NU-PROCESS IN EXOTIC MODELS

The exact physical conditions generating the abundances of r-elements in environments such as supernovae explosions are still under debate. We evaluated the characteristics expected for the neutrino wind in the proposed model of type-II supernova driven by conversion of nuclear matter to strange matter. Neutrinos will change the final abundance of elements after freeze out of r-process nucleosynthesis, specially those close to mass peaks.

Astrophysikalische Bedingungen für einen r-Prozess im Hoch-Entropie-Wind von Typ II Supernovae

Sterne mit einer Anfangsmasse zwischen etwa 8 und 25 Sonnenmassen enden ihre Existenz mit einer gewaltigen Explosion, einer Typ II Supernova. Die hierbei entstehende Hoch-Entropie-Blase ist ein Bereich am Rande des sich bildenden Neutronensterns und gilt als möglicher Ort für den r-Prozess. Wegen der hohen Temperatur T innerhalb der Blase ist die Materie dort vollkommen photodesintegriert. Das Verhältnis von Neutronen zu Protonen wird durch die Elektronenhäufigkeit Ye beschrieben. Die thermodynamische Entwicklung des Systems wird durch die Entropie S gegeben. Da die Expansion der Blase schnell vonstatten geht, kann sie als adiabatisch betrachtet werden. Die Entropie S ist dann proportional zu T^3/rho, wobei rho die Dichte darstellt. Die explizite Zeitentwicklung von T und rho sowie die Prozessdauer hängen von Vexp, der Expansionsgeschwindigkeit der Blase, ab. Der erste Teil dieser Dissertation beschäftigt sich mit dem Prozess der Reaktionen mit geladenen Teilchen, dem alpha-Prozess. Dieser Prozess endet bei Temperaturen von etwa 3 mal 10^9 K, dem sogenannten "alpha-reichen" Freezeout, wobei überwiegend alpha-Teilchen, freie Neutronen sowie ein kleiner Anteil von mittelschweren "Saat"-Kernen im Massenbereich um A=100 gebildet werden. Das Verhältnis von freien Neutronen zu Saatkernen Yn/Yseed ist entscheidend für den möglichen Ablauf eines r-Prozesses. Der zweite Teil dieser Arbeit beschäftigt sich mit dem eigentlichen r-Prozess, der bei Neutronenanzahldichten von bis zu 10^27 Neutronen pro cm^3 stattfindet, und innerhalb von maximal 400 ms sehr neutronenreiche "Progenitor"-Isotope von Elementen bis zum Thorium und Uran bildet. Bei dem sich anschliessendem Ausfrieren der Neutroneneinfangreaktionen bei 10^9 K und 10^20 Neutronen pro cm^3 erfolgt dann der beta-Rückzerfall der ursprünglichen r-Prozesskerne zum Tal der Stabilität. Diese Nicht-Gleichgewichts-Phase wird in der vorliegenden Arbeit in einer Parameterstudie eingehend untersucht. Abschliessend werden astrophysikalische Bedingungen definiert, unter denen die gesamte Verteilung der solaren r-Prozess-Isotopenhäufigkeiten reproduziert werden können.

VLT-FLAMES analysis of 8 giants in the bulge metal-poor globular cluster NGC 6522: oldest cluster in the Galaxy? Analysis of 8 giants in NGC 6522

Context. NGC 6522 has been the first metal-poor globular cluster identified in the bulge by Baade. Despite its importance, very few high-resolution abundance analyses of stars in this cluster are available. The bulge metal-poor clusters may be important tracers of the early chemical enrichment of the Galaxy. Aims. The main purpose of this study is to determine metallicity and elemental ratios in individual stars of NGC 6522. Methods. High-resolution spectra of 8 giants of the bulge's globular cluster NGC 6522 were obtained at the 8m VLT UT2-Kueyen telescope with the FLAMES+GIRAFFE spectrograph. Multiband V, I, J, K(s) photometry was used to derive effective temperatures as reference values. Spectroscopic parameters were derived from Fe I and Fe II lines, and adopted for the derivation of abundance ratios. Results. The present analysis provides a metallicity [Fe/H] = -1.0 +/- 0.2. The alpha-elements oxygen, magnesium and silicon show [O/Fe] = +0.4 +/- 0.3, [Mg/Fe] = [Si/Fe] = +0.25 +/- 0.15, whereas calcium and titanium show shallower ratios of [Ca/Fe] = [Ti/Fe] = +0.15 +/- 0.15. The neutron-capture r-process element europium appears to be overabundant by [Eu/Fe] = +0.4 +/- 0.4. The neutron-capture s-elements lanthanum and barium are enhanced by [La/Fe] = +0.35 +/- 0.2 and [Ba/Fe] = +0.5 +/- 0.5. The large internal errors, indicating the large star-to-star variation in the barium and europium abundances, are also discussed. Conclusions. The moderate metallicity combined to a blue horizontal branch (BHB), are characteristics similar to those of HP 1 and NGC 6558, pointing to a population of very old globular clusters in the Galactic bulge. Also, the abundance ratios in NGC 6522 resemble those in HP 1 and NGC 6558. The ultimate conclusion is that the bulge is old, and went through an early prompt chemical enrichment.

