Treffer: Dissipationless collapse of a set of N massive particles
Title:
Dissipationless collapse of a set of N massive particles
Authors:
Source:
Monthly Notices of the Royal Astronomical Society. 348(1):62-72
Publisher Information:
Oxford: Blackwell Science, 2004.
Publication Year:
2004
Physical Description:
print, 32 ref
Original Material:
INIST-CNRS
Subject Terms:
Astronomy earth cosmic environment, Astronomie et environnement cosmique terrestre, Sciences exactes et technologie, Exact sciences and technology, Terre, ocean, espace, Earth, ocean, space, Astronomie, Astronomy, Astronomie fondamentale et astrophysique. Instrumentation, techniques, et observations astronomiques, Fundamental astronomy and astrophysics. Instrumentation, techniques, and astronomical observations, Techniques d'observation et de réduction des données. Simulation et modélisation par ordinateur, Observation and data reduction techniques. Computer modeling and simulation, Méthodes mathématiques et méthodes de simulation sur ordinateur, Mathematical procedures and computer techniques, Systèmes stellaires. Objets et systèmes galactiques et extragalactiques. L'univers, Stellar systems. Galactic and extragalactic objects and systems. The universe, Caractéristiques et propriétés des galaxies externes et des objets extragalactiques, Characteristics and properties of external galaxies and extragalactic objects, Origine, formation, évolution, âge et formation stellaire, Origin, formation, evolution, age, and star formation, Amas globulaire, Globular clusters, Formation galaxies, Galaxy formation, Galaxies elliptiques, Elliptical galaxies, Méthode numérique, Numerical method, Método numérico, Particule massive, Massive particle, Partícula masiva, Simulation numérique, Digital simulation, Système autogravitant, Self-gravitating systems, Système n corps, N body system, Sistema n cuerpos, Trou noir, Black holes, galaxies: formation, globular clusters: general, methods: N-body simulations, methods: numerical
Document Type:
Fachzeitschrift
Article
File Description:
text
Language:
English
Author Affiliations:
École Nationale Supérieure de Techniques Avancées, Unité de Mathématiques Appliquées, 32 Bd Victor, 75015 Paris, France
Laboratoire de l'Univers et de ses THéories, Observatoire de Paris-Meudon, 5 place Jules Janssen, 92350 Meudon, France
Laboratoire de l'Univers et de ses THéories, Observatoire de Paris-Meudon, 5 place Jules Janssen, 92350 Meudon, France
ISSN:
0035-8711
Rights:
Copyright 2004 INIST-CNRS
CC BY 4.0
Sauf mention contraire ci-dessus, le contenu de cette notice bibliographique peut être utilisé dans le cadre d’une licence CC BY 4.0 Inist-CNRS / Unless otherwise stated above, the content of this bibliographic record may be used under a CC BY 4.0 licence by Inist-CNRS / A menos que se haya señalado antes, el contenido de este registro bibliográfico puede ser utilizado al amparo de una licencia CC BY 4.0 Inist-CNRS
CC BY 4.0
Sauf mention contraire ci-dessus, le contenu de cette notice bibliographique peut être utilisé dans le cadre d’une licence CC BY 4.0 Inist-CNRS / Unless otherwise stated above, the content of this bibliographic record may be used under a CC BY 4.0 licence by Inist-CNRS / A menos que se haya señalado antes, el contenido de este registro bibliográfico puede ser utilizado al amparo de una licencia CC BY 4.0 Inist-CNRS
Notes:
Astronomy
Accession Number:
edscal.15514281
Database:
PASCAL Archive
Weitere Informationen
The formation of self-gravitating systems is studied by simulating the collapse of a set of N particles which are generated from several distribution functions. We first establish that the results of such simulations depend on N for small values of N. We complete a previous work by Aguilar & Merritt concerning the morphological segregation between spherical and elliptical equilibria. We find and interpret two new segregations: one concerns the equilibrium core size and the other the equilibrium temperature. All these features are used to explain some of the global properties of self-gravitating objects: origin of globular clusters and central black hole or shape of elliptical galaxies.