Ultra-high energy extragalactic neutrinos interacting with ultra-light dark matter

We show the results and discussions of the study of a possible suppression of the extragalactic neutrino flux during its propagation due to a nonstandard interaction with a candidate field to dark matter. In particular, we show the study of neutrino interaction with an ultra-light scalar field. It is shown that the extragalactic neutrino flux may be suppressed by such an interaction, leading to a mechanism to reduce the ultra-high energy neutrino flux. We calculate both the cases of non-self-conjugate as well as self-conjugate ultra-light dark matter. In the first case, the suppression is independent of the neutrino and dark matter masses. We conclude that care must be taken when explaining limits on the neutrino flux through source acceleration mechanisms only, since there could be other mechanisms, as absorption during propagation, for the reduction of the neutrino flux [1], © Published under licence by IOP Publishing Ltd.

Avaliação das técnicas TDR (Reflectometria por Domínio do Tempo) e moderação de nêutrons, na determinação do teor de água em diferentes classificações do solo

Pós-graduação em Agronomia (Energia na Agricultura) - FCA

Desenvolvimento de uma interface gráfica avançada para os programas DBWS-9807a e Size 2003 empregados no refinamento de estruturas cristalinas obtidas por DRX

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Produção e caracterização de maltodextrinas a partir de amidos de mandioca e batata-doce

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

Férmions em referenciais acelerados: desintegração de prótons e outras aplicações

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

Momento de dipolo elétrico do nêutron no modelo 3-3-1

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Estudo teórico da contribuição à dose de partículas secundárias geradas por prótons de energias entre 100 e 200 MeV num Phantom de substituto de tecido MS20

The goal of this project is the reproduction, through the simulation code based on the MCNPX (Monte Carlo N-Particle eXtended) v2.50 method, of the proton beam interaction with the material, since, in proton therapy, only the particle ionization and excitation are analyzed and the occurence of nuclear interactive inelastic process are not considered. This work will help the development of studies concerning the contribution to the total dosis of secondary particles generated by nuclear interaction in proton therapy. They are: alpha particles ( ), deuterium(2H), tritium (3H), neutron (n) and helium (3He). A MS20 tissue substitute phantom was used as the target and the energy of the proton beams was within an interest range of 100 to 200MeV. With the results obtained, it was possible to generate graphics which allows the analysis of the dosis deposition relation with and without nuclear interaction, the percentage of secondary particles deposited dosis, the radial dispersion of neutrons in the material, the secondary particles multiplicity, as well as the relation between the secondary particles spectrum with the próton generated spectrum

Estudo teórico da contribuição a dose de partículas secundárias geradas por prótons de energias entre 100-200 MeV num phantom de músculo estriado

In the treatment plans in conventional Proton therapy are considered only the elastic interactions of protons with electrons and/or nuclei, it means, mainly ionization and coulomb excitation processes. As the energy needed to reach the deep tumors should be of several hundred of MeVs, certainly the nuclear inelastic channels are open. Only some previous studies of the contribution of these processes in the full dose have been made towards targets composed of water. In this study will be presented the results of the simulation of the processes of interaction of beams of protons in the range of 100-200 MeV of energy with a cylindrical phantom composed by striated muscle (ICRU), emphasizing in the contribution to total dose due to the deposition of energy by secondary particles alpha (α), deuterium (2H), tritium (3H), neutron (n) and hélio3 (3He), originated by nuclear inelastic processes. The simulations were performed by using the method of Monte Carlo, via the computer code MCNPX v2.50 (Monte Carlo N-Particle eXtended). The results will be shown demonstrated through the graphics of the deposited dose with or without nuclear interaction, the percentual of dose deposited by secondary particles, the radial dispersion of neutrons, as well as the multiplicity of secondary particles

Estudo teórico da contribuição à dose de partículas secundárias geradas por Prótons de energias entre 100 e 200 MeV num Phantom de osso cortical

In proton therapy, the deposition of secondary particles energy originated by nuclear inelastic process (n, 2H, 3H, 3He and α) has a contribution in the total dose that deserves to be discussed. In calculations of plans implemented for routine treatment, the paid dose is calculated whereas the proton loses energy by ionization and or coulomb excitement. The contribution of inelastic processes associated with nuclear reactions is not considered. There are only estimates for pure materials or simple composition (water, for example), because of the difficulty of processing targets consisting of different materials. For this project, we use the Monte Carlo method employing the code MCNPX v2.50 (Monte Carlo N-Particle eXtended) to present results of the contribution to the total dose of secondary particles. In this work, it was implemented a cylindrical phantom composed by cortical bone, for proton beams between 100 and 200 MeV. With the results obtained, it was possible to generate graphics to analyze: the dose deposition relation with and without nuclear interaction, the multiplicity and percentage of deposited dose for each secondary particle and a radial dispersion of neutrons in the material

Confecção e caracterização de filmes finos de boro para a medida da taxa de reação 10B(N, a)7LI na terapia por captura de nêutrons pelo boro

