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            <title xml:lang="en">Young binary systems and their nearby environment: high-angular resolution observations</title>
            <title xml:lang="fr">Les systemes binaires jeunes et leur environnement proche: observations a haute resolution angulaire</title>
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            <idno type="halRefHtml">Astrophysique [astro-ph]. Université Joseph-Fourier - Grenoble I, 2000. Français. &lt;a target="_blank" href="https://www.theses.fr/"&gt;&amp;#x27E8;NNT : &amp;#x27E9;&lt;/a&gt;</idno>
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            <idno type="stamp" n="UNIV-GRENOBLE1">Université Joseph Fourier - Grenoble I</idno>
            <idno type="stamp" n="UJF">Thèses de l'Université Joseph Fourier</idno>
            <idno type="stamp" n="OSUG">Observatoire des Sciences de la Terre, de l'Univers et de l'Environnement de Grenoble</idno>
            <idno type="stamp" n="LAOG">Laboratoire d'Astrophysique de Grenoble</idno>
            <idno type="stamp" n="UGA-EPE">Université Grenoble Alpes [2020-*]</idno>
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            <note type="commentary">President du jury: Guy Pelletier; Rapporteurs: Michel Mayor et Alfred Vidal-Madjar; Examinateurs: Karl Stapelfeldt et Hans Zinnecker</note>
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                <title xml:lang="en">Young binary systems and their nearby environment: high-angular resolution observations</title>
                <title xml:lang="fr">Les systemes binaires jeunes et leur environnement proche: observations a haute resolution angulaire</title>
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                <authority type="institution">Université Joseph-Fourier - Grenoble I</authority>
                <authority type="supervisor">Bouvier Jerome(jerome.bouvier@obs.ujf-grenoble.fr)</authority>
                <authority type="jury">Menard Francois (co-directeur)</authority>
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                <term xml:lang="en">Star formation</term>
                <term xml:lang="en">Monte carlo simulations</term>
                <term xml:lang="en">polarimetry</term>
                <term xml:lang="en">high angular resolution observations</term>
                <term xml:lang="en">accretion disk</term>
                <term xml:lang="en">binary systems</term>
                <term xml:lang="fr">Formation stellaire</term>
                <term xml:lang="fr">systemes binaires</term>
                <term xml:lang="fr">disque d'accretion</term>
                <term xml:lang="fr">observations a haute resolution angulaire</term>
                <term xml:lang="fr">polarimetrie</term>
                <term xml:lang="fr">simulations Monte Carlo</term>
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              <p>The work presented in this thesis focuses on some properties of pre-main sequence binary systems: their proportion among various populations, the frenquency and properties of dust and gaz discs in these systems, and the interaction of these discs with the two stellar components of the system. Several high-angular resolution imaging techniques are used to serve these purposes, as well as Monte-Carlo simulations. The binary frequency is determined in two two-million years-old stellar clusters. Then, a self-consistent comparison of these results with previously published surveys is performed. These data are compared to the predictions of formation and dynamical evolution models for stellar clusters, and are in agreement with the hypothesis that the star formation process leads to an ``initial'' binary fraction close to 100%, some systems being subsequently disrupted through the large number of encounters which occur within clusters. Optical spectroscopy of T Tauri binary systems reveals that both components of a system simultaneously possess circumstellar discs, suggesting that the environment of both stars do not evolve independently during the first million years. Direct images of two circumbinary discs and two circumstellar discs within binary systems were also obtained in the optical, the near-infrared, and the millimetric range. Coupling these observations with numerical simulations which describe photon multiple scattering allows us to estimate the geometrical characteristics of these discs, as well as the dust grain properties.</p>
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              <p>Le travail presente dans cette these a pour objet l'etude de certaines proprietes des systemes binaires pre-sequence principale: la proportion de ces systemes dans differentes populations, l'existence et les proprietes de disques de matiere en leur sein, et enfin l'interaction de ces disques avec les deux composantes stellaires du systeme. A ces fins, plusieurs techniques d'imagerie a haute resolution angulaire sont utilisees, ainsi que des simulations numeriques de type Monte-Carlo. La proportion de systemes binaires dans deux amas stellaires ages d'environ deux millions d'annees est determinee, puis une comparaison de ces resultats avec des etudes anterieures est presentee. L'ensemble de ces donnees est compare aux modeles de formation et d'evolution dynamique des amas d'etoiles, et semblent en accord avec l'hypothese selon laquelle le processus de formation aboutit a un proportion ``initiale'' de binaires proche de 100%, avant que les nombreuses interactions dans les amas ne detruisent une partie de ces systemes. La spectroscopie de systemes binaires T Tauri revele que les deux composantes d'un meme systeme possedent simultanement des disques circumstellaires, ce qui suggere que les environnements des deux composantes n'evoluent pas independamment durant le premier million d'annees. Des images directes de deux disques circumbinaires et deux disques circumstellaires au sein de systemes binaires ont egalement ete obtenues dans le visible, le proche infrarouge et le domaine millimetrique. En couplant ces resultats a l'utilisation d'un code numerique decrivant la diffusion multiple des photons, il est possible d'estimer les proprietes geometriques des disques, ainsi que celles des grains de poussiere qui y sont presents.</p>
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