The Michie (1963) radial-anisotropy term on King’s (1966) lowered cutoff: a
self-consistent, radially anisotropic cluster model. Test file:
tests/validation/test_michie_physics.py (see the
test dashboard for the live per-suite count); figures:
scripts/validate_michie.py. Theory at
Michie-King anisotropic model.
What is verified¶
Each row maps to assertions in test_michie_physics.py. Measured values are
regenerated by scripts/validate_michie.py. All use , , with
for the anisotropic case (it truncates: ) and
for the isotropic limit.
Property | Tolerance (as tested) | Measured | Anchor |
|---|---|---|---|
Isotropic limit: | 10-2 max rel | recovers King | |
King-limit convergence () | at | monotone-ish grid floor | |
Anisotropy vs DF oracle | per bin | max dev 0.027 | 2nd moments of the exact DF |
below Osipkov-Merritt ceiling | True (all bins) | lowering term breaks | |
isotropic at center, radial outward | , increasing | Michie anisotropy | |
More anisotropic more extended | radial-orbit support | ||
Virial ratio (unscaled) | 0.501 | , self-consistent | |
Bound fraction () | 100% | 100.00% | |
Over-anisotropy guarded | raises | raised () | no finite tidal radius |
Sampling differentiability () | AD central-FD | rel err , , |
|
Figures¶
Generated by scripts/validate_michie.py (PASS/FAIL per panel; PNG + PDF vector).

Figure 1:The anisotropy signature. Sampled (points) tracks the Michie-King DF oracle (solid, the 2nd-moment integral of the exact DF) to max deviation 0.027 — and both sit well below the pure Osipkov-Merritt ceiling (dotted). at the isotropic core, grows radially outward, and turns back toward isotropy at the tidal boundary.

Figure 2:Table-routed draws vs the exact quadrature oracle (,
, ). Since the 2026-06 memory batch,
MichieVelocityDF draws speeds from the anisotropic CDF table at
(Michie ≡ LIMEPY anisotropic — change-of-variables proven and
brute-force verified), with the original 2-D quadrature retained as
speed_method="quadrature". (a) Speed distributions: KS
(gate ; unpaired comparison — the two paths consume keys in different
orders). (b) Measured : (gate ).
Script: scripts/validate_speed_routing.py; see
performance & memory.

Figure 3:Anisotropic dispersions and equilibrium. (a) The radial dispersion exceeds the per-component tangential by a margin that widens outward — the kinematic signature of radial anisotropy. (b) Every velocity is bound, — 100%. (c) The unscaled IC is virial, , with no external rescale (self-consistent ).

Figure 4:Density and the King limit. As the Michie density coincides with the isotropic King profile (max rel ); finite (radial anisotropy) makes the model more extended ( at vs 33.8 for King).

Figure 5:Isotropic-limit convergence. The maximum density deviation from King falls with , reaching (an ODE-grid floor) by — well inside the 10-2 tolerance. The dip near is a genuine density-profile crossing.
Differentiability¶
The Michie structural parameters are differentiable through the diffrax ODE solve
and the jax.lax.scan sampling, enabling gradient-based / HMC inference of the
anisotropic model.

Figure 6:Gradient validation (autodiff vs central finite difference). for (a) , (b) , (c) : autodiff and finite difference agree to max rel err , , , so the anisotropic model can be fit jointly with the structural parameters.
How to run¶
# physics tests (~22 s on CPU)
pytest tests/validation/test_michie_physics.py -q
# regenerate the five figures with PASS/FAIL tables
python scripts/validate_michie.pyWhat this suite does not test¶
Multi-mass anisotropic equilibrium — single-mass Michie-King is covered; the multi-mass generalization is part of the lowered-model-family roadmap.
References¶
Michie (1963) (anisotropy term) and King (1966) (lowered cutoff). The per-paper notes are in the bibliography; theory and the DF derivation at Michie-King anisotropic model.
- 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
- King, I. R. (1966). The structure of star clusters. III. Some simple dynamical models. The Astronomical Journal, 71, 64–75. 10.1086/109857