O presente trabalho tem o objetivo principal de compreender os possíveis efeitos da radiação energética de um evento de Gamma-Ray Burst (GRB) sobre o meio interestelar no entorno de seu local de geração e em planetas possivelmente iluminados. Gamma-Ray Bursts foram detectados pela primeira vez nos anos 60 e rapidamente atraíram a atenção da comunidade astrofísica, uma vez que as energias emitidas apenas em poderiam alcançar 1054erg, o equivalente a massa de repouso do Sol. Não se conhecia nenhum mecanismo tão eficiente para extrair energia gravitacional para produzir tal evento. Mais tarde, a possibilidade da emissão ser colimada abaixou a energia em para 5x1050erg, mas o mecanismo central de geração ainda não foi completamente desvendado, havendo muito espaço para alternativas exóticas. Estudamos os efeitos de um GRB sobre o meio interestelar, em uma tentativa de distinguir os remanescentes do GRB do gerado por múltiplas supernovas. Usamos argumentos energéticos e sobre a possibilidade de alterações químicas e isotópicas devido a reações fotonucleares. Também trabalhamos com as implicações biológicas da iluminação de planetas por um GRB, concluindo que os efeitos de tais eventos podem afetar seriamente a biosfera de um planeta mesmo a distâncias de ~10kpc. / The present work has the main goal of understanding the possible effects of the hard gamma radiation produced during a Gamma-Ray Burst (GRB) event both on the interstellar medium surrounding the source of the burst and on planets possibly illuminated. Gamma-Ray Bursts were first detected on the 60s and quickly have attracted the attention of the astrophysical community, since the energies emitted just in could reach 1054erg, the rest mass of the Sun. No mechanism was known to be so efficient in extracting gravitational energy to produce such emission. Later on, the possibility of the emission being collimated has lowered the energy of the to 5x1051erg, but the central engine has not yet been completely understood, and there is still ample room for exotic alternatives. We have studied the effects of GRB on the ISM, in an attempt to distinguish the candidates of GRB remnants from those generated by multiple supernovae. We have used both energetic arguments and the possibility of chemical alterations due to photonuclear reactions. We have also worked on the biological implications of the illumination of planets by a GRB, concluding that the effects of such event could seriously harm the biosphere of a planet even at distances of ~10kpc.

AgÃncia Nacional do PetrÃleo / CoordenaÃÃo de AperfeiÃoamento de Pessoal de NÃvel Superior / Este trabalho teve como objetivo avaliar o comportamento das tensÃes residuais em tubulaÃÃes de aÃo ASTM A106 Gr. B com pequeno diÃmetro, soldada pelos processos TIG manual e automÃtico. Buscou-se tambÃm avaliar o efeito do aporte tÃrmico sobre o perfil de tensÃes, bem como correlacionar os resultados com a microestrutura e dureza. A mediÃÃo das tensÃes foi realizada atravÃs de difraÃÃo de raio-X, utilizando um minidifratÃmetro empregado para mediÃÃo em campo. AnÃlises metalogrÃficas foram realizadas na seÃÃo transversal da junta, atravÃs de microscopia Ãtica e microscopia eletrÃnica de varredura. Foram levantados os perfis de microdureza nas superfÃcies externa e interna. Os resultados mostraram que a mediÃÃo de tensÃes residuais por difraÃÃo de raio-X, usando o minidifratÃmetro para aplicaÃÃes em campo, à eficaz na determinaÃÃo do perfil de tensÃes, contudo, à necessÃria a realizaÃÃo de ajustes dos difratogramas por funÃÃes analÃticas, para determinar a correta localizaÃÃo do pico de difraÃÃo de raio-X, reduzindo o erro das medidas. As mediÃÃes das tensÃes residuais axiais realizadas na superfÃcie externa dos tubos mostraram que o perfil à formado por tensÃes compressivas na regiÃo da solda (zona fundida e zona afetada pelo calor) e por tensÃes trativas nas regiÃes mais afastadas. Foram observados elevados nÃveis de tensÃes residuais axiais compressivas na superfÃcie externa de tubos de parede fina, na regiÃo da solda, os quais podem representar uma situaÃÃo crÃtica, visto que o comportamento linear das tensÃes ao longo da espessura devido ao efeito torniquete à consensual e, portanto, isso indica a presenÃa de elevados nÃveis de tensÃes residuais de traÃÃo no metal de solda e na zona afetada pelo calor. O ciclo tÃrmico do passe de acabamento ocasionou um intenso refino de grÃo e uma significativa reduÃÃo de dureza, especialmente no metal de solda e na superfÃcie interna dos tubos, a exceÃÃo das amostras de 2â de diÃmetro soldadas com elevado aporte tÃrmico. Nenhuma das amostras soldadas apresentou valores de dureza acima do mÃximo estabelecido por norma, que à de 248 HV, mostrando que o fato da junta apresentar dureza baixa, nÃo necessariamente representa que esta nÃo esteja sujeita a um elevado nÃvel de tensÃes residuais. / The aim of this work was to evaluate the behavior of welding residual stress in small size pipes of ASTM A106 Gr. B steel, welded by manual and automatic GTAW processes. It was also evaluated the effect of the welding heat input on residual stress profile, as well as to correlate the results with microstructure and hardness. The residual stress measurement was accomplished through X-ray diffraction, using a minidiffractometer for measurement in field. Metallographics analysis were accomplished in the traverse section of the welded joint, using optic microscopy and scanning electron microscopy. The microhardness profiles in the outer and inner surfaces of pipe were determined. The results showed that the measures of residual stress by X-ray diffraction with minidiffractometer for applications in field was shown quite effective in the residual stress profile determination, however, it is necessary the accomplishment of diffractograms fittings by analytic functions, to determine the correct peak localization, reducing the measures error. The measurements of the axial residual stress accomplished in the outer surface pipes showed that the profile is formed by compressive stresses in the welds region (fusion zone and heat affected zone - HAZ) and for tension stresses in the areas more distant of weld bead. High levels of compressive axial residual stress were observed in the outer surface of small size pipes, located in the welds region, which can represent a critical situation, because the linear behavior of the through-thickness residual stress due to âtourniquetâ effect is consensual and, therefore, indicates the presence of high levels of tension residual stress in the inner surface, especially in the root weld metal and HAZ. The welding heat input of the finish pass caused an intense grain refining and a significant reduction of hardness of the weld metal in the inner surface, exception of 2" diameter sample welded with high heat input. None of the welded samples presented values of hardness above the maximum established for standard, which is 248 HV, showing that the fact of the welded joint to present low hardness, it does not necessarily represent that this is not subject to a high level of residual stress.

