Tuning the functional properties of Silicon Carbide Thin Film and Nanowires

The present thesis has been devoted to the synthesis and investigation of functional properties of silicon carbide thin films and nanowires. The work took profit from the experience of the research group in the synthesis of 3C-SiC from vapour phase. 3C-SiC thin films Thin films heteroepitaxy on silicon substrates was carried out in a vapour phase epitaxy reactor. The initial efforts were committed to the process development in order to enhance the crystal quality of the epi-layer. The carbonization process and a buffer layer procedure were optimized in order to obtain good quality monocrystalline 3C-SiC layers. The films characterization was used not only to improve the entire process, but also to assess the crystalline quality and to identify the defects. Methyltrichlorosilane (MTS) was introduced during the synthesis to increase the growth rate and enhance crystalline quality. The effect of synthesis parameters such as MTS flow and process temperature was studied in order to promote defect density reduction and the release of the strain due to lattice mismatch between 3C-SiC and silicon substrate. In-growth n-type doping was implemented using a nitrogen gas line and the effect of different synthesis parameters on doping level was studied. Raman measurements allowed a contactless characterization and evaluation of electrically active dopant. The effect of MTS on nitrogen incorporation was investigated and a promotion of dopant concentration together with a higher growth rate were demonstrated. This result allows to obtain higher doping concentrations without deteriorating crystal quality in 3C-SiC and, to the best of our knowledge, it has never been demonstrated before. 3C-SiC nanowires Core-shell SiC-SiO2 nanowires were synthesized using a chemical vapour deposition technique in an open tube configuration reactor on silicon substrates. Metal catalyst were used to promote a uniaxial growth and a dense bundle of nanowires 100 µm long and 60 nm thick was obtained. Substrate preparation was found to be fundamental in order to obtain a uniform nanowire density. Morphological characterization was carried out using scanning electron microscopy and the analysis of structural, compositional, optical properties is reported.

Spectroscopic analysis of terrestrial analogues for the interpretation of surface composition of rocky bodies in the solar system. Effects of mineral mixing and particle size. Applications to moon, mars and implications for mercury.

Among the Solar System’s bodies, Moon, Mercury and Mars are at present, or have been in the recent years, object of space missions aimed, among other topics, also at improving our knowledge about surface composition. Between the techniques to detect planet’s mineralogical composition, both from remote and close range platforms, visible and near-infrared reflectance (VNIR) spectroscopy is a powerful tool, because crystal field absorption bands are related to particular transitional metals in well-defined crystal structures, e.g., Fe2+ in M1 and M2 sites of olivine or pyroxene (Burns, 1993). Thanks to the improvements in the spectrometers onboard the recent missions, a more detailed interpretation of the planetary surfaces can now be delineated. However, quantitative interpretation of planetary surface mineralogy could not always be a simple task. In fact, several factors such as the mineral chemistry, the presence of different minerals that absorb in a narrow spectral range, the regolith with a variable particle size range, the space weathering, the atmosphere composition etc., act in unpredictable ways on the reflectance spectra on a planetary surface (Serventi et al., 2014). One method for the interpretation of reflectance spectra of unknown materials involves the study of a number of spectra acquired in the laboratory under different conditions, such as different mineral abundances or different particle sizes, in order to derive empirical trends. This is the methodology that has been followed in this PhD thesis: the single factors previously listed have been analyzed, creating, in the laboratory, a set of terrestrial analogues with well-defined composition and size. The aim of this work is to provide new tools and criteria to improve the knowledge of the composition of planetary surfaces. In particular, mixtures composed with different content and chemistry of plagioclase and mafic minerals have been spectroscopically analyzed at different particle sizes and with different mineral relative percentages. The reflectance spectra of each mixture have been analyzed both qualitatively (using the software ORIGIN®) and quantitatively applying the Modified Gaussian Model (MGM, Sunshine et al., 1990) algorithm. In particular, the spectral parameter variations of each absorption band have been evaluated versus the volumetric FeO% content in the PL phase and versus the PL modal abundance. This delineated calibration curves of composition vs. spectral parameters and allow implementation of spectral libraries. Furthermore, the trends derived from terrestrial analogues here analyzed and from analogues in the literature have been applied for the interpretation of hyperspectral images of both plagioclase-rich (Moon) and plagioclase-poor (Mars) bodies.