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<dc:title xml:lang="en">Massive black holes in dwarf galaxies : off-center binary formation through gravitational capture</dc:title>
<dcterms:alternative xml:lang="fr">Trous noirs massifs dans les galaxies naines : formation de binaires excentrées par capture gravitationnelle</dcterms:alternative>
<dc:subject xml:lang="fr">Astrophysique</dc:subject>
<dc:subject xml:lang="fr">Dynamique galactique</dc:subject>
<dc:subject xml:lang="fr">Galaxies naines</dc:subject>
<dc:subject xml:lang="fr">Trous noirs</dc:subject>
<dc:subject xml:lang="fr">Gravitation</dc:subject>
<dc:subject xml:lang="fr">Simulations</dc:subject>
<dc:subject xml:lang="en">Astrophysics</dc:subject>
<dc:subject xml:lang="en">Galactic dynamics</dc:subject>
<dc:subject xml:lang="en">Dwarf galaxies</dc:subject>
<dc:subject xml:lang="en">Black holes</dc:subject>
<dc:subject xml:lang="en">Gravity</dc:subject>
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<dcterms:abstract xml:lang="fr">L’observation de trous noirs (TNs) supermassifs à haut redshift questionne notre compréhension de leur croissance. Le scénario standard de fusion des TNs massifs prévoit que ces derniers se retrouvent au centre galactique, amenés par la friction dynamique. Cependant, le temps nécessaire à un TN de masse intermédiaire pour atteindre le centre d’une galaxie naine typique est bien plus grand que l’âge de l’univers. De plus, les phénomènes de rétroaction peuvent abaisser la densité centrale de ces galaxies et créer un cœur, permettant le phénomène de core stalling, où les TNs restent sur des orbites stables excentrées. Ainsi, la question se pose : ces TNs peuvent-ils fusionner à l'extérieur du centre galactique ? Cette thèse explore d'abord la formation de cœurs de densité dans les galaxies naines et propose un nouveau scénario de fusion excentrée des TNs massifs, initiée par une capture gravitationnelle. Nous découvrons que les captures permettent la formation de binaires dans 13% des cas dans notre configuration idéalisée. Ce résultat justifie une analyse approfondie des processus dissipatifs pour stabiliser ces captures, en particulier à la lumière des futurs observatoires comme LISA, qui détecteront les ondes gravitationnelles issues de telles fusions.</dcterms:abstract>
<dcterms:abstract xml:lang="en">The observation of supermassive black holes (BHs) at high redshift challenges our understanding of their growth. The standard scenario of massive BH mergers relies on the fact that they settle at the galactic center due to dynamical friction. However, the time required for an intermediate-mass BH to reach the center of a typical dwarf galaxy far exceeds the age of the universe. Additionally, feedback processes can reduce the central density of these galaxies, creating a core and leading to core stalling, where BHs remain in stable, off-center orbits.This raises the question: can these BHs merge outside the galactic center ? This thesis first examines the formation of density cores in dwarf galaxies and proposes a new scenario for off-center mergers of massive BHs, initiated by gravitational capture. We find that in our idealized setup, captures result in the formation of binaries in 13% of cases. This finding underscores the need for a detailed analysis of dissipative processes to stabilize these captures, especially given the upcoming capabilities of observatories like LISA, which are expected to detect gravitational waves from such mergers.</dcterms:abstract>
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