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Tabone, Benoît. "L'origine des jets protostellaires à l'ère d'ALMA : de la modélisation aux observations". Thesis, Paris Sciences et Lettres (ComUE), 2018. http://www.theses.fr/2018PSLEO024/document.
Pełny tekst źródłaThe question of angular momentum extraction from protoplanetary disks (hereafter PPDs) is fundamental in understanding the accretion process in young stars and the formation conditions of planets. Pioneering semi-analytical work, followed by a growing body of magnetohydrodynamic (MHD) simulations, have shown that when a significant vertical magnetic field is present, MHD disk winds (hereafter MHD-DWs) can develop and ex- tract some or all of the angular momentum flux required for accretion. The aim of this PhD thesis is to exploit the unprecedented capabilities provided by ALMA to clarify the accretion-ejection process in protostars. This goal is achieved following three approaches: 1) comparison of MHD-DW models with the kinematics of HH 212 jet observed by ALMA at high angular resolution. I report the discovery of a rotating SO/SO2 wind consistent with a MHD-DWs launched out to ∼40 au with SiO tracing dust-free streamlines launched from 0.05−0.3 au. 2) Analytical and numerical study of the interaction between a pulsat- ing inner jet embedded in a stationary disk wind. Observational signatures are identified from the morphology and the kinematics of bow-shock shells. 3) Chemical signatures of a jet launched inside the dust sublimation radius (∼ 0.2 au). I show that despite the strong X-FUV field and the absence of dust, molecules like SiO or CO can form efficiently from a small fraction of H2. This scenario will be confronted to JWST observations
Verliat, Antoine. "Origine du moment cinétique et influence des jets protostellaires sur la formation d'étoiles". Electronic Thesis or Diss., université Paris-Saclay, 2021. http://www.theses.fr/2021UPASP058.
Pełny tekst źródłaThe interstellar medium is the cradle of stars. It is a fantastic playground for physicists due to its richness and the complexity of the phenomena involved. Understanding the details of star formation is one of the great challenges of modern astrophysics.The complexity of the problems studied in this thesis makes numerical simulations a valuable tool. It has allowed me to study two fundamental aspects of star formation. The first part of my work is devoted to understanding the origin of the rotation of the disks made of gas and dust that surround young stars and in which planets form. The second is the study of the formation of star clusters. While it is known that stars form in clusters, the processes that influence the formation of these clusters and their structure are poorly understood. The study will focus particularly on the influence of jets of matter emitted by young stars on these clusters
Rabenanahary, Mialy Rabetanety. "Flots protostellaires poussés par un jet dans une enveloppe stratifiée : revisiter un modèle à l'ère d'ALMA". Electronic Thesis or Diss., Université Paris sciences et lettres, 2022. http://www.theses.fr/2022UPSLO014.
Pełny tekst źródłaA long-standing open question in star formation is the process responsible for its low efficiency on parsec scales (a few %), and for shifting down the Initial Mass Function (IMF) to only ∼30% of the prestellar core mass distribution. The most recent numerical simulations show that neither turbulence nor magnetic fields can, alone, reproduce these low efficiencies, and that feedback by protostellar outflows must play a crucial role by disrupting accretion streams, expelling material from cores, and/or sustaining turbulence. Unfortunately, the magnitude of outflow feedback (affected cloud volume, injected momentum, entrained mass, impact on the disk and infalling envelope) depends strongly on the underlying protostellar wind geometry, which remains uncertain and heavily debated: a fast wide-angle "X-wind”, a slower MHD disk wind, a narrow jet ? Clearly, if we want to reliably assess the role of outflow feedback in star formation, it is of utmost importance to determine which wind geometry is the most realistic (and/or which one can be excluded). As a new contribution towards this goal, we present, for the first time, numerical predictions for outflows driven by a narrow pulsed jet in a stratified prestellar core. We compare our simulations against recent ALMA observations and analogous predictions for a wide-angle X-wind. Our simulations are the first to combine jet variability, ambient density-stratification, and long timescales up to 10 000 yrs (typical of young outflows) on scales up to 0.1 pc. We find that the predicted widths, position-velocity diagrams, and mass-velocity distribution, show striking resemblance with ALMA observations of CO outflows such as HH46/47 and CARMA-7, and in closer agreement than models based on a wide-angle "X-wind". The results obtained in this work could have major implications for the feedback of protostellar outflows on star formation
Cabrit, Sylvie. "Ejection de matiere dans les objets protostellaires et les etoiles jeunes de faible masse". Paris 6, 1989. http://www.theses.fr/1989PA066082.
Pełny tekst źródłaCabrit, Sylvie. "Ejection de matière dans les objets protostellaires et les étoiles jeunes de faible masse". Phd thesis, Université Pierre et Marie Curie - Paris VI, 1989. http://tel.archives-ouvertes.fr/tel-00725199.
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