Dynamical Evolution of Dense Stellar Systems (IAU S246)
Dynamical Evolution of Dense Stellar Systems (IAU S246)

Author: International Astronomical Union. Symposium

Publisher: Cambridge University Press

Published: 2008-06-12

Total Pages: 516

ISBN-13: 9780521874687

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Dense stellar systems lie at the interface between dynamics, stellar evolution, and galaxy formation, and they provide us with an ideal laboratory to understand many different aspects of these important fields as well as to explore the interplay between them. The complete study of dense stellar systems is a very challenging task which requires the collaboration and the exchange of ideas of astronomers and physicists with observational and theoretical expertise in galactic and extra-galactic astronomy, stellar dynamics, hydrodynamics, stellar evolution, as well as knowledge of many aspects of computational physics. IAU Symposium 246 brought together experts in all these areas to cover the broad field of dense stellar systems with particular emphasis on the interplay between them and on the comparison between observations and simulations. This volume provides a complete review of the most recent studies in this topical research.

Globular Clusters
Globular Clusters

Author: C. Martinez Roger

Publisher: Cambridge University Press

Published: 1999-10-28

Total Pages: 380

ISBN-13: 9780521770583

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An accessible introduction to globular clusters for graduate students, and a comprehensive and up-to-date reference for researchers.

Mass Loss from Stars and the Evolution of Stellar Clusters
Mass Loss from Stars and the Evolution of Stellar Clusters

Author: Alex de Koter

Publisher:

Published: 2008

Total Pages: 512

ISBN-13:

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"In the spring of 2006 a four day international workshop was held in Lunteren, The Netherlands, in honor of the formal retirement of Prof. Henny Lamers. These proceedings provide a comprehensive overview of mass loss in massive stars and of the dynamical fate of clusters. The dynamical evolution of clusters is affected by stellar winds, mass loss outbursts and supernova explosions as well as by the loss of stars in dynamical interactions, thus linking the two central themes of the workshop. It is becoming clear that mass loss by radiation pressure on spectral lines is not only at work in normal O, B, and A stars but also in Luminous Blue Variables and Wolf-Rayet stars. The importance of these line-driven winds relative to outbursts in the Luminous Blue Variable phase of evolution is under debate. A central issue in this discussion is the importance of small and possibly large scale structure in stellar winds and its implications for the measured mass loss rates. These proceedings report on progress establishing wind properties, on theoretical predictions of mass loss and wind structure as a function of stellar properties, and on the effects of mass loss on the evolution of massive stars. As a result of dynamical interactions, clusters may dissolve completely over time. Observational studies of cluster dissolution timescales as a function of cluster formation history and cluster and environmental properties, are at the focus of cluster studies in the last decade. A key topic discussed in this book is whether the old globular clusters we observe today were once similar to present-day massive young clusters. The mass function of the two types of clusters is observed to be different. Is this a result of dynamical evoltuion or were the mass functions different at formation? The 12 invited reviews, 18 contributed talks, 48 poster papers, and two discussion sessions combine to provide and in-depth assessment of both observational and theoretical issues. The book is suitable for researchers and graduate students interested in stellar astrophysics and cluster dynamics."--Provided by publisher.

Dynamical Evolution of Globular Clusters
Dynamical Evolution of Globular Clusters

Author: Lyman Spitzer, Jr.

Publisher: Princeton University Press

Published: 2014-07-14

Total Pages: 192

ISBN-13: 1400858739

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One of the world's most distinguished astrophysicists presents a comprehensive theoretical treatment of the dynamical evolution of globular clusters. Lyman Spitzer's research in this field established the framework for decades of investigation. Now he summarizes in a unified, systematic way this branch of theoretical astrophysics with its still challenging problems. Originally published in 1988. The Princeton Legacy Library uses the latest print-on-demand technology to again make available previously out-of-print books from the distinguished backlist of Princeton University Press. These editions preserve the original texts of these important books while presenting them in durable paperback and hardcover editions. The goal of the Princeton Legacy Library is to vastly increase access to the rich scholarly heritage found in the thousands of books published by Princeton University Press since its founding in 1905.

The Role of Black Hole and Neutron Star Interaction on the Dynamical Evolution of Dense Stellar Systems
The Role of Black Hole and Neutron Star Interaction on the Dynamical Evolution of Dense Stellar Systems

Author: Michael Anton Pajkos

Publisher:

Published: 2017

Total Pages: 58

ISBN-13:

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"With the recent detection of gravitational waves from the Laser Interferometer Gravitational-Wave Observatory, or LIGO, a new realm of gravitational astrophysics has been opened. As the process of observing gravitational wave signals is still in its infancy, there is a need to provide gravitational astronomers with observable signatures in the electromagnetic spectrum. Hence, we explore the impact of solar mass black holes on the morphology of globular clusters. It has long been thought that due to high kick velocities from compact object gravitational interaction, Galactic age Globular Clusters are unable to retain black holes. Recent simulations, however, suggest that a significant population of black holes can be retained (Sippel & Hurley 2012, Rodriguez et al. 2016). We present the results from Fokker-Planck simulations of a time evolving Globular Cluster with an initial mass of 2.5x106 M☉. By exploring two different methods of IMF construction--evolved mass function and pure power-law--we are able to consistently determine their radial, density profiles with the introduction of 12 M☉ black holes. Because of the efficiency of the Fokker-Planck code, we are able to explore parameter space as we observe how the globular cluster changes over initial mass functions with 0.1%, 1%, and 10% black holes retention rates--from initial black hole formation--and discover a significant impact on the cluster morphology between once the black hole population is on the order of 100. Moreover, we observe the segregation of black holes from the rest of the stellar members of the cluster and the influence of 3 body binary heating on the core of the segregated black hole sub-cluster. As we only address the initial ejection of black holes, and not their escape from the cluster over time, our future work will account for 3 body binary kicks that cause them to escape"--Page 1.