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Michie-King anisotropic model

San Diego State University

The isotropic King model is the workhorse truncated globular-cluster model, but real clusters show radial velocity anisotropy in their outskirts. The Michie-King model adds Michie’s (1963) angular-momentum term to King’s (1966) lowered-Maxwellian cutoff, giving a one-parameter family (the anisotropy radius rar_a) of self-consistent, tidally truncated, radially anisotropic models.

The distribution function

f(E,J)exp ⁣(J22ra2σ2)[exp ⁣(Eσ2)1],E0,f(E, J) \propto \exp\!\left(-\frac{J^2}{2 r_a^2 \sigma^2}\right) \left[\exp\!\left(-\frac{E}{\sigma^2}\right) - 1\right],\qquad E \le 0,

↗ model card

with E=12v2+ΦE=\tfrac12 v^2 + \Phi, J=rvtJ = r v_t. The Gaussian exp(J2/2ra2σ2)\exp(-J^2/2r_a^2\sigma^2) depopulates high-angular-momentum (tangential) orbits — increasingly so at large rr (since J2r2J^2\propto r^2) — so the velocity ellipsoid is isotropic at the centre and becomes radial outward:

β(r)1σt2σr2:β(0)0,β outward,raβ0 (King).\beta(r) \equiv 1 - \frac{\sigma_t^2}{\sigma_r^2}:\quad \beta(0)\approx 0,\quad \beta \nearrow \text{ outward},\qquad r_a\to\infty \Rightarrow \beta\equiv 0 \text{ (King)}.

Here σt2\sigma_t^2 is a single tangential component (the convention used throughout progenax). Binney & Tremaine write β=1σt2/(2σr2)\beta = 1 - \sigma_t^2/(2\sigma_r^2) with σt2σθ2+σϕ2\sigma_t^2 \equiv \sigma_\theta^2 + \sigma_\phi^2 the two-component tangential dispersion; the factor of 2 cancels, so both give the same β(r)\beta(r) (see the Merritt 1985 note).

Unlike the Osipkov-Merritt construction (which holds a given density fixed and inverts for ff), Michie specifies ff and re-solves Poisson, so the density itself changes — hence β(r)\beta(r) is the DF-implied profile, not the OM form r2/(r2+ra2)r^2/(r^2+r_a^2).

Self-consistency

The density is the velocity integral of (1), which depends on radius explicitly through the anisotropy term, giving a radius-dependent King ODE — the King-1966 nondimensionalization of Michie (1963) Eq. 5.8, whose anisotropy weight eCz2η2(1μ2)e^{-Cz^2\eta^2(1-\mu^2)} is our eJ2/2ra2σ2e^{-J^2/2r_a^2\sigma^2} (ξ=r/rc\xi=r/r_c, r^a=ra/rc\hat r_a = r_a/r_c):

1ξ2ddξ ⁣(ξ2dψdξ)=9ρ^(ψ, ξ/r^a)ρ^(W0,0),ψ(0)=W0, ψ(0)=0.\frac{1}{\xi^2}\frac{d}{d\xi}\!\left(\xi^2\frac{d\psi}{d\xi}\right) = -9\,\frac{\hat\rho(\psi,\ \xi/\hat r_a)}{\hat\rho(W_0,0)}, \qquad \psi(0)=W_0,\ \psi'(0)=0.

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progenax solves this with diffrax (differentiable), the velocity scale fixed self-consistently as σ2=GM/(9rcμ)\sigma^2 = GM/(9 r_c \mu) — so the ICs are virial (Q0.5Q\approx0.5) without any external rescale.

Usage

from jaxstro.units import STELLAR
from progenax import MichieProfile, MichieVelocityDF

profile = MichieProfile.from_W0_rc(W0=7.0, r_c=1.0, r_a=8.0)   # positions
df = MichieVelocityDF(W0=7.0, r_c=1.0, r_a=8.0)               # velocities (2-D sampler)

masses = jnp.ones(1000)
positions = profile.sample_positions(masses, key_pos)
velocities = df.sample_velocities(positions, masses, key_vel, G=STELLAR.G)

Velocities are drawn by a 2-D marginal-then-conditional inverse-CDF over (vr,vt)(v_r, v_t) (no Osipkov-Merritt stretch trick — (1) is not a function of one integral). The whole pipeline (ODE solve + sampler) is JIT-compatible and differentiable in W0W_0, rcr_c, rar_a (FD-verified).

Validation

Implementation, validation & references

References
  1. Michie, R. W. (1963). On the distribution of high energy stars in spherical stellar systems. Monthly Notices of the Royal Astronomical Society, 125, 127–139. 10.1093/mnras/125.2.127
  2. King, I. R. (1966). The structure of star clusters. III. Some simple dynamical models. The Astronomical Journal, 71, 64–75. 10.1086/109857