Tesis sobre el tema "Cosmic ray detections"
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李耀華 y 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.
Texto completoMertsch, 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.
Texto completoBloomer, 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.
Texto completoMorris, 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.
Texto completoHalverson, Peter Georges. "Detection of high-energy cosmic ray showers by atmospheric fluorescence". Diss., The University of Arizona, 1989. http://hdl.handle.net/10150/184779.
Texto completoAllison, 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.
Texto completoLee, 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.
Texto completoLorek, 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.
Texto completoEdwards, 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.
Texto completoGiesen, Gaelle. "Dark Matter Indirect Detection with charged cosmic rays". Thesis, Paris 11, 2015. http://www.theses.fr/2015PA112160/document.
Texto completoOverwhelming 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
Barley, Steven Keith. "Investigation of the muon component of EAS initiated by primary radiation from Hercules X-1". Thesis, University of Nottingham, 1990. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.238221.
Texto completoWilliamson, Alexander. "Detecting Cosmic Rays with the Murchison Widefield Array". Thesis, Curtin University, 2021. http://hdl.handle.net/20.500.11937/87686.
Texto completoWANG, 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.
Texto completoChen, 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.
Texto completoKwok, Talent. "A study of background radiation and cosmic muon detection at the Aberdeen Tunnel laboratory in Hong Kong". Click to view the E-thesis via HKUTO, 2007. http://sunzi.lib.hku.hk/hkuto/record/B38819971.
Texto completoKwok, Talent y 郭天能. "A study of background radiation and cosmic muon detection at the Aberdeen Tunnel laboratory in Hong Kong". Thesis, The University of Hong Kong (Pokfulam, Hong Kong), 2007. http://hub.hku.hk/bib/B38819971.
Texto completoDelahaye, Timur. "Propagation of galactic cosmic rays and dark matter indirect detection". Chambéry, 2010. http://www.theses.fr/2010CHAMS019.
Texto completoThis thesis is dedicated to the study of propagation of cosmic electrons and positrons in the Milky Way and to the indirect detection of dark matter. The existence of dark matter is a hypothesis considered as reasonable from the point of view of cosmology, astrophysics and even particle physics. Nevertheless its detection still eludes us and it is not possible to verify this hypothesis by other means than gravitational one. A possible way to detect dark matter is to look for its annihilation or decay products among Galactic cosmic rays. During the last three years, data concerning cosmic ray electrons and positrons have been accumulated and have reached a remarkable precision. Such a precision requires from us to refine the theoretical models and to quantify the errors. This thesis addresses the study of all the sources of uncertainties affecting predictions of cosmic electrons and positron fluxes, primary and secondary, classical or from exotic origin. The greatest care has been dedicated to the sources and the propagation in the Galactic halo. Moreover a study of gamma and radio emissions associated to these cosmic rays is presented, again with the will of sizing uncertainties. Finally a status of the research for detection of annihilation or decay of Galactic dark matter is presented
Viberg, 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.
Texto completoBlackwell, Timothy Benjamin. "The use of cosmic-rays in detecting illicit nuclear materials". Thesis, University of Sheffield, 2015. http://etheses.whiterose.ac.uk/10432/.
Texto completoEl, 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.
Texto completoOption Physique du Doctorat en Sciences
info:eu-repo/semantics/nonPublished
MacRae, John Hamish Kenneth. "The detection of very high energy cosmic gamma rays using the atmospheric Cerenkov technique". Thesis, Durham University, 1985. http://etheses.dur.ac.uk/7854/.
Texto completoGate, Florian Sylvain. "Estimation of the composition of cosmic rays using the radio signal". Thesis, Nantes, Ecole des Mines, 2016. http://www.theses.fr/2016EMNA0295/document.
