A study of the turbulence of the neutral medium in two nearby spiral galaxies

The width of the 21 cm line (HI) emitted by spiral galaxies depends on the physical processes that release energy in the Interstellar Medium (ISM). This quantity is called velocity dispersion (σ) and it is proportional first of all to the thermal kinetic energy of the gas. The accepted theoretical picture predicts that the neutral hydrogen component (HI) exists in the ISM in two stable phases: a cold one (CNM, with σ~0.8 km/s) and a warm one (WNM, with σ~8 km/s). However, this is called into question by the observation that the HI gas has usually larger velocity dispersions. This suggests the presence of turbulence in the ISM, although the energy sources remain unknown. In this thesis we want to shed new light on this topic. We have studied the HI line emission of two nearby galaxies: NGC6946 and M101. For the latter we used new deep observations obtained with the Westerbork radio interferometer. Through a gaussian fitting procedure, we produced dispersion maps of the two galaxies. For both of them, we compared the σ values measured in the spiral arms with those in the interarms. In NGC6946 we found that, in both arms and interarms, σ grows with the column density, while we obtained the opposite for M 101. Using a statistical analysis we did not find a significant difference between arm and interarm dispersion distributions. Producing star formation rate density maps (SFRD) of the galaxies, we studied their global and local relations with the HI kinetic energy, as inferred from the measured dispersions. For NGC6946 we obtained a good log-log correlation, in agreement with a simple model of supernova feedback driven turbulence. This shows that in this galaxy turbulent motions are mainly induced by the stellar activity. For M 101 we did not find an analogous correlation, since the gas kinetic energy appears constant with the SFRD. We think that this may indicate that in this galaxy turbulence is driven also by accretion of extragalactic material.

Caratteristiche di emissione delle regioni HII

Le regioni HII sono nubi di idrogeno ionizzato da stelle di recente formazione, massicce e calde. Tali stelle, spesso raggruppate in ammassi, emettono copiosamente fotoni di lunghezza d’onda λ ≤ 912 Å, capaci di ionizzare quasi totalmente il gas che le circonda, composto prevalentemente da idrogeno, ma in cui sono presenti anche elementi ionizzati più pesanti, come He, O, N, C e Ne. Le dimensioni tipiche di queste regioni vanno da 10 a 100 pc, con densità dell’ordine di 10 cm−3. Queste caratteristiche le collocano all’interno del WIM (Warm Ionized Medium), che, insieme con HIM (Hot Ionized Medium), WNM (Warm Neutral Medium) ed CNM (Cold Neutral Medium), costituisce la varietà di fasi in cui si presenta il mezzo interstellare (ISM, InterStellar Medium). Il tema che ci prestiamo ad affrontare è molto vasto e per comprendere a fondo i processi che determinano le caratteristiche delle regioni HII sarebbero necessarie molte altre pagine; lo scopo che questo testo si propone di raggiungere, senza alcuna pretesa di completezza, è dunque quello di presentare l’argomento, approfondendone ed evidenziandone alcuni particolari tratti. Prima di tutto descriveremo le regioni HII in generale, con brevi indicazioni in merito alla loro formazione e struttura. A seguire ci concentreremo sulla descrizione dei processi che determinano gli spettri osservati: inizialmente mostreremo quali siano i processi fisici che generano l’emissione nel continuo, concentrandoci poi su quello più importante, la Bremmstrahlung. Affronteremo poi una breve digressione riguardo al processo di ricombinazione ione-elettrone nei plasmi astrofisici ed alle regole di selezione nelle transizioni elettroniche, concetti necessari per comprendere ciò che segue, cioè la presenza di righe in emissione negli spettri delle regioni foto-ionizzate. Infine ci soffermeremo sulle regioni HII Ultra-Compatte (UC HII Region), oggetto di numerosi recenti studi.

Microfluidic microbial fuel cell fabrication and rapid screening of electrochemically microbes

The demand for novel renewable energy sources, together with the new findings on bacterial electron transport mechanisms and the progress in microbial fuel cell design, have raised a noticeable interest in microbial power generation. Microbial fuel cell (MFC) is an electrochemical device that converts organic substrates into electricity via catalytic conversion by microorganism. It has represented a continuously growing research field during the past few years. The great advantage of this device is the direct conversion of the substrate into electricity and in the future, MFC may be linked to municipal waste streams or sources of agricultural and animal waste, providing a sustainable system for waste treatment and energy production. However, these novel green technologies have not yet been used for practical applications due to their low power outputs and challenges associated with scale-up, so in-depth studies are highly necessary to significantly improve and optimize the device working conditions. For the time being, the micro-scale MFCs show great potential in the rapid screening of electrochemically active microbes. This thesis presents how it will be possible to optimize the properties and design of the micro-size microbial fuel cell for maximum efficiency by understanding the MFC system. So it will involve designing, building and testing a miniature microbial fuel cell using a new species of microorganisms that promises high efficiency and long lifetime. The new device offer unique advantages of fast start-up, high sensitivity and superior microfluidic control over the measured microenvironment, which makes them good candidates for rapid screening of electrode materials, bacterial strains and growth media. It will be made in the Centre of Hybrid Biodevices (Faculty of Physical Sciences and Engineering, University of Southampton) from polymer materials like PDMS. The eventual aim is to develop a system with the optimum combination of microorganism, ion exchange membrane and growth medium. After fabricating the cell, different bacteria and plankton species will be grown in the device and the microbial fuel cell characterized for open circuit voltage and power. It will also use photo-sensitive organisms and characterize the power produced by the device in response to optical illumination.