Studio di popolazione sull'associazione tra sindrome delle gambe senza riposo ed emicrania

Introduzione: La sindrome delle gambe senza riposo (RLS) è un disturbo caratterizzato da sensazione spiacevole disestesica generalmente agli arti inferiori, che si presenta o peggiora nelle ore serali-notturne e che migliora con il movimento. Studi clinici hanno mostrato una maggiore prevalenza di RLS negli emicranici, mentre mancano studi condotti su popolazione generale non selezionata. Lo scopo di questo studio era quello di valutare la associazione tra emicrania e RLS in una popolazione italiana adulta. Inoltre è stata valutata l’associazione tra RLS e cefalea fenotipizzata attraverso metodica di principal components analysis (PCA). Materiali e metodi: la presenza di RLS e di emicrania è stata determinata attraverso questionari basati sui criteri diagnostici correnti in un campione di 1567 partecipanti di un fase preliminare di uno studio in corso sulla popolazione adulta della Val Venosta (BZ). Risultati: gli emicranici hanno presentato un significativo maggior rischio di soffrire di RLS rispetto ai non emicranici, anche dopo aggiustamento per fattori confondenti come età, sesso, depressione, ansia e qualità del sonno (p = 0.049). Questa associazione non era modificata dalla presenza di aura emicranica, di cause possibili di RLS secondaria e dalla frequenza di attacchi emicranici. Inoltre la RLS non era risultata significativamente associata alla cefalea di tipo tensivo (TTH). Dall’analisi di associazione tra RLS e cefalea fenotipizzata attraverso PCA era emerso che la componente 1, caratterizzata da sintomi di sensitivizzazione del sistema nervoso centrale (SNC), correlava significativamente con la presenza di RLS (p = 0.021). Conclusioni: RLS ed emicrania sono risultate associate nel nostro campione di popolazione adulta; inoltre la RLS ha mostrato una correlazione significativa con i sintomi di sensitivizzazione del SNC legati agli attacchi di cefalea. Questa associazione potrebbe risiedere in una possibile base patogenetica comune.

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.

Mass Loss in Population II Red Giants: an IRAC@Spitzer Survey of Galactic Globular Clusters

With the goal of studying ML along the RGB, mid-IR observations of a carefully selected sample of 17 Galactic globular clusters (GGCs) with different metallicity and horizontal branch (HB) morphology have been secured with IRAC on board Spitzer: a global sample counting about 8000 giant has been obtained. Suitable complementary photometry in the optical and near-IR has been also secured in order to properly characterize the stellar counterparts to the Spitzer sources and their photospheric parameters. Stars with color (i.e. dust) excess have been identified, their likely circumstellar emission quantified and modelled, and empirical estimates of mass loss rates and timescales obtained. We find that mass loss rates increases with increasing stellar luminosity and decreasing metallicity. For a given luminosity, we find that ML rates are systematically higher than the prediction by extrapolating the Reimers law. CMDs constructed from ground based near-IR and IRAC bands show that at a given luminosity some stars have dusty envelopes and others do not. From this, we deduce that the mass loss is episodic and is ``on'' for some fraction of the time. The total mass lost on the RGB can be easily computed by multiplying ML rates by the ML timescales and integrating over the evolutionary timescale. The average total mass lost moderately increases with increasing metallicity, and for a given metallicity is systematically higher in clusters with extended blue HB.