A quantificação da atividade de radionuclídeos emissores de raios gama em amostras medidas por espectrometria gama com detectores HPGe depende da análise dos fotopicos presentes no espectro, especialmente da determinação exata das suas áreas líquidas. Tal análise é geralmente realizada com o auxílio de ferramentas de software proprietário. Este trabalho apresenta uma metodologia, descrição de algoritmos e um aplicativo de código aberto, denominado OpenGamma, para a busca e análise de fotopicos a fim de se obter seus parâmetros relevantes e as atividades dos radionuclídeos na amostra. A implementação computacional é distribuída sob licença aberta para o código principal e com o uso de pacotes de software aberto para o projeto da interface e para bibliotecas matemáticas. O procedimento para a busca de picos é realizado em três etapas. Primeiramente, executa-se uma pesquisa preliminar com o método da segunda diferença, que consiste na geração de um espectro derivado para a busca de picos candidatos. Na segunda etapa, calculam-se as larguras experimentais dos picos, dos quais escolhem-se aqueles bem formados e isolados para a obtenção da função de ajuste da largura vs. canal, por meio do método de Levenberg-Marquardt para ajustes não-lineares. Por fim, regiões do espectro com picos agrupados são delimitadas e novo ajuste não-linear é aplicado a cada região para a obtenção dos termos da linha de base e dos fotopicos. A partir destes termos, são calculadas as áreas líquidas dos picos. Para a determinação da atividade, curvas de calibração de eficiência previamente obtidas, bem como dados de transições gama dos radionuclídeos, são incorporadas ao código e aplicadas. O código foi escrito em linguagem C++ e a interface foi desenvolvida com a ferramenta Qt. Para as funções matemáticas e procedimentos de ajuste, foi usada a biblioteca científica GNU (GSL). A validação de código foi feita por meio da análise de: 1) espectros sintéticos de teste da AIEA, especialmente desenhados para a avaliação de desempenho de software; 2) espectros obtidos com amostras de exercícios de intercomparação e 3) espectros da rotina de trabalho do Laboratório de Radiometria Ambiental (LRA) do IPEN e analisados com o aplicativo comercial InterWinner. Os resultados obtidos são consistentes com os valores de referência e com aqueles obtidos pelo aplicativo citado, sugerindo que o código OpenGamma pode ser utilizado com segurança na espectrometria de raios gama de uso geral. / Radioactivity quantification of gamma-ray emitter radionuclides in samples measured by HPGe gamma-ray spectrometry relies on the analysis of the photopeaks present in the spectra, especially on the accurate determination of their net areas. Such a task is usually performed with the aid of proprietary software tools. This work presents a methodology, algorithm descriptions and an open source application, called OpenGamma, for the peak search and analysis in order to obtain the relevant peaks parameters and radionuclides activities. The computational implementation is released entirely in open-source license for the main code and with the use of open software packages for interface design and mathematical libraries. The procedure for the peak search is performed on a three step approach. Firstly a preliminary search is done by using the second-difference method, consisting in the generation of a derived spectrum in order to find candidate peaks. In the second step, the experimental peaks widths are assessed and well formed and isolated ones are chosen to obtain a FWHM vs. channel relationship, by application of the Levenberg-Marquardt minimization method for non-linear fitting. Lastly, regions of the spectrum with grouped peaks are marked and a non-linear fit is again applied to each region to obtain baseline and photopeaks terms; from these terms, peaks net areas are then assessed. For the activity determination, previously obtained efficiency calibration curves, as well as nuclides gamma-ray data, are incorporated in the code and applied. The code was developed in C++ language and the interface was developed with Qt GUI software toolkit. GNU scientific library, GSL, was employed to perform fitting procedures as needed. Validation of code was done by analyzing: 1) synthetic test spectra from IAEA, especially designed for software performance evaluation; 2) spectra obtained from samples of intercomparison exercises and 3) spectra from routine activities of the Environmental Radiometric Laboratory (LRA) at IPEN and analyzed with the commercial software package InterWinner. Results obtained are consistent with the reference values and with those obtained by the aforementioned package. The results suggest that the OpenGamma code could be safely used in general-purpose gamma-ray spectrometry.