Texto completoMore than a century after their discovery, cosmic-raysare still puzzling physicists. The flux of these particlescoming from extraterrestrial sources strongly decreasesas a function of their energy. Above 1 PeV (10¹⁵ eV), theparticle flux becomes too low to allow a direct detectionon a reasonable time scale. However, the cascades ofsecondary particles produced after the interaction ofcosmic-rays with the constituents of the atmosphere aredetectable at the ground level; it is the indirect detection.Above 100 PeV, the number of observations is too lowto accurately estimate the mass of the cosmic rays andthen to constrain the prediction models of accelerationmechanisms, propagation and type of sources. Thedetermination of their composition is achieved at thePierre Auger Observatory using fluorescencetelescopes from the measurement of the Xmaxobservable with a duty cycle of 14%. Xmax, defined asthe atmosphere depth at which the number ofsecondary particles reaches its maximal value, is highlycorrelated to the mass of the cosmic ray that hascreated the air shower. A large number of observationsis required for a precise estimation of the mass as theXmax statistical fluctuations are important. The radiodetection is a perfect alternative to the fluorescencemethod as the duty cycle of a typical radio detector isclose to 100%. This thesis proposes a method toestimate the mass of ultra-high energy cosmic raysusing only the radio signals and their simulation. Thegoal is to systematically reconstruct the Xmax depth ofeach air shower detected by the AERA experimentwithin the site of the Pierre Auger Observatory inArgentina. The influence of the description of theatmosphere on the reconstructed shower parameters, inthe SELFAS code, has been studied. It includes thegeometry of the atmospheric layers, the way to calculatethe air refractive index and density, as well as their dailyand seasonal fluctuations
Lundberg, 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.
Texto completoA 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.
Holt, Ewa Marlen [Verfasser], J. [Akademischer Betreuer] Blümer y 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.
Texto completoGriffith, Nathan E. "Microwave Detection of Cosmic Rays and Multi-Messenger Analysis of the Parameters of Ultra-High Energy Astrophysical Sources". The Ohio State University, 2015. http://rave.ohiolink.edu/etdc/view?acc_num=osu1429799044.
Texto completoPorelli, 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.
Texto completoThe 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.
Font, 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.
Texto completoPrecisament 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.
Fenu, Francesco [Verfasser] y Andrea [Akademischer Betreuer] Santangelo. "A Simulation Study of the JEM-EUSO Mission for the Detection of Ultra-High Energy Cosmic Rays / Francesco Fenu ; Betreuer: Andrea Santangelo". Tübingen : Universitätsbibliothek Tübingen, 2013. http://d-nb.info/1162896736/34.
Texto completoLagage, Pierre-Olivier. "Acceleration et propagation des rayons cosmiques : production, oscillations et detection de neutrinos". Paris 7, 1987. http://www.theses.fr/1987PA077124.
Texto completoKönig, Hampus. "Evaluation of detector Mini-EUSO to study Ultra High-Energy Cosmic Rays and Ultra Violet light emissions observing from the International Space Station". Thesis, Luleå tekniska universitet, Institutionen för system- och rymdteknik, 2019. http://urn.kb.se/resolve?urn=urn:nbn:se:ltu:diva-72552.
Texto completoToni, Greta. "Detection and characterization of galaxy clusters in the COSMOS field with the AMICO algorithm". Master's thesis, Alma Mater Studiorum - Università di Bologna, 2022. http://amslaurea.unibo.it/25229/.
Texto completoJung, 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.
Texto completoThe 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.
Buscar texto completoHalliday, 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.
Texto completoZimmermann, Benedikt Hermann [Verfasser] y M. [Akademischer Betreuer] Weber. "Radio-detection of ultra-high energy cosmic rays: multi-channel data acquisition and combined analysis of timing and energy information / Benedikt Hermann Zimmermann ; Betreuer: M. Weber". Karlsruhe : KIT-Bibliothek, 2017. http://d-nb.info/1143026993/34.
Texto completoPainter, William [Verfasser] y J. [Akademischer Betreuer] Blümer. "Development of a SiPM camera for detection and measurement of fluorescence emission from extensive air-showers generated by ultra high energy cosmic rays / William Painter ; Betreuer: J. Blümer". Karlsruhe : KIT-Bibliothek, 2019. http://d-nb.info/1197138757/34.
Texto completoMaller, Jennifer. "Caractérisation de signaux transitoires radio à l'observatoire Pierre Auger". Thesis, Nantes, Ecole des Mines, 2014. http://www.theses.fr/2014EMNA0186/document.
