Skip to article frontmatterSkip to article content
Site not loading correctly?

This may be due to an incorrect BASE_URL configuration. See the MyST Documentation for reference.

Tidal physics & substructure

San Diego State University

This section covers three orthogonal modifier layers that progenax applies on top of the base spatial profile + velocity DF + IMF combination (What is an initial condition?):

Modifier

What it adds to the IC

Tidal physics

Truncation at the Jacobi (tidal) radius set by the host galaxy’s tidal field

Fractal substructure

Theory of fractal/clumpy substructure (Goodwin & Whitworth (2004)) and the CW04 QQ diagnostic. The differentiable generator moved to the experimental, repo-only gravoturb package in the 2026-06 clean-room rewrite; released progenax keeps the diagnostics (progenax.diagnostics)

Mass segregation

Mass segregation two ways: the energy-ranked PRIMORDIAL generator (energy_sorted_segregation, after Baumgardt et al. (2008)) and the differentiable EQUILIBRIUM route (MultiComponentCluster.from_mass_segregation)

Tidal truncation is a standalone array utility and can be applied around either path. Turbulent/fractal substructure ICs live outside the released package (experimental gravoturb), so within released progenax the segregation routes and tidal truncation are the two modifiers you can actually apply.

Why these three?

The three correspond to the three observed deviations of real young / old clusters from smooth-equilibrium-sphere idealisations:

  1. Truncation. No real cluster extends to infinite radius. Old globular clusters are tidally limited; young clusters are limited by the embedding gas cloud’s mass. The tidal modifier captures this.

  2. Substructure. Young clusters inherit clumpy substructure from their parent molecular clouds Goodwin & Whitworth, 2004Allison et al., 2009. The fractal modifier captures this.

  3. Mass segregation. Old clusters show massive stars preferentially in their cores. Whether this is primordial Baumgardt et al., 2008 or dynamical Allison et al., 2009 is a debated observational question. The mass-segregation modifier seeds the primordial case.

All three are post-equilibrium in the sense that they perturb a base equilibrium IC. Whether the resulting non-equilibrium configuration is the right starting state for a given science target depends on the science: cool fractal ICs are appropriate for studying violent relaxation; smooth virial-equilibrium-plus-segregation is appropriate for studying long-timescale relaxation.

Current API sketch

import jax
import jax.numpy as jnp
from jaxstro.units import STELLAR
from progenax import MultiComponentCluster
from progenax.tidal import jacobi_radius, apply_tidal_truncation

# Equilibrium mass segregation: two components in ONE shared potential,
# with the equipartition law w_j = mu_j^(-delta) (differentiable in delta)
cluster = MultiComponentCluster.from_mass_segregation(
    alpha_j=jnp.array([0.5, 0.5]),   # central density fractions
    m_j=jnp.array([0.3, 1.0]),       # representative stellar masses [Msun]
    W0=7.0, g=1.0, delta=0.5,
)
ic = cluster.sample_cluster(jax.random.PRNGKey(42), n_stars=1000, G=STELLAR.G)
# ic.component_id labels each star's generating component

r_J = jacobi_radius(
    M_cluster=1e4,
    M_galaxy=1e10,
    R_galactic=8000.0,
)
positions, velocities, masses, keep_mask = apply_tidal_truncation(
    ic.positions, ic.velocities, ic.masses, r_t=r_J,
)

For primordial (non-equilibrium) segregation, use progenax.energy_sorted_segregation to energy-rank an orbit pool drawn from any equilibrium profile — see Mass segregation. The legacy string-dispatch generator (generate_cluster_ic with SpatialStructureParams layers) was retired in the 2026-06 unified redesign.

Implementation, validation & references

References
  1. Goodwin, S. P., & Whitworth, A. P. (2004). The dynamical evolution of fractal star clusters: The survival of substructure. Astronomy and Astrophysics, 413, 929–937. 10.1051/0004-6361:20031529
  2. Baumgardt, H., De Marchi, G., & Kroupa, P. (2008). Evidence for primordial mass segregation in globular clusters. The Astrophysical Journal, 685, 247–253. 10.1086/590488
  3. Allison, R. J., Goodwin, S. P., Parker, R. J., Portegies Zwart, S. F., de Grijs, R., & Kouwenhoven, M. B. N. (2009). Using the minimum spanning tree to trace mass segregation. Monthly Notices of the Royal Astronomical Society, 395, 1449–1454. 10.1111/j.1365-2966.2009.14508.x
  4. Aarseth, S. J., Henon, M., & Wielen, R. (1974). A comparison of numerical methods for the study of star cluster dynamics. Astronomy and Astrophysics, 37, 183–187.
  5. Küpper, A. H. W., Maschberger, T., Kroupa, P., & Baumgardt, H. (2011). Mass segregation and fractal substructure in young massive clusters. Monthly Notices of the Royal Astronomical Society, 417, 2300–2317. 10.1111/j.1365-2966.2011.19412.x