Alvos naturais de Mg, Al, Si, Cr, Ti, Ni e Zr foram irradiados com prótons e as seções de choque para várias reações nucleares foram determinadas a energias inferiores a 30 MeV. As irradiações foram efetuadas nos ciclotrons CV-28 e CYCLONE 30 do IPEN, que possuem energia nominal de 24 e 30 MeV, respectivamente. O feixe de prótons foi monitorado por meio de lâminas de Cu ou a partir da formação de nuclídeos na própria amostra com seção de choque conhecida para as energias utilizadas. Especial interesse foi dedicado às reações raras di tipo (p, 2alfa) e (p, ANTPOT.3 H) das quais existem, em geral, poucos dados publicados, principalmente para energias próximas do limiar. A determinação da seção de choque foi realizada a partir da medida da atividade residual dos produtos pelo método de espectroscopia gama simples. Um detector HPG com resolução menor que 2 keV foi utilizado. Devido ao valor reduzido da seção de choque das reações de interesse no intervalo de energia considerado, uma análise estatística cuidadosa dos dado foi necessária. Em áreas reduzidas dos picos detectados precisaram da quantificação, em alguns casos, da contribuição de nuclídeos formados na própria amostra por outras reações, a partir de impurezas ou provenientes do fundo radioativo. Entre os produtos obtidos encontram-se os nuclídeos ANTPOT.22 Na, ANTPOT.26 Al, ANTPOT.44 Ti, e ANTPOT.54 Mn. A detecção de ANTPOT.26 Al nas amostras de Al e Si, permitiu estimar os limites do método proposto para o estudo de reações raras de interesse astrofísico. No total, são apresentados neste trabalho 72 valores de seção de choque. Desse total, 21 dados são apresentados pela primeira vez ou foram obtidos pela primeira vez pelo método proposto ou às energias estudadas. Os resultados mais importantes referem-se às reações ANTPOT.29 Si(p, 2alfa)ANTPOT.22 Na,ANTPOT.53 Cr(p, 2alfa)ANTPOT.46 Sc, ANTPOT.46 Ti(p, ANTPOT.3 H)ANTPOT.44 Ti, )ANTPOT.58 Ni(p, ANTPOT.3 H)ANTPOT.56 Ni e ANTPOT.90 Zr(p, ANTPOT.3 H)ANTPOT.88 Zr. Os resultados foram comparados com valores publicados na literatura e com o resultado do cálculo realizado a partir de modelos teóricos conhecidos, permitindo a obtenção de conclusões relativas ao método experimental, assim como aos mecanismos da reação envolvidos. / Natural targets of Mg, Al, Si, Cr, Ti, Ni and Zr were irradiated with protons and the cross section for several reactions were determined for incident energies up to 30 MeV. The irradiations were performed at the CV-28 and CYCLONE 30 cyclotrons from the IPEN, which have nominal energies of 24 and 30 MeV, respectively. The protons beams were monitored by copper foils or by the nuclide formation in the irradiated targets with known cross sections for the used energy. Special interest was dedicated to rare reactions of the (p, 2alfa) and (p, ANTPOT.3 H) kind, from which we have a few published data, mainly for energies near the threshold. The cross section determination was accomplished by the residual actives measurement of the reaction products by the simple gamma spectroscopy method using an HPGe detector with resolution better than 2 keV. Due to the low value of the cross section for the considered reaction, a careful statistical analysis of the obtained data was needed. The small areas of the detected peaks required the quantification of the contributions of nuclides produced by others reactions, from contaminants or from the radioactive background. Among others, the ANTPOT.22 Na, ANTPOT.26 Al, ANTPOT.44 Ti and ANTPOT.54 Mn products have been detected. The detection of ANTPOT.26 Al in the Al and Si targets allow the estimation of the limits of the proposed method for the study of astrophysical interest reaction. In total, 72 cross section values are being presented. Out of this amount, 21 are being presented for the first time or have been obtained for the first time by the method or for the studied energies. The most important results refer to the ANTPOT.29 Si(p, 2gamma)²²Na, ANTPOT.53 Cr(p, 2gamma)ANTPOT.46 Sc, ANTPOT.46 Ti(p, ANTPOT.3 H)ANTPOT.44 Ti, ANTPOT.58 Ni(p, ANTPOT.3 H)ANTPOT.56 Ni and ANTPOT.90 Zr(p, ANTPOT.3 H)ANTPOT.88 Zr reactions. The results have been compared to published vales and calculations using known theoretical models, allowing the achievement of conclusions related to the experimental method, as well as the reaction mechanism involved.

