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Paolo Bianchini (Observatoire astronomique de Strasbourg, CNRS)20/08/2024, 14:00Numerical approaches to modelling stellar systems and their constituentsTalk
The majority of Milky Way globular clusters (GCs) display a small, yet significant, amount of angular momentum, clearly detectable from line-of-sight and proper motion data sets. The origin of this angular momentum is still unknown, but its emergence may be linked to the primordial formation of GCs in the high-redshift universe.
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In this talk, I will present 2 sets of direct N-body simulations... -
Long Wang (Sun Yat-sen University)20/08/2024, 14:20Numerical approaches to modelling stellar systems and their constituentsTalk
Massive stars have a significant impact on the dynamical evolution of star clusters. They play a crucial role during star formation, as their radiation can push surrounding gas away and inhibit further star formation. Additionally, strong mass loss from massive stars via strong winds can rapidly reduce the gravitational potential of star clusters and trigger their fast expansion. Once these...
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Nathan Leigh (Universidad de Concepcion)20/08/2024, 14:40Numerical approaches to modelling stellar systems and their constituentsTalk
Each outcome of the four-body problem can be regarded as some variation of the three-body problem. For example, when two single stars are produced (the 2 + 1 + 1 outcome), each ejection event is modeled as its own three-body interaction by assuming that the ejections are well separated in time. For each outcome, we derive, using the density-of-states formalism, analytical distribution...
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Alessandro A. Trani (Niels Bohr Institute)20/08/2024, 15:00Numerical approaches to modelling stellar systems and their constituentsTalk
The 3-body problem poses a longstanding challenge in physics and celestial mechanics. Despite the impossibility of obtaining general analytical solutions, statistical theories have been developed based on the ergodic principle. This assumption is justified by chaos, which is expected to fully mix the accessible phase space of the 3-body problem.
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We probed the presence of regular (i.e. non... -
Vaclav Pavlik (Astronomical Institute of the Czech Academy of Sciences, Prague, Czech Republic)20/08/2024, 15:20Numerical approaches to modelling stellar systems and their constituentsTalk
Recent observations with HST and Gaia deepened our understanding of the internal kinematics of star clusters. Motivated by those findings, we aim to gain theoretical insights into how various kinematic properties influence the overall dynamical development of these stellar systems. Through N-body simulations, we explore the effects of different initial velocity distributions, ranging from...
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Steven Rieder (KU Leuven)20/08/2024, 16:05Numerical approaches to modelling stellar systems and their constituentsTalk
AMUSE, the Astrophysical Multipurpose Software Environment, has been around since 2009, and it has been used in many different projects. AMUSE offers users the ability to combine different specialised simulation codes in a single simulation, which makes it possible to simulate complex systems that require interaction between different physical aspects and/or scales. Topics AMUSE has been used...
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Francisco I. Aros (Indiana University)20/08/2024, 16:25Numerical approaches to modelling stellar systems and their constituentsTalk
Globular clusters (GCs) have multiple populations identified through abundance variations in a number of light elements. These populations also show, in some cases, differences in some dynamical properties such as their concentration, systemic rotation, and velocity anisotropy, differences that might still preserve partial memory of the initial configuration of the stellar populations. In this...
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Aleksey Generozov (Technion Israel Institute of Technology)20/08/2024, 16:45Numerical approaches to modelling stellar systems and their constituentsTalk
I will discuss how gas affects the evolution of multiple star systems in young star clusters and other gas-rich environments. In particular, gas can shrink and circularize wide binaries, potentially explaining observed changes in binary properties with star cluster age. Additionally, gas can trigger instabilities in multiple systems. Finally, gas may trigger the formation of binaries and...
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Francesco Maria Flammini Dotti (University of Heidelberg)20/08/2024, 17:05Talk
The dynamical evolution of planet-like objects in star clusters is not easy observable in star clusters, and it still not possible in dense star clusters such as globular clusters. I will first introduce previous works that looked into the motion of these objects, and then I will numerically explore the dynamical evolution of such objects, varying the number density of the hosting star...
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Poojan Agrawal (University of North Carolina at Chapel Hill)21/08/2024, 11:20Numerical approaches to modelling stellar systems and their constituentsTalk
Stripped stars, also known as naked helium stars, are the helium cores of stars that have lost their hydrogen-rich outer layer. The recent discoveries of stripped stars have provided valuable insights into massive star evolution, as well as the evolution of stellar binaries. In my talk, I will present results from the rapid stellar evolution code METISSE, used within the binary population...
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Francesco Gabrielli (SISSA)21/08/2024, 11:40Numerical approaches to modelling stellar systems and their constituentsTalk
Pair-instability supernovae (PISNe) are explosions developing in the core of massive stars due to a thermonuclear, runaway process, ultimately leading to the total disruption of the progenitor.
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They are expected to be the endpoint of the evolution of low-metallicity stars in the mass range between ~ 140 and 260 solar masses, and responsible for the existence of the upper mass gap in the black... -
Amedeo Romagnolo21/08/2024, 12:00Numerical approaches to modelling stellar systems and their constituentsTalk
Canonical stellar evolution models from both population synthesis and detailed evolutionary codes may predict Very Massive Stars (VMS, defined as $M_{\rm ZAMS}$ > 100 M$_\odot$) to become red supergiants and expand sometimes even more than 10,000 R$_\odot$. At those masses we now know that the luminosity levels are high enough for stellar envelopes to eject mass through winds at...
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