A comparison between vertical mixing parameterizations in the Levantine Sea

The goal of this thesis was the study of an optimal vertical mixing parameterization scheme in a mesoscale dominated field characterized from a strong vorticity and the presence of a layer of colder, less saline water at about 100 m depth (Atlantic Waters); in these conditions we compared six different experiments, that differ by the turbulent closure schemes, the presence or not of an enhanced diffusion parameterization and the presence or not of a double diffusion mixing parameterization. To evaluate the performance of the experiments and the model we compared the simulations with the ARGO observations of temperature and salinity available in our domain, in our period of interest. The conclusions were the following: • the increase of the resolution gives better results in terms of temperature in all the considered cases, and in terms of salinity. • The comparisons between the Pacanovski-Philander and the TKE turbulent closure schemes don’t show significant differences when the simulations are compared to the observations. • The removing of the enhanced diffusion parameterization in presence of the TKE turbulent closure submodel doesn’t give positive results, and show limitations in the resolving of gravitational instabilities near the surface • The k-ϵ turbulent closure model utilized in all the GLS experiments, is the best performing closure model among the three considered, with positive results in all the salinity comparison with the in situ observation and in most of the temperature comparisons. • The double mixing parameterization utilized in the k-ϵ closure submodel improves the results of the experiments improving both the temperature and salinity in comparison with the ARGO data.

Experimental analysis of the aerodynamic and mixing performance of a ventilation device

Numerous types of acute respiratory failure are routinely treated using non-invasive ventilatory support (NIV). Its efficacy is well documented: NIV lowers intubation and death rates in various respiratory disorders. It can be delivered by means of face masks or head helmets. Currently the scientific community’s interest about NIV helmets is mostly focused on optimising the mixing between CO2 and clean air and on improving patient comfort. To this end, fluid dynamic analysis plays a particularly important role and a two- pronged approach is frequently employed. While on one hand numerical simulations provide information about the entire flow field and different geometries, they exhibit require huge temporal and computational resources. Experiments on the other hand help to validate simulations and provide results with a much smaller time investment and thus remain at the core of research in fluid dynamics. The aim of this thesis work was to develop a flow bench and to utilise it for the analysis of NIV helmets. A flow test bench and an instrumented mannequin were successfully designed, produced and put into use. Experiments were performed to characterise the helmet interface in terms of pressure drop and flow rate drop over different inlet flow rates and outlet pressure set points. Velocity measurements by means of Particle Image Velocimetry were performed. Pressure drop and flow rate characteristics from experiments were contrasted with CFD data and sufficient agreement was observed between both numerical and experimental results. PIV studies permitted qualitative and quantitative comparisons with numerical simulation data and offered a clear picture of the internal flow behaviour, aiding the identification of coherent flow features.

Investigating stellar mixing processes through the study of the Red-Giant Branch bump

Extra mixing at the borders of convective zones in stellar interiors takes on an important role in the chemical evolution of stars and galaxies through the transport of chemical elements towards the stellar surface: knowing the overshooting mechanism can therefore lead to a better understanding of the observed chemical abundances in stellar photospheres. The comprehension of this phenomenon is quite uncertain and currently object of many studies. In particular, concerning low mass stars, in the past decades several works highlighted a discrepancy between the observed luminosity of the Red-Giant Branch bump and its prediction from simulations, which can be fixed including overshooting at the base of the convective envelope. This work, studying the Red-Giant Branch bump and using it as a diagnostic for extra mixing processes, tries to classify two different types of overshooting, instantaneous and diffusive, using both simulations from stellar models and Globular Clusters’ data. The aim is to understand which one of the two mixing processes is the most suitable in reproducing the observed stellar behaviour and, in case both of them provide reliable results, what are the conditions under which they produce the same effects on the Red-Giant Branch bump luminosity function and are consequently indistinguishable. Finally, possible dependences of overshooting efficiency on stellar parameters, such as chemical composition, are analysed.