Oxygen sequence Wolf-Rayet stars (WO) are thought to be the final evolution phase of some high-mass stars, as such they may be the progenitors of Type Ic SNe as well as potential progenitors of broad-lined Ic and long gamma-ray bursts. We present the first spectropolarimetric observations of the Galactic WO stars WR93b and WR102 obtained with FORS1 on the Very Large Telescope. We find no sign of a line effect, which could be expected if these stars were rapid rotators. We also place constraints on the amplitude of a potentially undetected line effect. This allows us to derive upper limits on the possible intrinsic continuum polarization and find Pcont < 0.077 per cent and Pcont < 0.057 per cent for WR93b and WR102, respectively. Furthermore, we derive upper limits on the rotation of our WO stars by considering our results in the context of the wind compression effect. We estimate that for an edge-on case the rotational velocity of WR93b is vrot < 324 km s−1 while for WR102 vrot < 234 km s−1. These correspond to values of vrot/vcrit < 19 per cent and j) < 18.0 cm2 s−1 for WR93b and 2 s−1 for WR102. The upper limits found on vrot/vcrit and log(j) for our WO stars are therefore similar to the estimates calculated for Galactic Wolf-Rayet (WR) stars that do show a line effect. Therefore, although the presence of a line effect in a single WR star is indicative of fast rotation, the absence of a line effect does not rule out significant rotation, even when considering the edge-on scenario.

<p><font face="TimesNewRomanPSMT"> <p align="left">Natural radioactivity studies have been carried out to study the textural characteristics, heavy mineral composition, provenance, sediment transport, and depositional environment of beach placer deposits. The naturally occurring radionuclides such as properties of beach sands, which reflect the geological characteristics such as transport and sorting processes and the depositional environment. The present work focuses on the radiometric characteristics of beach sand deposits along the west coastof South Africa. Beach sands samples were collected at the Melkbosstrand (MBS) and Ouskip (OSK) beach. The activity concentrations of these radionuclides were determined by high-resolution gamma-ray spectrometry using a high-purity germanium (HPGe) detector in a low-background configuration.</p> </font></p>

Gamma-ray spectrometry measurements performed on site, or “in situ”, is a widely used and powerful method that can be employed both to identify and quantify ground deposited radionuclides. The purpose of this thesis is to improve the calibration of high purity germanium (HPGe) detectors for in situ measurements, and calculate the combined uncertainty and potential systematic effects. An improved semi-empirical calibration method is presented, based on a novel expression for the intrinsic detector efficiency that includes both the energy and angular response of the detector. A three-layer model for the description of the depth distribution of the radionuclide and the soil density is proposed. The combined uncertainty of intrinsic detector efficiency calibrations and in situ measurements according to the proposed method was estimated. The uncertainty in the intrinsic detector efficiency was found to be 5.1 and 8.1% (coverage factor k=1, i.e. for a confidence interval of about 68%), for the two detectors calibrated. These numbers were, however, at a later stage reduced to 3.7 and 4.2%, using a revised expression for the intrinsic detector efficiency. For in situ measurements, the combined standard uncertainty was found to be 15-20% (k=1), based on the original expression for the intrinsic detector efficiency. Monte Carlo models of the two detectors were created and Monte Carlo calculated values for intrinsic detector efficiency were compared with experimental data. As a discrepancy was found, a thorough investigation of the detector response was performed. Scanning of the detector surface with a collimated 59.5 keV photon beam revealed the detector response to be highly irregular over the detector surface. It was concluded that the efficiency deficit of the detector could most likely be attributed to an increase in dead layer thickness compared with manufacturer supplied data. The thickness of the dead layer was estimated to be 1.5-1.9 mm, whereas the nominal value was 0.7 mm. Radiographs of the detectors were produced that provided valuable information about the physical dimensions of the germanium crystal, as well as its actual location within the detector housing. The Monte Carlo models were employed to calculate in situ measurement efficiencies for measurements of 137Cs deposition from the Chernobyl fallout. Results from the Monte Carlo simulations were compared both with the semi-empirical method and with soil sample data, and satisfactory agreement was confirmed. It was then proceeded to employ the Monte Carlo model to calculate the effect on in situ measurement results by two influencing parameters: ground curvature and activity in trees. Neither of these parameters was found to influence the result by more than about 25%. This deviation is comparable with the measurement uncertainty, and should not deter from measurements in such terrain.