O presente trabalho tem o objetivo principal de compreender os possíveis efeitos da radiação energética de um evento de Gamma-Ray Burst (GRB) sobre o meio interestelar no entorno de seu local de geração e em planetas possivelmente iluminados. Gamma-Ray Bursts foram detectados pela primeira vez nos anos 60 e rapidamente atraíram a atenção da comunidade astrofísica, uma vez que as energias emitidas apenas em poderiam alcançar 1054erg, o equivalente a massa de repouso do Sol. Não se conhecia nenhum mecanismo tão eficiente para extrair energia gravitacional para produzir tal evento. Mais tarde, a possibilidade da emissão ser colimada abaixou a energia em para 5x1050erg, mas o mecanismo central de geração ainda não foi completamente desvendado, havendo muito espaço para alternativas exóticas. Estudamos os efeitos de um GRB sobre o meio interestelar, em uma tentativa de distinguir os remanescentes do GRB do gerado por múltiplas supernovas. Usamos argumentos energéticos e sobre a possibilidade de alterações químicas e isotópicas devido a reações fotonucleares. Também trabalhamos com as implicações biológicas da iluminação de planetas por um GRB, concluindo que os efeitos de tais eventos podem afetar seriamente a biosfera de um planeta mesmo a distâncias de ~10kpc. / The present work has the main goal of understanding the possible effects of the hard gamma radiation produced during a Gamma-Ray Burst (GRB) event both on the interstellar medium surrounding the source of the burst and on planets possibly illuminated. Gamma-Ray Bursts were first detected on the 60s and quickly have attracted the attention of the astrophysical community, since the energies emitted just in could reach 1054erg, the rest mass of the Sun. No mechanism was known to be so efficient in extracting gravitational energy to produce such emission. Later on, the possibility of the emission being collimated has lowered the energy of the to 5x1051erg, but the central engine has not yet been completely understood, and there is still ample room for exotic alternatives. We have studied the effects of GRB on the ISM, in an attempt to distinguish the candidates of GRB remnants from those generated by multiple supernovae. We have used both energetic arguments and the possibility of chemical alterations due to photonuclear reactions. We have also worked on the biological implications of the illumination of planets by a GRB, concluding that the effects of such event could seriously harm the biosphere of a planet even at distances of ~10kpc.