Search for sterile neutrino mixing in the MINOS long-baseline experiment

A search for depletion of the combined flux of active neutrino species over a 735 km baseline is reported using neutral-current interaction data recorded by the MINOS detectors in the NuMI neutrino beam. Such a depletion is not expected according to conventional interpretations of neutrino oscillation data involving the three known neutrino flavors. A depletion would be a signature of oscillations or decay to postulated noninteracting sterile neutrinos, scenarios not ruled out by existing data. From an exposure of 3.18 x 10(20) protons on target in which neutrinos of energies between similar to 500 MeV and 120 GeV are produced predominantly as nu(mu), the visible energy spectrum of candidate neutral-current reactions in the MINOS far detector is reconstructed. Comparison of this spectrum to that inferred from a similarly selected near-detector sample shows that of the portion of the nu(mu) flux observed to disappear in charged-current interaction data, the fraction that could be converting to a sterile state is less than 52% at 90% confidence level (C. L.). The hypothesis that active neutrinos mix with a single sterile neutrino via oscillations is tested by fitting the data to various models. In the particular four-neutrino models considered, the mixing angles theta(24) and theta(34) are constrained to be less than 11 degrees and 56 degrees at 90% C. L., respectively. The possibility that active neutrinos may decay to sterile neutrinos is also investigated. Pure neutrino decay without oscillations is ruled out at 5.4 standard deviations. For the scenario in which active neutrinos decay into sterile states concurrently with neutrino oscillations, a lower limit is established for the neutrino decay lifetime tau(3)/m(3) > 2.1 x 10(-12) s/eV at 90% C.L.

Search for Active Neutrino Disappearance Using Neutral-Current Interactions in the MINOS Long-Baseline Experiment

We report the first detailed comparisons of the rates and spectra of neutral-current neutrino interactions at two widely separated locations. A depletion in the rate at the far site would indicate mixing between nu(mu) and a sterile particle. No anomalous depletion in the reconstructed energy spectrum is observed. Assuming oscillations occur at a single mass-squared splitting, a fit to the neutral- and charged-current energy spectra limits the fraction of nu(mu) oscillating to a sterile neutrino to be below 0.68 at 90% confidence level. A less stringent limit due to a possible contribution to the measured neutral-current event rate at the far site from nu(e) appearance at the current experimental limit is also presented.

The gross theory model for neutrino-nucleus cross-section

The nuclear gross theory, originally formulated by Takahashi and Yamada (1969 Prog. Theor. Phys. 41 1470) for the beta-decay, is applied to the electronic-neutrino nucleus reactions, employing a more realistic description of the energetics of the Gamow-Teller resonances. The model parameters are gauged from the most recent experimental data, both for beta(-)-decay and electron capture, separately for even-even, even-odd, odd-odd and odd-even nuclei. The numerical estimates for neutrino-nucleus cross-sections agree fairly well with previous evaluations done within the framework of microscopic models. The formalism presented here can be extended to the heavy nuclei mass region, where weak processes are quite relevant, which is of astrophysical interest because of its applications in supernova explosive nucleosynthesis.

The (9)Be((8)Li, (9)Be)(8)Li elastic-transfer reaction

Angular distributions for the (9)Be((8)Li, (9)Be) (8)Li elastic-transfer reaction have been measured with a 27-MeV (8)Li radioactive nuclear beam. Spectroscopic factors for the <(9)Be vertical bar(8)Li + p > bound system were obtained from the comparison between the experimental differential cross sections and finite-range distorted-wave Born approximation calculations made with the code FRESCO. The spectroscopic factors so obtained are compared with shell-model calculations and other experimental values. Using the present value for the spectroscopic factors, cross sections and reaction rates for the (8)Li(p,gamma) (9)Be direct proton-capture reaction of astrophysical interest were calculated in the framework of the potential model.

