scholarly journals Models of cuspy triaxial stellar systems – III. The effect of velocity anisotropy on chaoticity

2014 ◽  
Vol 438 (4) ◽  
pp. 2871-2881 ◽  
Author(s):  
D. D. Carpintero ◽  
J. C. Muzzio ◽  
H. D. Navone
2012 ◽  
Vol 428 (4) ◽  
pp. 2995-3000 ◽  
Author(s):  
J. C. Muzzio ◽  
H. D. Navone ◽  
A. F. Zorzi

1993 ◽  
Vol 153 ◽  
pp. 407-408
Author(s):  
Richard Arnold ◽  
Tim De Zeeuw ◽  
Chris Hunter

Analytic dynamic models of triaxial stellar systems, such as elliptical galaxies and galactic bulges, can be used to calculate the velocity fields of systems in a wide range of potentials without the need for orbit integrations. We present results from a first application of these models, in the form of velocity fields projected onto the sky. The appearance of the velocity field depends strongly on the viewing angle. Thin orbit models provide a theoretical upper limit to streaming in all possible kinematic models in a given potential.


1985 ◽  
Vol 113 ◽  
pp. 301-303
Author(s):  
E. Bettwieser ◽  
K. J. Fricke ◽  
R. Spurzem

Spherical stellar systems show during their secular evolution the development of velocity anisotropy in their halo (cf. e.g. Hénon, 1971). The present study examines the general reasons for generation of anisotropy in stellar systems by means of a gaseous star cluster model including anisotropy. Moment equations of the Boltzmann equation are considered for spherical symmetry in coordinate space but not in velocity space closed in third order by a heat flux equation. The coefficient of heat conductivity is tailored to describe the flux of energy due to the cumulative effect of distant gravitative encounters and generalized to include effects of anisotropy and external gravitation by a massive central object (Bettwieser et al., 1984).


1993 ◽  
Vol 153 ◽  
pp. 273-274
Author(s):  
D. Friedli ◽  
S. Udry

Depending on the nature of the various components (stars, gas) present in triaxial stellar systems (elliptical galaxies, bulges and bars), the dynamics is expected to be rather different. The stars are collisionless, dissipationless, and dynamically hot; they are mainly trapped by quasi-periodic or chaotic orbits. On the contrary, the gas is collisional, dissipational, and dynamically cold; the cold or warm gas (≲ 104 K) is a powerful orbital tracer, however shocks prevent it from following self-crossing orbits. The hot gas (≲ 106 K) is influenced by “repulsive” pressure forces which prevent in close encounters the flow from being strongly shocked; it rather follows chaotic trajectories. By means of fully self-consistent 3D simulations with stars and gas using PM (Pfenniger & Friedli 1992) and SPH (Friedli & Benz 1992) techniques, we investigate the response of gaseous components in the following situations: 1) slow or fast pattern speed Ωp, 2) direct or retrograde gas motion with respect to the stars, and 3) warm or hot gas temperature T. Initial parameters and final characteristics of each runs are reported in Table I.


1993 ◽  
pp. 407-408
Author(s):  
Richard Arnold ◽  
Tim de Zeeuw ◽  
Chris Hunter

2007 ◽  
Vol 99 (4) ◽  
pp. 307-324 ◽  
Author(s):  
Roberto O. Aquilano ◽  
Juan C. Muzzio ◽  
Hugo D. Navone ◽  
Alejandra F. Zorzi

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