Texto completoAfter more than a century of studies, one of the challenging questions related to ultra-high energy cosmic rays concerns their nature, which remains unclear. Improving the knowledge about the composition of cosmic rays will permit to constrain the models concerning their origins and the production mechanisms in the astrophysical sources. Simulations show that, the electric field emitted by the shower is sensitive to its development. This electric-field can be measured with a high duty cycle, and thus is apromising technique to identify an observable sensitive to the nature of the primary cosmic ray. The radio signal is also used to measure its arrival direction and its energy. Since 2006, the Pierre Auger Observatory hosts several radio detection arrays of cosmic rays, starting from small size prototypes (RAuger, MAXIMA) to achieve a large scale array of 124 radio stations: AERA, the Auger Engineering Radio Array covering 6 km². These different arrays allow the study of the radio emission during the development of the shower in the MHz domain. AERA is deployed in the low energy extension of the Pierre Auger Observatory in order to have a larger statistics. It enables interesting hybrid measurements, with the comparison of radio observable with those obtained with the surface detector (SD) and the fluorescence telescopes close to the array. This thesis is dedicated to the characterization of the radio transient signals detected by RAuger and AERA. As one of the challenges of the radio detection of air-shower is to remove the anthropic background causing accidental triggering, methods for background rejection and SD-AERA coincidences selection have been developed. A study of the correlation between the shower development in the atmosphere (longitudinal profile) and the electric-field measured by the radio stations is also presented. This study shows the relationship between the electric-field and the shower development in the atmosphere and confirms that the radio signal is a powerful tool to study the nature of the ultra-high energy cosmic rays
Taoso, Marco. "Particle dark matter and astrophysical constraints". Doctoral thesis, Università degli studi di Padova, 2009. http://hdl.handle.net/11577/3426084.
Texto completoL'esistenza di Materia Oscura non-barionica è provata da numerose osservazioni astrofisiche e cosmologiche. Tracce della sua presenza si trovano a scale molto diverse, dai sistemi galattici e sub-galattici alle strutture a larga scale e alle scale cosmologiche. Nonostante queste molteplici osservazioni, la natura della Materia Oscura è ancora ignota. In questo lavoro di tesi abbiamo studiato le prospettive per la rivelazione di Materia Oscura attraverso osservazioni astrofisiche.
Escudie, Antony. "From the observation of UHECR signal in [1-200] MHz to the composition with the CODALEMA and EXTASIS experiments". Thesis, Ecole nationale supérieure Mines-Télécom Atlantique Bretagne Pays de la Loire, 2019. http://www.theses.fr/2019IMTA0145/document.
Texto completoDespite the discovery of cosmic rays there are more than one hundred years ago, many questions remain unanswered today: what are cosmic rays, how are they created and where do they come from ? Since 2002, the CODALEMA instrument, located within the Nançay Radio Observatory, studies the ultra-high energy cosmic rays (UHECR, above 1017 eV) arriving in the Earth atmosphere. Their low flux makes it impossible to detect them directly at these energies. These cosmic rays, however, will interact with the atoms of the atmosphere, generating a cascade of secondary charged particles, commonly known as extensive air shower (EAS), detectable at ground level, and from which we will extract information on the primary cosmic ray. The objective is to go back to the characteristics of the primary that generated the EAS, thus to determine its direction of arrival, its nature and its energy. During the development of the shower, these charged particles in movement generate a fast electric field transient, detected at ground by CODALEMA with dedicated radio antennas over a wide frequency band (between 1 and 200 MHz). The major advantage of radio-detection is its sensibility to the whole profile of the shower and its duty cycle close to 100 %, which could increase the number of events detected at very high energy, and thus to better constrain the properties of the RCUHE. Over the years, significant efforts have been devoted to the understanding of the radio emission of extensive air shower (EAS) in the range [20-80] MHz but, despite some studies led until the nineties, the[1-10] MHz band has remained unused for nearly 30 years. One of the contributions of this thesis concerns the EXTASIS experiment, supported by the CODALEMA instrument, which aims to reinvestigate the [1-10] MHz band and to study the so-called ”sudden death” contribution, which is the expected impulsive electric field created by the particles at their arrival and their disappearance on the ground. We present the instrumental set up of EXTASIS, composed of 7 low frequency antennas exploited in [1.7-3.7] MHz, covering approximately 1 km2. We report the observation, over 2 years, of 25 low-frequency events detected in coincidence by CODALEMA and EXTASIS and estimate a detection limit of 23±4 μV/m from comparisons with simulations. We also report a strong correlation between the observation of the low frequency signal and the atmospheric electric field. The other major contribution of this thesis concerns the study of the electric field emitted by the EAS and the improvement of the detector’s performances in the [20-200] MHz band. First, we propose a calibration method for CODALEMA antennas using the radio emission of the Galaxy. We are also investigating several noise rejection algorithms to improve the selectivity of recorded events. We then present a method for reconstructing the parameters of the primary cosmic ray, implementing systematic comparisons combing polarization and frequency information between the recorded data and simulations, leading finally to a proposal for a mass composition of cosmic rays detected
Machado, Laura Paulucci. "Matéria de quarks (strangelets) de origem astrofísica e sua detecção por experimentos terrestres". Universidade de São Paulo, 2008. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-26112008-100951/.