The Boron Neutron Capture Therapy (BNCT), based on the 10B(n,α)7Li reaction, represents a promising modality for the treatment of cancers that are resistents to conventional treatments. So, it is necessary to find drugs (boron compounds) with high selectivity for each type of cancer, the neutrons source should be well characterized and the rate of 10B(n,α)7Li reaction should be measured with great accuracy as possible. This study aimed to develop a method for manufacturing thin films of boron, for measure the 10B(n,α)7Li reaction, and analyze the uniformity of the films. Five thin films of boron were manufactured with three different concentrations of boric acid, heated to transform the acid in boron, irradiated with thermic neutrons coupled to CR-39 detectors, in BNCT line at the reactor IEA-R1 IPEN/CNEN, São Paulo. After the irradiation, the detectors were chemically attacked with NaOH to reveal the tracks. The methodology presented is effective because it resulted in deposition of boron as thin film enabling the quantitative analysis of 10B(n,α)7Li reaction. The analysis of the uniformity of density of the induced tracks in CR-39 shows that, in most of the films, there is no uniformity in surface distribution of boron, but when the film is divided, we obtain some uniform sectors

Produção de partículas secundárias em reações de “spallation” induzidas por prótons

Cosmic radiation has been identi ed as one of the main hazard to crew, aircraft and sensitive equipments involved in long-term missions and even high-altitude commercial ights. Generally, shields are used in spatial units to avoid excessive exposure, by holding the incident radiation. Unfortunatelly, shielding in space is problematic, especially when high-energy cosmic particles are considered, due to the production of large number of secondary particles, mainly neutrons, protons and alpha particles, caused by spallation reactions and quasi-elastic processes of the corpuscular radiation with the shield. Good parameters for checking the secondary particle production at target material are diferential cross section and energy deposited in the shield. Addition experiments, some computer codes based on Monte Carlo method show themselves a suitable tool to calculate shield parameters, due to have evaluated nuclear data libraries implemented on the algorithm. In view of this, the aim of this work is determining the parameters evaluated in shielding materials, by using MCNPX code, who shows good agreement with experimental data from literature. Among the materials, Aluminium had lower emission and production of secondary particles

Three-body Faddeev calculation for 11Li with separable potentials

The halo nucleus 11Li is treated as a three-body system consisting of an inert core of 9Li plus two valence neutrons. The Faddeev equations are solved using separable potentials to describe the two-body interactions, corresponding in the n-9Li subsystem to a p1/2 resonance plus a virtual s-wave state. The experimental 11Li energy is taken as input and the 9Li transverse momentum distribution in 11Li is studied. [S0556-2813(99)01703-3].

K-41(n, gamma)K-42 thermal and resonance integral cross section measurements

We measured the K-41 thermal neutron absorption and resonance integral cross sections after the irradiation of KNO3 samples near the core of the IEA-R1 IPEN pool-type research reactor. Bare and cadmium-covered targets were irradiated in pairs with Au-Al alloy flux-monitors. The residual activities were measured by gamma-ray spectroscopy with a HPGe detector, with special care to avoid the K-42 decay beta(-) emission effects on the spectra. The gamma-ray self-absorption was corrected with the help of MCNP simulations. We applied the Westcott formalism in the average neutron flux determination and calculated the depression coefficients for thermal and epithermal neutrons due to the sample thickness with analytical approximations. We obtained 1.57(4) and 1.02(4) b, for thermal and resonance integral cross sections, respectively, with correlation coefficient equal to 0.39.

New structures in the continuum of C-15 populated by two-neutron transfer

The C-13(O-18,O-16)C-15 reaction has been studied at 84 MeV incident energy. The ejectiles have been detected at forward angles and C-15 excitation energy spectra have been obtained up to about 20 MeV. Several known bound and resonant states of C-15 have been identified together with two unknown structures at 10.5 MeV (FWHM = 2.5 MeV) and 13.6 MeV (FWHM = 2.5 MeV). Calculations based Oil the removal of two uncorrelated neutrons from the projectile describe a significant part of the continuum observed in the energy spectra. In particular the structure at 10.5 MeV is dominated by a resonance of C-15 near the C-13 + n + n threshold. Similar structures are found in nearby nuclei such as C-14 and Be-11. (c) 2012 Elsevier BM. All rights reserved.

Stellar Models in General Relativity

Neutron stars are some of the most fascinating objects in Nature. Essentially all aspects of physics seems to be represented inside them. Their cores are likely to contain deconfined quarks, hyperons and other exotic phases of matter in which the strong interaction is the dominant force. The inner region of their solid crust is penetrated by superfluid neutrons and their magnetic fields may reach well over 1012 Gauss. Moreover, their extreme mean densities, well above the densities of nuclei, and their rapid rotation rates makes them truly relativistic both in the special as well as in the general sense. This thesis deals with a small subset of these phenomena. In particular the exciting possibility of trapping of gravita-tional waves is examined from a theoretical point of view. It is shown that the standard condition R < 3M is not essential to the trapping mechanism. This point is illustrated using the elegant tool provided by the optical geometry. It is also shown that a realistic equation of state proposed in the literature allows stable neutron star models with closed circular null orbits, something which is closely related to trapped gravitational waves. Furthermore, the general relativistic theory of elasticity is reviewed and applied to stellar models. Both static equilibrium as well as radially oscillating configurations with elasticsources are examined. Finally, Killing tensors are considered and their applicability to modeling of stars is discussed