A high-efficiency gamma-ray counting system has been built at Los Alamos National Laboratory for use in analyzing nuclear forensics samples. This system consists of two clover high-purity germanium detectors and is surrounded by a thallium-doped sodium iodide annulus. Special precautions have been taken to ensure the system has a low background. The system is connected to XIA Pixie-4 fast digitizers and collects data in list-mode. This work is split into two main parts. The first part describes the proper steps and techniques to initialize the settings of a detector system connected to fast digitizers in order to optimize the system for resolution and throughput. The various counting modes for this particular system are described in detail, including the benefits and drawbacks of each mode. Steps are then shown to characterize the system by obtaining efficiency curves for various counting modes and sample geometries. Because of the close counting geometry involved with this system, true-coincidence summing factors must be calculated, and are done so in part by measuring the peak-to-total ratios of the system in its various counting modes across a wide energy range. The dead-time for the system can be complicated due to the multiple inputs of the system. Techniques for calculating the dead-time of multiple-detector systems are discussed. The second part of this work shows the system's usefulness in analyzing nuclear forensics samples, specifically irradiated enriched uranium. Three fission product parent-daughter pairs of different lifetimes are analyzed over a course of six months. The activities of each nuclide are calculated at each time step. Age dating techniques using the parent-daughter pairs are discussed, as well as the detection limits of each nuclide for a range of sample ages. Finally, avenues for further research are presented, as well as potential sources of error or uncertainty for this work. / text

The nuclides present in spent nuclear fuel are categorized according to their capacity for detection by Compton suppression or gamma-gamma coincidence methods. The fifty nuclides with the highest activities in spent fuel are identified, their decay schemes analyzed, and the best detection scheme for each is recommended. / text

Precision measurements of superallowed Fermi β-decay allow for stringent tests of the magnitude of isospin-symmetry-breaking effects in nuclei, the validity of the conserved vector current hypothesis, and the unitarity of the Cabibbo-Kobayashi-Maskawa (CKM) quark-mixing matrix. A high-precision measurement of the branching ratio for the superallowed β+ decay of 74Rb has been performed at the Isotope Separator and ACcelerator (ISAC) facility at TRIUMF. The 8π spectrometer, an array of 20 HPGe detectors, was used to detect γ-rays emitted following the Gamow-Teller and non-analogue Fermi β-decays of 74Rb. PACES, an array of 5 Si(Li) detectors, was used to detect emitted conversion electrons, while half of SCEPTAR, a close-packed array of 10 plastic scintillators, was used to detect emitted β particles. In this experiment, 23 excited states were identified in 74Kr which were populated following the β-decay of 74Rb. A total of 58 γ-rays were identified following the 8.241(4)x108 detected β-particles. An observed non-superallowed branching ratio of 0.396(7)% was determined from the intensity of the identified γ-rays, while the unobserved non-superallowed intensity was calculated to be 0.05(5)%, leading to a superallowed branching ratio of 99.55(5)%. The superallowed branching ratio is now the most precise experimental quantity in the determination of the superallowed ft-value of 74Rb. Combining the half-life and Q-value with the superallowed branching ratio measured in this work leads to a superallowed ft-value of 3082.6(66) s. Finally, comparisons between the superallowed ft-value, the world average Ft-value, and the non-analogue Fermi branching ratio are made to provide future guidance in the refinement of the theoretical models required to describe the crucial isospin-symmetry-breaking term in superallowed β-decay.

