Models of cuspy triaxial stellar systems – IV. Rotating systems

We built two self-consistent models of triaxial, cuspy, rotating stellar systems adding rotation to non-rotating models presented in previous papers of this series. The final angular velocity of the material is not constant and varies with the distance to the centre and with the height over the equa...

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Detalles Bibliográficos
Autores principales: Carpintero, Daniel Diego, Muzzio, Juan Carlos
Formato: Articulo
Lenguaje:Inglés
Publicado: 2016
Materias:
Ciencias Astronómicas
methods: numerical
galaxies: elliptical and lenticular, cD
galaxies: kinematics and dynamics
Acceso en línea:http://sedici.unlp.edu.ar/handle/10915/123896
Aporte de:
SEDICI (UNLP) de Universidad Nacional de La Plata
id I19-R120-10915-123896
record_format dspace
institution Universidad Nacional de La Plata
institution_str I-19
repository_str R-120
collection SEDICI (UNLP)
language Inglés
topic Ciencias Astronómicas
methods: numerical
galaxies: elliptical and lenticular, cD
galaxies: kinematics and dynamics
spellingShingle Ciencias Astronómicas
methods: numerical
galaxies: elliptical and lenticular, cD
galaxies: kinematics and dynamics
Carpintero, Daniel Diego
Muzzio, Juan Carlos
Models of cuspy triaxial stellar systems – IV. Rotating systems
topic_facet Ciencias Astronómicas
methods: numerical
galaxies: elliptical and lenticular, cD
galaxies: kinematics and dynamics
description We built two self-consistent models of triaxial, cuspy, rotating stellar systems adding rotation to non-rotating models presented in previous papers of this series. The final angular velocity of the material is not constant and varies with the distance to the centre and with the height over the equator of the systems, but the figure rotation is very uniform in both cases. Even though the addition of rotation to the models modifies their original semi-axes ratios, the final rotating models are considerably flattened and triaxial. An analysis of the orbital content of the models shows that about two-thirds of their orbits are chaotic yet the models are very stable over intervals of the order of one Hubble time. The bulk of regular orbits are short-axis tubes, while long-axis tubes are replaced by tubes whose axes lie on the short-long axes plane, but do not coincide with the major axis. Other types of regular orbits that do not appear in non-rotating systems, like horseshoes and orbits that cross themselves, are also found in the present models. Finally, our frequency maps show empty regions where studies of orbits on fixed potentials found orbits, a likely consequence of the self-consistency of our models that excludes them.
format Articulo
Articulo
author Carpintero, Daniel Diego
Muzzio, Juan Carlos
author_facet Carpintero, Daniel Diego
Muzzio, Juan Carlos
author_sort Carpintero, Daniel Diego
title Models of cuspy triaxial stellar systems – IV. Rotating systems
title_short Models of cuspy triaxial stellar systems – IV. Rotating systems
title_full Models of cuspy triaxial stellar systems – IV. Rotating systems
title_fullStr Models of cuspy triaxial stellar systems – IV. Rotating systems
title_full_unstemmed Models of cuspy triaxial stellar systems – IV. Rotating systems
title_sort models of cuspy triaxial stellar systems – iv. rotating systems
publishDate 2016
url http://sedici.unlp.edu.ar/handle/10915/123896
work_keys_str_mv AT carpinterodanieldiego modelsofcuspytriaxialstellarsystemsivrotatingsystems
AT muzziojuancarlos modelsofcuspytriaxialstellarsystemsivrotatingsystems
bdutipo_str Repositorios
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