Texto completoThe strange quark matter hypothesis, which states that a plasma composed of quarks up, down and strange in roughly equal amounts is absolutely stable at zero pressure, has been studied for more than twenty years, both theoretically and during searches for its detection in specific experiments. If strange quark matter is indeed stable, then there could be important implications for the field of Astrophysics. Among the most stimulating ones is the possibility of conversion of ordinary nuclear matter in strange quark matter in the interior of neutron stars due to the extremely high densities reached in the core of these compact objects. Processes such as the merger in neutron star binaries systems and supernovae themselves, responsible for the birth of these stars, may eject lumps of strange quark matter, termed strangelets, in the interstellar medium. In this way, strangelets may be present among the cosmic ray flux and be subjected to elementary processes much in the same way as ordinary nuclei. In this Thesis, strangelets are studied from their likely astrophysical production sites, passing through the interstellar medium until they reach the Earth neighborhood. Estimates of the low energy flux of strangelets that could be trapped in the terrestrial magnetosphere are given. Also, the interaction of these particles with components in the Earth atmosphere are studied with the aim of providing better understanding of the resulting observational signatures. It allows the determination of the relevant characteristics for the identification of these exotics by experiments testing the cosmic ray flux, helping to better understand the properties of nuclear matter at high densities and low temperatures.
Taoso, Marco. "Particle dark matter and astrophysical constraints". Doctoral thesis, Paris 7, 2009. http://www.theses.fr/2009PA077262.
Texto completoNumerous astrophysical and cosmological observations support the existence of non-baryonic Dark Matter in the Universe. Its presence is well established at different scales, from galaxies to large scale structures and cosmological scales. However, despite the numerous and independent evidences, the nature of Dark Matter in not yet understood. Among the large number of Dark Matter candidates proposed in literature, Weakly Interacting Massive Particles (WIMPs) are the most popular. In this thesis we study the prospect for indirect detection of WIMPs. We first focus on searches of large DM overdensities around Intermediate Mass Black Holes with gamma-ray experiments. We then consider DM searches in the antimatter cosmic-ray fluxes and finally we study the impact of WIMPs annihilations in the evolution of the first stars
Martraire, Diane. "Étude du pouvoir de discrimination des primaires initiant les grandes gerbes atmosphériques avec des réseaux de détecteurs au sol : analyse des rayons cosmiques de ultra haute énergie détectés à l’observatoire Pierre Auger, Estimation des performances pour la detection de gamma de très haute énergie du future observatoire LHAASO". Thesis, Paris 11, 2014. http://www.theses.fr/2014PA112276/document.