Medidas Fonológicas em Crianças com Perturbação dos Sons da Fala. Estudo comparativo entre o português europeu e o português brasileiro.

O objetivo deste estudo é comparar as características de dois grupos de crianças com diagnóstico de Perturbação dos Sons da Fala (PSF), falantes de português europeu (PE) e falantes de português brasileiro (PB), considerando um conjunto de medidas fonológicas que incluem Percentagem de Consoantes Corretas (PCC), Percentagem de Consoantes Corretas Revista (PCC-R), Process Density Index (PDI), Índices Absolutos (IA) e Índices Relativos (IR) de Substituição, Omissão e Distorção, tipos de Processos Fonológicos e Percentagem de Acerto por Fonema (PAF). Método: Neste estudo participaram dezoito crianças com diagnóstico de Perturbação dos Sons da Fala (PSF), com idades compreendidas entre os cinco anos e dois meses e os sete anos e 11 meses, sendo doze do sexo masculino e seis do sexo feminino, divididas em dois grupos - falantes de português europeu (GPE) e falantes de português brasileiro (GPB) - emparelhadas por idade, sexo e valor de PCC. A partir da análise das transcrições fonéticas constantes nas folhas de registo de cada subteste de nomeação de cada sujeito - Teste Fonético-Fonológico - Avaliação de Linguagem Pré-Escolar (TFF - ALPE) (Mendes et al., 2009) para o português europeu, e provas de fonologia do Teste de Linguagem Infantil ABFW (Andrade et al., 2004) para o português brasileiro,- foram calculadas e comparadas as medidas fonológicas referidas, recorrendo a testes estatísticos (paramétricos e não paramétricos). Resultados: O emparelhamento do GPE com o GPB foi bem sucedido. Não existiram diferenças estatísticamente significativas nas medidas fonológicas em estudo entre o GPE e o GPB. No Estudo 1, não existiram diferenças nos tipos de erros à exceção do erro de omissão. No Estudo 2, no GPE verificamos um menor número de erros de distorção e um maior número de erros de omissão. Existem algumas particularidades devido à variante da língua, nomeadamente no processo fonológico de PAL e de DESV. Conclusão: Esta investigação permitiu realizar a comparação do GPE e do GPB com a utilização de dois instrumentos recolha de dados diferentes. Os resultados foram de encontro ao que é descrito por outros estudos nesta área de investigação. As poucas diferenças que se observaram podem ser explicadas pelas diferenças existentes entre os sistemas fonético-fonológicos das duas variedades linguísticas. É extremamente importante a metodologia de recolha de dados para a avaliação das PSF. A mais valia desta pesquisa é o contributo de indicadores clínicos para diagnóstico, prognóstico e intervenção terapêutica nas PSF.

Organizational capacity and knowledge transfer : a qualitative case study of the 2007 Canada Winter Games host society

Understanding and managing the knowledge transfer process in sport organizations is an essential component to enhance organizational capacity. Very little research on either capacity or knowledge transfer within a sport organization exists. Consequently, the purpos e of this qualitative case study was to, examine the transfer of knowledge process within a major games host society. Specifically, two research goals guided the study: 1) To develop a model to explain a knowledge t r ans f e r process in a non-profit ma jor games hos t organization and 2) To examine the relevance of the model to a Canada Games Hos t Society. Data we r e collected from interviews with middle and senior level volunteers as well as senior s t a f f members (n= 27), document s and observations. The findings indicated three barriers to knowledge transfer: structural, systemic, and cultural. As a result of the findings a revised model for knowledge transfer wa s proposed that included modifications related to the direction of knowledge flow, timing of the knowledge transfer process, and group inter-relations. Implications identified the importance of intuition managers, time and organizational levels for successful knowledge transfer. Recommendations for future host societies and the Canada Games Council are presented.

Lines of heavy elements and Fe II in the UV of CS 31082-001

The abundance of heavy r-elements may provide a better understanding of the r-process, and the determination of several reference r-elements should allow a better determination of a star`s age. The space UV region (lambda < 3000 angstrom) presents a large number of lines of the heavy elements, and in the case of some elements, such as Bi, Pt, Au, detectable lines are not available elsewhere. The extreme ""r-process star"" CS 31082-001 ([Fe/H] = -2.9) was observed in the space UV to determine abundances of the heaviest stable elements, using STIS on board Hubble Space Telescope.