<p><font face="TimesNewRomanPSMT"> <p align="left">Natural radioactivity studies have been carried out to study the textural characteristics, heavy mineral composition, provenance, sediment transport, and depositional environment of beach placer deposits. The naturally occurring radionuclides such as properties of beach sands, which reflect the geological characteristics such as transport and sorting processes and the depositional environment. The present work focuses on the radiometric characteristics of beach sand deposits along the west coastof South Africa. Beach sands samples were collected at the Melkbosstrand (MBS) and Ouskip (OSK) beach. The activity concentrations of these radionuclides were determined by high-resolution gamma-ray spectrometry using a high-purity germanium (HPGe) detector in a low-background configuration.</p> </font></p>

In the presented thesis, the most advanced photon reconstruction technique of ground-based γ-ray astronomy is adapted to the H.E.S.S. 28 m telescope. The method is based on a semi-analytical model of electromagnetic particle showers in the atmosphere. The properties of cosmic γ-rays are reconstructed by comparing the camera image of the telescope with the Cherenkov emission that is expected from the shower model. To suppress the dominant background from charged cosmic rays, events are selected based on several criteria. The performance of the analysis is evaluated with simulated events. The method is then applied to two sources that are known to emit γ-rays. The first of these is the Crab Nebula, the standard candle of ground-based γ-ray astronomy. The results of this source confirm the expected performance of the reconstruction method, where the much lower energy threshold compared to H.E.S.S. I is of particular importance. A second analysis is performed on the region around the Galactic Centre. The analysis results emphasise the capabilities of the new telescope to measure γ-rays in an energy range that is interesting for both theoretical and experimental astrophysics. The presented analysis features the lowest energy threshold that has ever been reached in ground-based γ-ray astronomy, opening a new window to the precise measurement of the physical properties of time-variable sources at energies of several tens of GeV. / In der vorliegenden Dissertation wird die zur Zeit sensitivste Methode zur Photonrekonstruktion in der bodengebundenen Gammastrahlungsastronomie an das 28 m H.E.S.S. Teleskop angepasst. Die Analyse basiert auf einem semi-analytischen Modell von elektromagnetischen Teilchenschauern in der Erdatmosphäre. Die Rekonstruktion erfolgt durch den Vergleich des Bildes der Teleskopkamera mit der Tscherenkow-Emission, die mittels des Schauermodells berechnet wurde. Zur Verringerung des dominanten Untergrundes, der hauptsächlich durch Teilchen der geladenen kosmischen Strahlung hervorgerufen wird, werden Ereignisse anhand bestimmter Kriterien ausgewählt. Die Leistungsfähigkeit der Analyse wird unter Verwendung simulierter Ereignisse evaluiert. Die Methode wird anschließend auf zwei Gammastrahlungsquellen angewendet. Zuerst wird der Krebsnebel analysiert, die Standardkerze der bodengebundenen Gammastrahlungsastronomie. Die Resultate der Analyse des Krebsnebels bestätigen die bereits zuvor erwartete Leistungsfähigkeit der Rekonstruktionsmethode, wobei hier insbesondere die im Vergleich zu H.E.S.S. I stark verringerte Energieschwelle hervorzuheben ist. Als Zweites werden Beobachtungen der Region um das galaktische Zentrum ausgewertet. Die Analyseergebnisse dieser Daten unterstreichen die Fähigkeiten des neuen Teleskops zur Messung kosmischer Gammastrahlung in einem für die theoretische und experimentelle Astrophysik interessanten Energiebereich. Die vorgestellte Analyse besitzt die niedrigste Energieschwelle, die in der bodengebundenen Gammastrahlungsastronomie je erreicht wurde. Sie ermöglicht damit präzise Messungen der physikalischen Eigenschaften von zeitabhängigen Quellen im Energiebereich von 10 bis 100 GeV.