Orbital structure of triaxial galaxies
نویسندگان
چکیده
منابع مشابه
Orbital Structure of Triaxial Black - Hole Nuclei
Orbital motion in triaxial nuclei with central point masses, representing supermassive black holes, is investigated. The stellar density is assumed to follow a power law, ρ ∝ r −γ , with γ = 1 or γ = 2. At low energies the motion is essentially regular; the major families of orbits are the tubes and the pyramids. Pyramid orbits are similar to box orbits but have their major elongation parallel ...
متن کامل0 Orbital Structure of Triaxial Black - Hole Nuclei
Orbital motion in triaxial nuclei with central point masses, representing supermassive black holes, is investigated. The stellar density is assumed to follow a power law, ρ ∝ r −γ , with γ = 1 or γ = 2. At low energies the motion is essentially regular; the major families of orbits are the tubes and the pyramids. Pyramid orbits are similar to box orbits but have their major elongation parallel ...
متن کاملTriaxial Galaxies with Cusps
We have constructed fully self-consistent models of triaxial galaxies with central density cusps. The triaxial generalizations of Dehnen's (1993) spherical mass models are presented, which have densities that vary as r −γ near the center and r −4 at large radii. We computed libraries of ∼ 7000 orbits in each of two triaxial models with γ = 1 (" weak cusp ") and γ = 2 (" strong cusp "); these tw...
متن کاملResonant Orbits in Triaxial Galaxies
Box orbits in triaxial potentials are generically thin, that is, they lie close in phase space to a resonant orbit satisfying a relation of the form lω1 +mω2 + nω3 = 0 between the three fundamental frequencies. Boxlets are special cases of resonant orbits in which one of the integers (l,m, n) is zero. Resonant orbits are confined for all time to a membrane in configuration space; they play roug...
متن کاملOrbital Instabilities in a Triaxial Cusp Potential
This paper constructs an analytic form for a triaxial potential that describes the dynamics of a wide variety of astrophysical systems, including the inner portions of dark matter halos, the central regions of galactic bulges, and young embedded star clusters. Specifically, this potential results from a density profile of the form ρ(m) ∝ m−1, where the radial coordinate is generalized to triaxi...
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ژورنال
عنوان ژورنال: Symposium - International Astronomical Union
سال: 2004
ISSN: 0074-1809
DOI: 10.1017/s0074180900183159