Synthesis of Na-PSS geopolymers and analysis of the H2O/Na2O molar ratio influence over their mechanical properties

Geopolymers are solid aluminosilicate material made by mixing an activating solution and a solid precursor. This work studied the mechanisms of synthesis of metakaolin-based geopolymers and the influence of water content, described by the molar ratio H2O/Na2O, on the final product. The samples were tested using a Uniaxial Compressive Test (UCT) to define their compressive resistance. Two geopolymers series were synthetized and let them rest for 7- days and 28-days, each of them composed by six different sets. 7-day rest series showed that water addition had no relevant effect over its resistance while the 28-day rest series almost doubled the compressive resistance, although those with the highest H2O/Na2O molar ratio showed instead a drastic reduction. Two other series were synthesized by adding silt aggregate, a waste material obtained in the production of aggregate for concrete, corresponding to 10wt% and 20wt%of the metakaolin used. After 28 days of aging, these samples were tested via UCT to measure the variation of the compressive resistance after the silt addition. The aggregate has disruptive effects over the compressive resistance, but the 20wt% samples achieved a higher compressive resistance. Samples with highest and lowest compressive resistance have been chosen to carry out an XRD analysis. In all the samples it has been recognized the presence of Anatase (TiO2), a titanium oxide found in the metakaolin and Thermonatrite, a hydrated sodium carbonate [Na2CO3 • (H2O)]. Scanning Electron Microscopy was carried out on the samples with the highest compressive resistance and showed that the samples with lower water content developed a homogeneous geopolymeric texture, while those with higher water content showed instead a spongy-like texture and a higher air or pore solution bubbles presence. Silt/geopolymer composites showed a fracture system developing across the interstitial transition zone between the geopolymer matrix and the aggregate particle.

Caratteristiche principali dell'emissione di galassie a spirale

L’universo è il luogo che permette agli esseri umani di osservare i fenomeni fondamentali che regolano le leggi della fisica e della natura. La luce e quindi la radiazione elettromagnetica è ciò che gli astronomi utilizzano e studiano, per conoscere i meccanismi principali che governano la moltitudine di corpi celesti presenti nel cosmo. Tra questi le galassie a spirale, crogiolo di oggetti e fenomeni che permettono lo studio dell’evoluzione e dell’avanzamento dell’universo. In questo elaborato verranno presentate le loro peculiarità prestando attenzione alla loro morfologia, composizione e ai principali processi di emissione di radiazione andandone ad analizzare le diverse bande dello spettro elettromagnetico

Emissione di Bremsstrahlung e applicazioni astrofisiche

Scopo di questo elaborato è studiare il processo di emissione di radiazione chiamato Bremsstrahlung, parola tedesca che letteralmente vuol dire radiazione di frenamento e che indica la radiazione emessa da una carica elettrica accelerata dal campo coulombiano di un’altra carica. L’emissione di Bremsstrahlung avviene nel continuo e interessa un ampio intervallo di lunghezze d’onda, che va dalle onde radio fino ai raggi γ. Nel capitolo 1 tratteremo sia la radiazione prodotta da un singolo evento, sia quella prodotta da un plasma reale. Successivamente, ci concentreremo sulla Bremsstrahlung termica, approfondendo anche la questione dell’autoassorbimento e della brillanza di Bremsstrahlung. Il capitolo si chiude con la descrizione della Bremsstrahlung relativistica. Nel capitolo 2 descriveremo invece alcuni oggetti astrofisici in cui la Bremsstrahlung gioca un ruolo importante (il mezzo interstellare e le regioni HII, il mezzo intracluster) e concluderemo accennando al ruolo che questo processo radiativo ha nelle cascate elettromagnetiche nell’atmosfera terrestre che consentono lo studio dei raggi γ.

The molecular gas content of star-forming galaxies in the ALPINE fields.

In this thesis, I aim to study the evolution with redshift of the gas mass fraction of a sample of 53 sources (from z ∼ 0.5 to z > 5) serendipitously detected in ALMA band 7 as part of the ALMA Large Program to INvestigate C II at Early Times (ALPINE). First, I used SED-fitting software CIGALE, which is able to implement energy balancing between the optical and the far infrared part, to produce a best-fit template of my sources and to have an estimate of some physical properties, such as the star formation rate (SFR), the total infrared luminosity and the total stellar mass. Then, using the tight correlation found by Scoville et al. (2014) between the ISM molecular gas mass and the rest-frame 850 μm luminosity, I used the latter, extrapolating it from the best-fit template using a code that I wrote in Python, as a tracer for the molecular gas. For my sample, I then derived the most important physical properties, such as molecular gas mass, gas mass fractions, specific star formation rate and depletion timescales, which allowed me to better categorize them and find them a place within the evolutionary history of the Universe. I also fitted our sources, via another code I wrote again in Python, with a general modified blackbody (MBB) model taken from the literature (Gilli et al. (2014), D’Amato et al. (2020)) to have a direct method of comparison with similar galaxies. What is evident at the end of the paper is that the methods used to derive the physical quantities of the sources are consistent with each other, and these in turn are in good agreement with what is found in the literature.