within the FPGA of the PDM control board (Chapter 9). A short summary of the thesis will be given in Chapter 10
Cratere, Angela. "Prospects for future observations of off-axis short gamma-ray burst jets associated with binary neutron star mergers." Master's thesis, Alma Mater Studiorum - Università di Bologna, 2021.
Знайти повний текст джерелаLundberg, Johan. "On the Search for High-Energy Neutrinos : Analysis of data from AMANDA-II." Doctoral thesis, Uppsala University, Department of Physics and Astronomy, 2008. http://urn.kb.se/resolve?urn=urn:nbn:se:uu:diva-8906.
Повний текст джерелаA search for a diffuse flux of cosmic neutrinos with energies in excess of 1014 eV was performed using two years of AMANDA-II data, collected in 2003 and 2004. A 20% evenly distributed sub-sample of experimental data was used to verify the detector description and the analysis cuts. A very good agreement between this 20% sample and the background simulations was observed. The analysis was optimised for discovery, to a relatively low price in limit setting power. The background estimate for the livetime of the examined 80% sample is 0.035 ± 68% events with an additional 41% systematical uncertainty.
The total neutrino flux needed for a 5σ discovery to be made with 50% probability was estimated to 3.4 ∙ 10-7 E-2 GeV s-1 sr-1 cm-2 equally distributed over the three flavours, taking statistical and systematic uncertainties in the background expectation and the signal efficiency into account. No experimental events survived the final discriminator cut. Hence, no ultra-high energy neutrino candidates were found in the examined sample. A 90% upper limit is placed on the total ultra-high energy neutrino flux at 2.8 ∙ 10-7 E-2 GeV s-1 sr-1 cm-2, taking both systematical and statistical uncertainties into account. The energy range in which 90% of the simulated E-2 signal is contained is 2.94 ∙ 1014 eV to 1.54 ∙ 1018 eV (central interval), assuming an equal distribution over the neutrino flavours at the Earth. The final acceptance is distributed as 48% electron neutrinos, 27% muon neutrinos, and 25% tau neutrinos.
A set of models for the production of neutrinos in active galactic nuclei that predict spectra deviating from E-2 was excluded.
Halliday, Robert Paul. "Electronics and Timing for the AugerPrime Upgrade and Correlation of Starburst Galaxies with Arrival Directions of Ultra High Energy Cosmic Rays." Case Western Reserve University School of Graduate Studies / OhioLINK, 2019. http://rave.ohiolink.edu/etdc/view?acc_num=case1553599216169462.
Повний текст джерелаKéfélian, Cécile. "Search for dark matter with EDELWEISS-III excluding background from muon-induced neutrons." Thesis, Lyon, 2016. http://www.theses.fr/2016LYSE1020/document.
Повний текст джерелаThe aim of the EDELWEISS-III experiment is to detect the elastic scattering of WIMPs from the galactic dark matter halo on germanium bolometers. The most problematic background arises from neutrons, which can mimic a WIMP interaction in a detector. Neutrons are notably induced by high energy cosmic ray muons reaching the underground laboratory despite the 4800 m w.e. of rock overburdened. Remaining muons are tagged using an active muon-veto system of 46 plastic scintillator modules surrounding the experiment, which allows to reject most of the associated background. The goal of this thesis was to give a precise estimation of the irreducible muon-induced neutron background, needed to identify a potential WIMP signal. The expected background depends on the geometry of the experiment as well as on the used materials, both strongly modified since EDELWEISS-II. Geant4-based simulations of muons through the modified geometry were performed to derive the rate of events induced by muons in the bolometer array. This rate has been shown to be in good agreement with the measured one extracted from the Run308 data. In parallel, a lower limit on the muon-veto efficiency was derived using bolometer data only. A new method based on an AmBe source was developed to extract precisely the detection efficiency of individual modules from the simulation. From these results, it was shown that the expected background is negligible for the WIMP search analyses performed with the Run308 data and won't limit the future sensitivity of the EDELWEISS-III experiment
Yeh, Chun Chao, and 葉俊昭. "Detection on Cosmic-Ray Neutron." Thesis, 1994. http://ndltd.ncl.edu.tw/handle/62691931923881036816.
Повний текст джерелаO'Connor, Daniel Joseph. "Cosmic ray muons in the deep ocean." Thesis, 1990. http://hdl.handle.net/10125/10074.
Повний текст джерелаJames, Clancy William. "Ultra-high energy particle detection with the lunar Cherenkov technique." 2009. http://hdl.handle.net/2440/57706.
Повний текст джерелаhttp://proxy.library.adelaide.edu.au/login?url= http://library.adelaide.edu.au/cgi-bin/Pwebrecon.cgi?BBID=1371947
Thesis (Ph.D.) - University of Adelaide, School of Chemistry and Physics, 2009.
James, Clancy William. "Ultra-high energy particle detection with the lunar Cherenkov technique." Thesis, 2009. http://hdl.handle.net/2440/57706.
Повний текст джерелаThesis (Ph.D.) - University of Adelaide, School of Chemistry and Physics, 2009.
Pereira, Maria Elias Lopes. "Characterization of direct X-ray Detectors based on Organic Semiconductor thin films." Master's thesis, 2018. http://hdl.handle.net/10362/130841.
Повний текст джерелаA deteção de radiação ionizante, como os raios-X, é uma área de pesquisa em constante crescimento, graças aos seus vastos campos de aplicação, que abrangem desde a astrofísica, centrais nucleares, segurança industrial e civil, até ao diagnóstico médico. Neste projeto, realizado na Universidade de Bolonha, no departamento de física, um dos grupos de investigação mais ativos nesta área, quatro mo-léculas diferentes (TIPS, TIPGe, diF TES ADT e diF TEG ADT) foram estudadas na forma de filme fino orgânico semicondutor num fotocondutor. Os dispositivos foram preparados através da deposição por drop-casting de uma solução destas moléculas em três substratos (PET, PEN e vidro), para uma abordagem direta na deteção desta radiação. A influência de diferentes parâmetros, como a resistividade, percentagem de área ativa coberta pela molécula, quantidade e espessura dos cristais, foi investigada quanto ao desempenho dos detetores de raios-X. Descobriu-se que, no substrato PET, há um processo de descarga que parece ser importante para o desempenho do detetor e que aparentemente induz uma diminuição na corrente dos dispositivos base-ados em diF TES ADT e diF TEG ADT, tornando-os inadequados para qualquer tipo de aplicação. Com o substrato PEN, é possível obter dispositivos fiáveis e reprodutíveis com baixo ruído e sensibilidades aceitáveis. O substrato de vidro com o TIPGe daria o melhor dispositivo porque combina uma alta sensibilidade com um dispositivo fiável e reprodutível. No entanto, não é um substrato flexível e, portanto, não é adequado para muitas das aplicações de interesse, como por exemplo, aplicações de diagnóstico de saúde, como a dosimetria pessoal. Finalmente, ficou provado que as moléculas com o elemento germânio apresentam, como esperado pelo seu número atómico mais elevado que o do silício, as mais altas sensibilidades. Descobriu-se, ainda, que isso também se deve aos cristais de alta qualidade obtidos nessas moléculas. Em função dos resultados obtidos, a linha de investigação parece profícua, esperando-se aplicações práticas muito interessantes.
Hadji, Bahman. "Evaluation of a Direct Detection Selenium-CMOS 8×8 Passive Pixel Sensor Array for Digital X-Ray Imaging Applications." Thesis, 2010. http://hdl.handle.net/10012/5130.
Повний текст джерела