B14. Interferenza.

Trasparenze presentate a lezione. Si consiglia agli studenti di stamparne una copia prima della lezione e di portarla con sé onde riportare su di essa ulteriori annotazioni.

BE01. Esercizi risolti di elettrostatica.

Trasparenze presentate a lezione. Si consiglia agli studenti di stamparne una copia prima della lezione e di portarla con sé onde riportare su di essa ulteriori annotazioni.

BE02. Esercizi risolti di elettrodinamica.

Trasparenze presentate a lezione. Si consiglia agli studenti di stamparne una copia prima della lezione e di portarla con sé onde riportare su di essa ulteriori annotazioni.

BE03. Esercizi risolti di ottica.

Trasparenze presentate a lezione. Si consiglia agli studenti di stamparne una copia prima della lezione e di portarla con sé onde riportare su di essa ulteriori annotazioni.

EE03. Esercizi di esame di Elettromagnetismo con risultati

Esercizi di esame per i corsi di Fisica Generale. I compiti di esame contengono esercizi sorteggiati da questa lista, nell'ultima versione disponibile sul Web 15 giorni prima della data di esame. I punteggi riportati a fianco dei quesiti/esercizi sono calcolati dinamicamente sulla base dei precedenti risultati nelle prove di esame, in modo da rendere il secondo terzile della distribuzione dei voti sul singolo esercizio pari a 3/3. In altre parole il punteggio assegnato al singolo quesito/esercizio è tale da assicurare che un terzo degli studenti che hanno affrontato l'esercizio ottenga la massima valutazione. Il punteggio degli esercizi riportato sul file è indicativo. Esso si modifica dinamicamente a ogni esame, in modo che a ogni esame diviene una valutazione più precisa della difficoltà dell'esercizio (all'aumentare della statistica sperimentale l'errore di misura diminuisce).

EQ03. Quesiti di esame di Elettromagnetismo

Quesiti di esame per i corsi di Fisica Generale. I compiti di esame contengono quesiti sorteggiati da questa lista, nell'ultima versione disponibile sul Web 15 giorni prima della data di esame. I punteggi riportati a fianco dei quesiti/esercizi sono calcolati dinamicamente sulla base dei precedenti risultati nelle prove di esame, in modo da rendere il secondo terzile della distribuzione dei voti sul singolo esercizio pari a 3/3. In altre parole il punteggio assegnato al singolo quesito/esercizio è tale da assicurare che un terzo degli studenti che hanno affrontato l'esercizio ottenga la massima valutazione. Il punteggio degli esercizi riportato sul file è indicativo. Esso si modifica dinamicamente a ogni esame, in modo che a ogni esame diviene una valutazione più precisa della difficoltà dell'esercizio (all'aumentare della statistica sperimentale l'errore di misura diminuisce).

A spectroscopic and photometric study of MSP companions in Galactic Globular Clusters

This Thesis is devoted to the study of the optical companions of Millisecond Pulsars in Galactic Globular Clusters (GCs) as a part of a large project started at the Department of Astronomy of the Bologna University, in collaboration with other institutions (Astronomical Observatory of Cagliari and Bologna, University of Virginia), specifically dedicated to the study of the environmental effects on passive stellar evolution in galactic GCs. Globular Clusters are very efficient “Kilns” for generating exotic object, such as Millisecond Pulsars (MSP), low mass X-ray binaries(LMXB) or Blue Straggler Stars (BSS). In particular MSPs are formed in binary systems containing a Neutron Star which is spun up through mass accretion from the evolving companion (e.g. Bhattacharia & van den Heuvel 1991). The final stage of this recycling process is either the core of a peeled star (generally an Helium white dwarf) or a very light almos exhausted star, orbiting a very fast rotating Neutron Star (a MSP). Despite the large difference in total mass between the disk of the Galaxy and the Galactic GC system (up a factor 103), the percentage of fast rotating pulsar in binary systems found in the latter is very higher. MSPs in GCs show spin periods in the range 1.3 ÷ 30ms, slowdown rates ˙P 1019 s/s and a lower magnetic field, respect to ”normal” radio pulsars, B 108 gauss . The high probability of disruption of a binary systems after a supernova explosion, explain why we expect only a low percentage of recycled millisecond pulsars respect to the whole pulsar population. In fact only the 10% of the known 1800 radio pulsars are radio MSPs. Is not surprising, that MSP are overabundant in GCs respect to Galactic field, since in the Galactic Disk, MSPs can only form through the evolution of primordial binaries, and only if the binary survives to the supernova explosion which lead to the neutron star formation. On the other hand, the extremely high stellar density in the core of GCs, relative to most of the rest of the Galaxy, favors the formation of several different binary systems, suitable for the recycling of NSs (Davies at al. 1998). In this thesis we will present the properties two millisecond pulsars companions discovered in two globular clusters, the Helium white dwarf orbiting the MSP PSR 1911-5958A in NGC 6752 and the second case of a tidally deformed star orbiting an eclipsing millisecond pulsar, PSR J1701-3006B in NGC6266

