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Titlebook: Stability of Collisionless Stellar Systems; Mechanisms for the D P. L. Palmer Book 1994 Springer Science+Business Media Dordrecht 1994 Cosm

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書目名稱Stability of Collisionless Stellar Systems
副標(biāo)題Mechanisms for the D
編輯P. L. Palmer
視頻videohttp://file.papertrans.cn/876/875328/875328.mp4
叢書名稱Astrophysics and Space Science Library
圖書封面Titlebook: Stability of Collisionless Stellar Systems; Mechanisms for the D P. L. Palmer Book 1994 Springer Science+Business Media Dordrecht 1994 Cosm
描述Recent advances in our understanding of instabilities ingalactic type systems have led to an unravelling of some of themysteries of what determines the form galaxies take. This book focuseson the mathematical development of the subject, assuming no priorknowledge of it, with a strong emphasis on the underlying physicalinterpretation. This framework is used to discuss the most relevantinstabilities which are believed to be closely involved in the waygalaxies are formed, in a model independent manner. The relevantobserved properties of galaxies that may be used to establish the roleof these physical mechanisms are discussed. .The book also includes a chapter discussing numerical simulationtechniques, with attention paid to their limitations and to recentadvances in this approach. It is demonstrated that recent developmentsin computer hardware enable a detailed comparison of simulations withanalysis. Thus the simulations extend our physical understandingbeyond the limitations of the analysis. .The book is intended for use by postgraduate students and researchersin the areas of cosmology, extragalactic astronomy and dynamics. .
出版日期Book 1994
關(guān)鍵詞Cosmology; Galaxy; astronomy; simulation; stellar
版次1
doihttps://doi.org/10.1007/978-94-017-3059-4
isbn_softcover978-90-481-4315-3
isbn_ebook978-94-017-3059-4Series ISSN 0067-0057 Series E-ISSN 2214-7985
issn_series 0067-0057
copyrightSpringer Science+Business Media Dordrecht 1994
The information of publication is updating

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https://doi.org/10.1007/978-94-017-3059-4Cosmology; Galaxy; astronomy; simulation; stellar
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General Perturbation Theory,ual stars and thus we cannot infer anything about collective instability in the system, which requires a self-consistent build up of the combination of the perturbations to all the orbits of the stars in the system. A good account of the use of action and angle variables in perturbation theory can be found in [30].
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Description of the Orbital Motions,dels with at least one axis of symmetry. The results derived in this chapter will provide the groundwork for the next chapter where we shall consider the effects of perturbing the equilibrium potential that governs the motions of the stars.
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