Mass varying neutrinos in supernovae

Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)

The Li-8(p, alpha)He-5 reaction at low energies, and Be-9 spectroscopy around the proton threshold

We present a direct measurement of the low-energy Li-8(p, alpha)He-5 cross section, using a radioactive Li-8 beam impinging on a thick target. With four beam energies, we cover the energy range between E-c.m. = 0.2 and 2.1 MeV. An R-matrix analysis of the data is performed and suggests the existence of two broad overlapping resonances (5/2(+) at E-c.m. = 1.69 MeV and 7/2(+) at E-c.m. = 1.76 MeV). At low energies our data are sensitive to the properties of a subthreshold state (E-x = 16.67 MeV) and of two resonances above threshold. These resonances were observed in previous experiments. The R-matrix fit confirms spin assignments, and provides partial widths. We propose a new Li-8(p, alpha)He-5 reaction rate and briefly discuss its influence in nuclear astrophysics. DOI: 10.1103/PhysRevC.86.064321

Elemental abundances and classification of carbon-enhanced metal-poor stars

We present a detailed study of carbon-enhanced metal-poor (CEMP) stars, based on high-resolution spectroscopic observations of a sample of 18 stars. The stellar spectra for this sample were obtained at the 4.2 m William Herschel Telescope in 2001 and 2002, using the Utrecht Echelle Spectrograph, at a resolving power R similar to 52 000 and S/N similar to 40, covering the wavelength range lambda lambda 3700-5700 angstrom. The atmospheric parameters determined for this sample indicate temperatures ranging from 4750 K to 7100 K, log g from 1.5 to 4.3, and metallicities -3.0 <= [Fe/H]<=-1.7. Elemental abundances for C, Na, Mg, Sc, Ti, Cr, Cu, Zn, Sr, Y, Zr, Ba, La, Ce, Nd, Sm, Eu, Gd, Dy are determined. Abundances for an additional 109 stars were taken from the literature and combined with the data of our sample. The literature sample reveals a lack of reliable abundance estimates for species that might be associated with the r-process elements for about 67% of CEMP stars, preventing a complete understanding of this class of stars, since [Ba/Eu] ratios are used to classify them. Although eight stars in our observed sample are also found in the literature sample, Eu abundances or limits are determined for four of these stars for the first time. From the observed correlations between C, Ba, and Eu, we argue that the CEMP-r/s class has the same astronomical origin as CEMP-s stars, highlighting the need for a more complete understanding of Eu production.

Origin of the heavy elements in HD 140283 Measurement of europium abundance

Context. HD 140283 is a nearby (V = 7.7) subgiant metal-poor star, extensively analysed in the literature. Although many spectra have been obtained for this star, none showed a signal-to-noise (S/N) ratio high enough to enable a very accurate derivation of abundances from weak lines. Aims. The detection of europium proves that the neutron-capture elements in this star originate in the r-process, and not in the s-process, as recently claimed in the literature. Methods. Based on the OSMARCS 1D LTE atmospheric model and with a consistent approach based on the spectrum synthesis code Turbospectrum, we measured the europium lines at 4129 angstrom and 4205 angstrom, taking into account the hyperfine structure of the transitions. The spectrum, obtained with a long exposure time of seven hours at the Canada-France-Hawaii Telescope (CFHT), has a resolving power of 81 000 and a S/N ratio of 800 at 4100 angstrom. Results. We were able to determine the abundance A(Eu) = -2.35 +/- 0.07 dex, compatible with the value predicted for the europium from the r-process. The abundance ratio [Eu/Ba] = +0.58 +/- 0.15 dex agrees with the trend observed in metal-poor stars and is also compatible with a strong r-process contribution to the origin of the neutron-capture elements in HD 140283.

First measurement of beta decay half-lives in neutron-rich Tl and Bi isotopes

Neutron-rich isotopes around lead, beyond N = 126, have been studied exploiting the fragmentation of an uranium primary beam at the FRS-RISING setup at GSI. For the first time beta-decay half-lives of Bi-219 and Tl-211,Tl-212,Tl-213 isotopes have been derived. The half-lives have been extracted using a numerical simulation developed for experiments in high-background conditions. Comparison with state of the art models used in r-process calculations is given, showing a systematic underestimation of the experimental values, at variance from close-lying nuclei. (c) 2012 Elsevier B.V. All rights reserved.