Generalized isochrone models for spherical stellar systems

Non - Spherical Stellar Models of Compact Stars

Stability of rotating spherical stellar systems

We study the stability of rotating collisionless self-gravitating spherical systems by using high resolution N-body experiments on a Connection Machine CM-5. We added rotation to Ossipkov-Merritt (hereafter OM) anisotropic spherical systems by using two methods. The first method conserves the anisotropy of the distribution function defined in the OM algorithm. The second method distorts the sys...

Cusped Spherical Stellar Systems with Anisotropic Velocities

Spherical models with constant velocity anisotropy β have distribution functions depending on binding energy E and angular momentum L of the form f (E, L) = L−2β fE(E). An inversion for the unknown function fE (E) is straightforward to derive and reduces to Eddington’s famous algorithm for isotropic models (β = 0). Importantly, if the anisotropy parameter of the model is a half-integer constant...

NSF-ITP-93-122 A family of models for spherical stellar systems

We describe a one-parameter family of models of stable spherical stellar systems in which the phase-space distribution function depends only on energy. The models have similar density pro les in their outer parts ( / r 4 ) and central power-law density cusps, / r 3 , 0 < 3. The family contains the Ja e (1983) and Hernquist (1990) models as special cases. We evaluate the surface brightness pro l...

Hypervirial Models of Stellar Systems

A family of cusped potential-density pairs is presented for modelling galaxies and dark haloes. The density profile is cusped like ρ ∼ rp−2 at small radii. The distribution function is simple and takes the form f ∝ Lp−2E(3p+1)/2 (where E is the binding energy and L is the angular momentum). The models all possess the remarkable property that the virial theorem holds locally, from which they ear...