We present multi-wavelength observations and modeling of the exceptionally bright long gamma-ray burst GRB 160625B. The optical and X-ray data are well fit by synchrotron emission from a collimated blastwave with an opening angle of theta(j) approximate to 3 degrees.6 and kinetic energy of E-K approximate to 2 x 10(51) erg, propagating into a low-density (n approximate to 5 x 10(-5) cm(-3)) medium with a uniform profile. The forward shock is sub-dominant in the radio band; instead, the radio emission is dominated by two additional components. The first component is consistent with emission from a reverse shock, indicating an initial Lorentz factor of Gamma(0) greater than or similar to 100 and an ejecta magnetization of R-B approximate to 1-100. The second component exhibits peculiar spectral and temporal evolution and is most likely the result of scattering of the radio emission by the turbulent Milky Way interstellar medium (ISM). Such scattering is expected in any sufficiently compact extragalactic source and has been seen in GRBs before, but the large amplitude and long duration of the variability seen here are qualitatively more similar to extreme scattering events previously observed in quasars, rather than normal interstellar scintillation effects. High-cadence, broadband radio observations of future GRBs are needed to fully characterize such effects, which can sensitively probe the properties of the ISM and must be taken into account before variability intrinsic to the GRB can be interpreted correctly.

With energy outputs >~10^51 erg in 0.1-1000 seconds, Gamma-ray Bursts (GRBs) are the most powerful events yet observed in the Universe. As such they are potential probes of the very early Universe, back to the era of re-ionisation and the first stars, but at the same time they have been observed to span a wide range in luminosity and redshift from the relatively local Universe (z~0.0085) out to z~6.29. GRBs divide into two classes based primarily on their duration as measured by T90 (the time taken to observe 90% of the total burst fluence). Long bursts (L-GRBs) have T90>~2 seconds, and shorts (S-GRBs) T90<~2 seconds. Though much has been learned regarding long duration GRBs since the first afterglow discovery in 1997 (including their likely association with massive core collapse supernovae), much remains unknown regarding short duration GRBs. In this work, after a brief historical introduction and review, we present analyses of the angular cross-correlation on the sky of short GRBs from the BATSE catalogue with galaxies in the local Universe sampled from the PSCz Redshift Survey and the Third Reference Catalogue of Bright Galaxies (RC3). In particular we show that 20%+/-8% (1 sigma) of all BATSE short duration bursts (localised to 10 degrees or better) show correlation with galaxy samples (morphological T-type<=4) within ~112 Mpc. Our statistics thus provide evidence that a substantial fraction of BATSE short GRBs show a tendency to be associated with large scale structure on the sky traced by a variety of galaxy types. Short GRBs are believed to be produced in the final merger of compact object (neutron star-neutron star or neutron star-black hole) binaries, though other possible progenitors are known to exist. The short initial spike of a giant flare from a Soft Gamma Repeater (SGR) such as the December 27th 2004 event from SGR1806-20 would have been detectable by BATSE as a short GRB if it occurred in a galaxy within ~30-50 Mpc (assuming a distance to SGR1806-20 of 15 kpc). Using the observed luminosities and rates of Galactic SGR giant flares, as well as theoretical predictions for the rate of binary mergers, we investigate the ability of plausible Luminosity Functions (LF), singly and in combination, to reproduce our observed correlations and a cosmological S-GRB population. We find the correlations are best explained by a separate population of lower luminosity S-GRBs, with properties consistent with them being due to giant flares from extra-galactic SGRs. Overall predicted number counts are a good fit to the observed BATSE number counts, and furthermore, the wider redshift distribution is consistent with the early Swift S-GRB redshift distribution. The three closest GRBs which have been observed to date were all long duration bursts, and we have therefore also searched for cross-correlation signals between the BATSE long GRBs and local galaxies. The three nearby bursts shared several similar properties such as being under-luminous, spectrally soft and of low variability. We have therefore also investigated a subset of L-GRBs with light curve properties similar to these known nearby bursts. The whole sample is found to exhibit a correlation level consistent with zero (1 sigma upper limit=10%, equivalent to 144 bursts) out to a radius of ~155 Mpc, but a spectrally soft, low observed fluence and low variability subset shows a correlation level of 28%+/-16% (=50+/-28 bursts) within 155 Mpc. These results are consistent with low-luminosity, low-variability bursts being a separate sub-class of L-GRBs which may be much more prevalent in the local Universe than their high-luminosity, cosmologically distant counterparts. To investigate this further, we once again examined plausible luminosity functions for single and dual high and low luminosity populations, based on observed intrinsic rates from the literature. The local population was once again found only to be produced to a sufficient level (while maintaining consistency with the observed overall number counts) by a separate low luminosity population with intrinsic rates several hundred times greater than their cosmological counterparts. Constraining the models via the Swift overall redshift distribution instead of threshold-adjusted BATSE number counts showed that the dual LF models were able to produce excellent fits to the entire redshift distribution while adequately reproducing a local population. Finally, suggestions are made as to the direction future work may follow in order to build on these initial investigations, as well as to how observations with future missions and detectors such as Fermi (formerly GLAST), Advanced LIGO and LOFAR may shed further light on nearby GRBs.

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