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Les éléments transposables (ET) sont des séquences d’ADN capables de catalyser son propre mouvement et d’entrer dans de nouvelles régions du génome. Dans la présente étude, nous avons étudié Helena, un élément LINE qui est à différents stades de son cycle évolutif et donc, il est un bon modèle pour l’étude de la dynamique évolutive des TE. À travers une analyse de bio-informatique dans les douze génomes séquencés de la drosophile nous avons étudié l’évolution de Helena, et nous proposons un scénario possible pour l’évolution de cet élément. Helena est à différents stades de son cycle de vie, allant d’un état complet (D. simulans et D. mojavensis) à très dégradé (D. yakuba, D.erecta, D. ananassae et D. virilis) ou absent (D. pseudoobscura, D. persimilis, D. grimshawi et d. willistoni). L’analyse phylogénétique a montré que Helena était présent chez l’ancêtre commun du genre Drosophila et a été transmis verticalement dans des lignées dérivées. De plus, nous avons détectées des copies intactes uniquement chez D. mojavensis et nous avons étudié plus en détail sa région 5’ (extrémité). Nous avons utilisé un gène rapporteur et confirmé la présence du promoteur interne pour Pol II qui est associé à des modifications épigénétiques de l’histone : hétérochromatine permissive (H3K4me2) et répressive (H3K27me3). Ces « marques bivalents » indiquent que Helena peuvent être exprimés en réponse à un stimulus spécifique. Une étude de l’élément BS, un TE étroitement liée à Helena, a montré que la dynamique évolutive des deux ETs sont très similaires. Les résultats montrent que CET élément, comme Helena, se trouve à différents stades de son cycle évolutif / The transposable elements (TEs) are DNA sequences capable of catalyze its own movement and to enter into new regions of the genome. In the present study we studied Helena, a LINE element that is at different stages of its evolutionary cycle and therefore, it is a good model for studies of TEs evolutionary dynamics. Through bioinformatics analysis of 12 Drosophila species which have their genomes sequenced, we found Helena in different stages of its evolutionary cycle, that varies of at least one full active copy (D. mojavensis) an putatively complete copy, but inactive (D. simulans) to highly degenerate (D. yakuba, D. erecta, D. ananassae and D. virilis) or absent (D. pseudoobscura, D. persimilis, D. willistoni and D. grimshawi) sequences. Phylogenetic analysis showed that Helena was present in the common ancestor of the Drosophila genus and has been vertically transmitted in derived lineages, but lost on some of them. Since a complete highly active copy was observed only in D. mojavensis, we studied in more detail its 5' end region. We used a reporter gene and verified the presence of internal promoter for Pol II that is associated with epigenetic histone modifications for permissive (H3K4me2) and repressive heterochromatin (H3K27me3). These “bivalent marks” indicate that Helena can be expressed in response to specific stimulus. A study of BS element, a TE closely related to Helena, showed that the evolutionary dynamics of both TEs are very similar. Bioinformatics analysis of the 12 Drosophila genomes revealed that BS is also widely variable in the species analyzed regarding to distribution, abundance, degree of degradation and also about their evolutionary cycle

The theory of stellar evolution and stellar structure relies on the observation of stars in di erent phases of their evolutionary cycle. The relation between observations and theory can be strengthened by obtaining observational data of a large sample of stars in a particular evolutionary phase. The search for Cephei stars, as conducted in this study, can contribute to the sample of known Cephei stars, where these interesting stars are massive non-supergiant early B-type stars, displaying pulsating behaviour which is not well understood. Stars tend to form in clusters where it can therefore be expected that young massive stars can be found in open clusters. For this reason two young southern open clusters were observed in order to search for B-type pulsating stars. The region of NGC 6204 and Hogg 22 was observed over a period of thirteen nights in Johnson B, V and I bands. NGC 6204 is believed to be the oldest cluster of the two at a distance of 0.8 kpc while the much younger Hogg 22 is more distant at 2.8 kpc. These two open clusters are located 6 arcminutes apart which made it possible to observe them simultaneously with a 12.8 12.8 arcminute eld of view. The observations were done with the newly installed 1600 telescope of the North-West University, South Africa. In order to do a variability search, periodic stars need to be identi ed from the cluster data, where a typical data set may contain thousands of scienti c images. In addition to the main motivation for this study, a pipeline was created in order to automate the photometry and data reduction processes. A Lomb-Scargle transform was applied to the stellar light curves in order to identify periodic sources. 354 signi cantly periodic stars were identi ed from the 3182 observed stars. Amongst them, two new possible Cephei stars were found together with a possible slowly pulsating B star (SPB), and numerous eclipsing binary systems. By using photometry of this region obtained by Forbes & Short (1996), instrumental magnitudes were transformed to a standard system in order to compare photometry results. From the constructed colour magnitude diagram of the two clusters, it could be seen that some stars, indicated by Forbes & Short (1996) to be cluster members, were in fact eld stars belonging to neither cluster. The reduction and photometry pipeline was implemented successfully on the data set, which also highlighted the importance of instrumentation and correct data analysis procedures. Possible improvements were identi ed in order to overcome di culties experienced during this study. / Thesis (MSc (Space Physics))--North-West University, Potchefstroom Campus, 2013

The theory of stellar evolution and stellar structure relies on the observation of stars in di erent phases of their evolutionary cycle. The relation between observations and theory can be strengthened by obtaining observational data of a large sample of stars in a particular evolutionary phase. The search for Cephei stars, as conducted in this study, can contribute to the sample of known Cephei stars, where these interesting stars are massive non-supergiant early B-type stars, displaying pulsating behaviour which is not well understood. Stars tend to form in clusters where it can therefore be expected that young massive stars can be found in open clusters. For this reason two young southern open clusters were observed in order to search for B-type pulsating stars. The region of NGC 6204 and Hogg 22 was observed over a period of thirteen nights in Johnson B, V and I bands. NGC 6204 is believed to be the oldest cluster of the two at a distance of 0.8 kpc while the much younger Hogg 22 is more distant at 2.8 kpc. These two open clusters are located 6 arcminutes apart which made it possible to observe them simultaneously with a 12.8 12.8 arcminute eld of view. The observations were done with the newly installed 1600 telescope of the North-West University, South Africa. In order to do a variability search, periodic stars need to be identi ed from the cluster data, where a typical data set may contain thousands of scienti c images. In addition to the main motivation for this study, a pipeline was created in order to automate the photometry and data reduction processes. A Lomb-Scargle transform was applied to the stellar light curves in order to identify periodic sources. 354 signi cantly periodic stars were identi ed from the 3182 observed stars. Amongst them, two new possible Cephei stars were found together with a possible slowly pulsating B star (SPB), and numerous eclipsing binary systems. By using photometry of this region obtained by Forbes & Short (1996), instrumental magnitudes were transformed to a standard system in order to compare photometry results. From the constructed colour magnitude diagram of the two clusters, it could be seen that some stars, indicated by Forbes & Short (1996) to be cluster members, were in fact eld stars belonging to neither cluster. The reduction and photometry pipeline was implemented successfully on the data set, which also highlighted the importance of instrumentation and correct data analysis procedures. Possible improvements were identi ed in order to overcome di culties experienced during this study. / Thesis (MSc (Space Physics))--North-West University, Potchefstroom Campus, 2013