A spectroscopic and photometric study of stellar populations in a sample of clusters in the Magellanic Clouds

This Ph.D. Thesis has been carried out in the framework of a long-term and large project devoted to describe the main photometric, chemical, evolutionary and integrated properties of a representative sample of Large and Small Magellanic Cloud (LMC and SMC respectively) clusters. The globular clusters system of these two Irregular galaxies provides a rich resource for investigating stellar and chemical evolution and to obtain a detailed view of the star formation history and chemical enrichment of the Clouds. The results discussed here are based on the analysis of high-resolution photometric and spectroscopic datasets obtained by using the last generation of imagers and spectrographs. The principal aims of this project are summarized as follows: • The study of the AGB and RGB sequences in a sample of MC clusters, through the analysis of a wide near-infrared photometric database, including 33 Magellanic globulars obtained in three observing runs with the near-infrared camera SOFI@NTT (ESO, La Silla). • The study of the chemical properties of a sample of MCs clusters, by using optical and near-infrared high-resolution spectra. 3 observing runs have been secured to our group to observe 9 LMC clusters (with ages between 100 Myr and 13 Gyr) with the optical high-resolution spectrograph FLAMES@VLT (ESO, Paranal) and 4 very young (<30 Myr) clusters (3 in the LMC and 1 in the SMC) with the near-infrared high-resolution spectrograph CRIRES@VLT. • The study of the photometric properties of the main evolutive sequences in optical Color- Magnitude Diagrams (CMD) obtained by using HST archive data, with the final aim of dating several clusters via the comparison between the observed CMDs and theoretical isochrones. The determination of the age of a stellar population requires an accurate measure of the Main Sequence (MS) Turn-Off (TO) luminosity and the knowledge of the distance modulus, reddening and overall metallicity. For this purpose, we limited the study of the age just to the clusters already observed with high-resolution spectroscopy, in order to date only clusters with accurate estimates of the overall metallicity.

Properties of gas and dark matter in X-ray galaxy clusters with Sunyaev Zel'dovich measurements

I have studied entropy profiles obtained in a sample of 24 X-ray objects at high redshift retrieved from the Chandra archive. I have discussed the scaling properties of the entropy S, the correlation between metallicity Z and S, the profiles of the temperature of the gas, Tgas, and performed a comparison between the dark matter 'temperature' and Tgas in order to constrain the non-gravitational processes which affect the thermal history of the gas. Furthermore I have studied the scaling relations between the X-ray quantities and Sunyaev Zel'dovich measurements. I have observed that X-ray laws are steeper than the relations predicted from the adiabatic model. These deviations from expectations based on self-similarity are usually interpreted in terms of feedback processes leading to non-gravitational gas heating, and suggesting a scenario in which the ICM at higher redshift has lower both X-ray luminosity and pressure in the central regions than the expectations from self-similar model. I have also investigated a Bayesian X-ray and Sunyaev Zel'dovich analysis, which allows to study the external regions of the clusters well beyond the volumes resolved with X-ray observations (1/3-1/2 of the virial radius), to measure the deprojected physical cluster properties, like temperature, density, entropy, gas mass and total mass up to the virial radius.