Texto completoDuring the past century, ultra-high-energy cosmic rays (UHECR), those with an energy larger than 1018 eV, remain as a mystery: What are cosmic rays? Where do they come from? How do they attain their huge energy? When these charged particles strike the earth's atmosphere, they dissipate their energy by generating a shower of secondary particles whose development is significantly different depending on the nature of the primaries. The Pierre Auger observatory, with its hybrid structure and huge size network of ground detectors, can shed some light into these questions.The study of the composition of UHECR was performed with the Pierre Auger apparatus. This is crucial both to understand the hadronic interactions, which govern the evolution of showers, and to identify their sources. It can help to understand the origin of the energy spectrum cut-off: is it the GZK cut-off or the exhaustion of sources? These reasons motivate the first part of this thesis: the development of a method to extract the muonic component of air showers and deduce the implications on the composition of UHECR at the Pierre Auger observatory. The results of this method show a dependence of the composition with the distance to the axis of the shower, which could help to improve the hadronic models. The determination of the muon component is limited by the surface detector setup.The second part is devoted to the new observatory in China, LHAASO. This project focuses on the study of gamma rays with an energy higher than 30 TeV, which probe the acceleration of protons in the galaxy, providing indirect information on cosmic rays. Moreover, the observatory studies cosmic rays between 10 TeV and 1 EeV, one of the regions where the energy spectrum presents a break. This region requires the ability to discriminate gamma rays and cosmic rays. For this reason, one of the detectors of LHAASO, the KM2A, was simulated and its power of discrimination gamma/hadron evaluated
Yeh, Chun Chao y 葉俊昭. "Detection on Cosmic-Ray Neutron". Thesis, 1994. http://ndltd.ncl.edu.tw/handle/62691931923881036816.
Texto completoO'Connor, Daniel Joseph. "Cosmic ray muons in the deep ocean". Thesis, 1990. http://hdl.handle.net/10125/10074.
Texto completoHsu, Shih-Ying y 許世穎. "Studies of the Radio Wave Detection of Cosmic Rays and Cosmic Neutrinos for TAROGE and ANITA". Thesis, 2016. http://ndltd.ncl.edu.tw/handle/57504740617599111809.
Texto completo國立臺灣大學
物理學研究所
104
The detection of the ultra high energy cosmic rays (UHECRs) and the cosmic neutrinos has been studied for ages. In the past decades, the use of radio frequency waves (RF) to detect UHE cosmic rays an neutrinos has advanced significantly. ANtarctic Impulse Transient Antenna (ANITA) is a balloon-borne observatory. It searches for the RF emissions induced by the Askaryan effect when cosmic neutrinos interact with the ice and the ice-reflected signals emitted from the air showers induced by UHECRs. With the enormous harvest from its two flights, ANITA took the third flight in 2014-2015. This thesis presents the study of the ANITA-III storage system. The design principle was the heat dissipation and the RF shielding. The ANITA-III storage system was the largest-storage device in NASA balloon-borne telescope. Taiwan Astroparticle Radio Observatory of Geosynchrotron Emissiom (TAROGE) is also an RF-based detector. TAROGE is located on a coastal mountain-top in Hua-Lian and its 12 antennas are horizontally pointing toward the Pacific Ocean. It can detect not only the direct signals but also the reflected signals emitted from the air showers induced by the CRs. In addition, the Earth-skimming neutrinos are also detectable for TAROGE.This thesis presents the simulation result of the cosmic rays events. This thesis also includes the studies of the TAROGE-2 power system. There is usually no existing power supply system in a RF-quiet location. We built the solar power supply system and the power control system for TAROGE-2.
Chen, Chih-Ching y 陳志清. "The Radio Detection of Ultra High Energy Neutrinos and Cosmic Rays". Thesis, 2015. http://ndltd.ncl.edu.tw/handle/01149387018368952528.
Texto completo國立臺灣大學
天文物理研究所
103
In this thesis we study the Cherenkov radiation pulse from ultra-high energy particle shower by a numerical finite-difference time-domain (FDTD) method. Expounding the work on ANITA experiment include detection method, instrument and operation method. The design concept of Askaryan Radio Array (ARA) experiment and the hardware, deploy and operation. We propose our strategy to identify the neutrino flavor in observing cosmogenic neutrinos by radio neutrino telescopes, such as ARA, ARIANNA.
Prouza, Michael. "Ultra-High Energy Cosmic Rays and Theirs Detection in Auger Project". Doctoral thesis, 2006. http://www.nusl.cz/ntk/nusl-266019.
Texto completoJames, Clancy William. "Ultra-high energy particle detection with the lunar Cherenkov technique". 2009. http://hdl.handle.net/2440/57706.
Texto completohttp://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.
Texto completoThesis (Ph.D.) - University of Adelaide, School of Chemistry and Physics, 2009.
Schröder, Frank Gerhard [Verfasser]. "Instruments and methods for the radio detection of high energy cosmic rays / von Frank Gerhard Schröder". 2011. http://d-nb.info/1010373439/34.
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