The Status of Multi-Dimensional Core-Collapse Supernova Models

Models of neutrino-driven core-collapse supernova explosions have matured considerably in recent years. Explosions of low-mass progenitors can routinely be simulated in 1D, 2D, and 3D. Nucleosynthesis calculations indicate that these supernovae could be contributors of some lighter neutron-rich elements beyond iron. The explosion mechanism of more massive stars remains under investigation, although first 3D models of neutrino-driven explosions employing multi-group neutrino transport have become available. Together with earlier 2D models and more simplified 3D simulations, these have elucidated the interplay between neutrino heating and hydrodynamic instabilities in the post-shock region that is essential for shock revival. However, some physical ingredients may still need to be added/improved before simulations can robustly explain supernova explosions over a wide range of progenitors. Solutions recently suggested in the literature include uncertainties in the neutrino rates, rotation, and seed perturbations from convective shell burning. We review the implications of 3D simulations of shell burning in supernova progenitors for the ‘perturbations-aided neutrino-driven mechanism,’ whose efficacy is illustrated by the first successful multi-group neutrino hydrodynamics simulation of an 18 solar mass progenitor with 3D initial conditions. We conclude with speculations about the impact of 3D effects on the structure of massive stars through convective boundary mixing.

Comparison of digital imaging systems for neutron radiography

FAPESP:95/02610

Boron uptake in normal melanocytes and melanoma cells and boron biodistribution study in mice bearing B16F10 melanoma for boron neutron capture therapy

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

Artificial Neural Network and Neutron Aplication in a Volume Fraction Calculation in Annular and Stratified Multiphase System

Multiphase flows, type oil–water-gas are very common among different industrial activities, such as chemical industries and petroleum extraction, and its measurements show some difficulties to be taken. Precisely determining the volume fraction of each one of the elements that composes a multiphase flow is very important in chemical plants and petroleum industries. This work presents a methodology able to determine volume fraction on Annular and Stratified multiphase flow system with the use of neutrons and artificial intelligence, using the principles of transmission/scattering of fast neutrons from a 241Am-Be source and measurements of point flow that are influenced by variations of volume fractions. The proposed geometries used on the mathematical model was used to obtain a data set where the thicknesses referred of each material had been changed in order to obtain volume fraction of each phase providing 119 compositions that were used in the simulation with MCNP-X –computer code based on Monte Carlo Method that simulates the radiation transport. An artificial neural network (ANN) was trained with data obtained using the MCNP-X, and used to correlate such measurements with the respective real fractions. The ANN was able to correlate the data obtained on the simulation with MCNP-X with the volume fractions of the multiphase flows (oil-water-gas), both in the pattern of annular flow as stratified, resulting in a average relative error (%) for each production set of: annular (air= 3.85; water = 4.31; oil=1.08); stratified (air=3.10, water 2.01, oil = 1.45). The method demonstrated good efficiency in the determination of each material that composes the phases, thus demonstrating the feasibility of the technique.

Le Blue Straggler Stars e le popolazioni multiple in quattro ammassi globulari galattici

In questo elaborato viene presentato lo studio fotometrico di quattro ammassi globulari galattici. I target di questa Tesi fanno parte della HST UV Legacy Survey degli ammassi globulari galattici (Piotto et al. 2015). Nell'ambito di questa survey sono stati osservati, in modo omogeneo, 57 ammassi globulari galattici con il telescopio spaziale Hubble e la camera WFC3, in tre bande fotometriche ultraviolette e blu. Un dataset così composto è adatto a numerosi scopi, tra cui lo studio delle popolazioni calde come le BSS e delle popolazioni multiple. Sono stati selezionati quattro ammassi particolarmente popolosi e tra i più densi del campione, allo scopo di mettere a punto indicatori di evoluzione dinamica e comprendere il ruolo di quest'ultima sulle proprietà delle popolazioni multiple presenti nei sistemi selezionati. Lo studio dell'evoluzione dinamica è stato effettuato tramite la distribuzione radiale delle BSS (Blue Straggler Stars), che è stato dimostrato esserne un efficiente indicatore (Ferraro et al. 2012). I risultati ottenuti evidenziano chiaramente che tutti gli ammassi selezionati si trovano in fasi avanzate di evoluzione dinamica, come suggerito dall'alta densità che li caratterizza. Anche lo studio delle proprietà delle popolazioni multiple, ovvero sottopopolazioni con differenti abbondanze chimiche di elementi leggeri, la cui presenza è stata recentemente osservata negli ammassi globulari, è stato effettuato tramite lo studio della loro distribuzione radiale. Tra i quattro casi analizzati, soltanto M 15 ha mostrato una separazione significativa tra le distribuzioni radiali delle due popolazioni.

Abbondanze chimiche delle Blue Straggler Stars dell'ammasso aperto NGC 188

My Thesis work is aimed at searching for evidence of CO-depletion in the atmosphere of these objects. To this end, I am analyzing high-resolution spectra recently acquired with the spectrograph HDS at the Subaru Telescope. The global sample is composed of 5 BSSs with hot WD companions, 3 additional binary BSSs with no a significant far-UV excess, and one "normal" stars (along the RGB star) needed for comparison. The analysis will provide us with the surface chemical abundances (especially of C and O) of the target stars. The final goal is to verify the expected {chemical signature} and put constraints on its characteristic time scale (for instance, a positive detection in the 5 BSSs with hot companions and a non-detection in the other 3 binary BSSs would imply that CO-depletion is a transient phenomenon, lasting approx 300 Myr only). The analysis will also provide us with the rotational velocities of each target, thus allowing to investigate their kinematical properties and shed new light on their evolutionary path.

Resolved Stars' Insights into Galaxy Physics

Thesis (Ph.D.)--University of Washington, 2016-08