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Binary energy budget (B9)

San Diego State University

A cluster with primordial binaries carries two energy scales, and conflating them is a classic mistake. build_binary_cluster virializes the system centres-of-mass to Q=0.5Q=0.5 treating each binary as a single point mass — the McLuster scale-separation convention Küpper et al., 2011 — and leaves the internal binary binding energy as a separate reservoir that the global virial scaling never touches. This demo makes that separation explicit and shows why the naive virial ratio of the resolved stars is not the cluster’s.

The two scales, from binary_energy_budget:

Qresolved=TWresolved stars  Qcom,Q_{\rm resolved} = \frac{T}{|W|}\Big|_{\rm resolved\ stars} \ \neq\ Q_{\rm com},

because the resolved ratio mixes the two scales. It is not the cluster’s virial ratio (audit S10): a hard binary’s internal virial is itself 0.5\approx 0.5 (time-averaged), so sampled at random orbital phases QresolvedQ_{\rm resolved} scatters around 0.5 rather than deflating monotonically. The robust, gated statement is the energy separationQcomQ_{\rm com} cleanly recovers 0.5 while Einternal|E_{\rm internal}| dwarfs Wcom|W_{\rm com}|.

Why a young cluster. Primordial binaries are the population present at birth, before dynamical processing ionizes the soft ones and hardens the rest. Their natural home is therefore a young cluster, for which the Elson–Fall–Freeman (1987) Elson et al., 1987 extended power-law profile is the standard parametrization — not the King model of an old, relaxed globular. So the primary cluster here is EFF (a=1a=1 pc, γ=2.5\gamma=2.5, rt=15r_t=15 pc); a concentrated King (W0=7W_0=7) King, 1966 appears only in the environment figure (below).

What is built

A Plummer-masses-first EFF young cluster of Nsys=2000N_{\rm sys}=2000 systems, virialized to Q=0.5Q=0.5, with a smooth (differentiable) Maschberger α=2.3\alpha=2.3 primary IMF over [0.08,100]M[0.08, 100]\,\Msun and companions from IndependentCompanions (or the full Moe & Di Stefano (2017) Moe & Di Stefano, 2017 model). Two controlled sweeps:

Inputs and assumptions

This demo fits nothing — it is a controlled sweep over hardness and binary fraction, gating the energy separation and reporting diagnostics. Every quantity is a known/fixed physical input or a swept/numerical choice.

Table 1:Model inputs

Input

Meaning and role

Status (fiducial)

EFF a,γ,rta,\gamma,r_t

Young-cluster profile (scale, slope, truncation) — the primary cluster potential WcomW_{\rm com}.

known / fixed (1.0, 2.5, 15.0)

King W0,rcW_0, r_c

Concentrated GC-like comparison potential (environment figure only).

known / fixed (7.0, 1.0)

primary IMF

Maschberger (α=2.3\alpha=2.3, 0.08100M100\,M_\odot) — draws primaries, hence m1m2m_1 m_2 and EinternalE_{\rm internal}.

known / fixed

qq distribution, eccentricity

Flat mass ratio with qmin=0.3q_{\min}=0.3, and a thermal ee distribution (the headline sweeps use these independent distributions, not the Moe coupling).

known / fixed

QQ (virial)

Build-time virial ratio the system centres of mass are scaled to.

known / fixed (0.5)

NsysN_{\rm sys}, GG

System count (2000); STELLAR units.

known / fixed

period band, fbf_b sweeps, seeds, gates

LOGP_CENTERS (hard\tosoft) and FB_VALUES (0.11.0); per-point seeds SEED+i; gates Qcom0.5<102|Q_{\rm com}-0.5|<10^{-2}, realized-fbf_b 3σ3\sigma Poisson.

sweep / numerical choices

Result — freshly run, ALL PASS

Measured 2026-06-12 (CPU/float64, Nsys=2000N_{\rm sys}=2000, seeds from PRNGKey(0); wall 32\approx 32 s; exit 0).

Hardness sweep (EFF, fb=0.5f_b=0.5). QcomQ_{\rm com} is pinned at 0.5 to four decimals at every point; Einternal|E_{\rm internal}| spans three orders of magnitude; QresolvedQ_{\rm resolved} scatters (the contamination):

log10P\log_{10} P

QcomQ_{\rm com}

QresolvedQ_{\rm resolved}

Einternal|E_{\rm internal}|

Wcom|W_{\rm com}|

1.5 (hard)

0.5000

0.464

1.22×1061.22\times10^{6}

6.4×1026.4\times10^{2}

2.5

0.5000

0.420

8.4×1058.4\times10^{5}

1.0×1031.0\times10^{3}

3.5

0.5000

0.512

4.1×1044.1\times10^{4}

5.2×1025.2\times10^{2}

4.5

0.5000

0.491

1.4×1041.4\times10^{4}

6.4×1026.4\times10^{2}

5.5 (soft)

0.5000

0.327

7.1×1037.1\times10^{3}

6.1×1026.1\times10^{2}

Across both sweeps the reservoir ratio Einternal/Wcom|E_{\rm internal}|/|W_{\rm com}| stays in [11.6, 1.9×103][11.6,\ 1.9\times10^{3}] — the internal binding always dwarfs the cluster potential — while maxQresolvedQcom=0.257\max|Q_{\rm resolved}-Q_{\rm com}| = 0.257 confirms the resolved ratio is a contaminated proxy. Gate summary:

Check

Gate

Status

Qcom0.5Q_{\rm com}\approx0.5 (all 12 points)

Qcom0.5<0.01|Q_{\rm com}-0.5|<0.01

PASS

Einternal<0E_{\rm internal}<0 (all bound)

<0<0

PASS

realized fbf_b matches set fbf_b

3σ3\sigma Poisson

PASS

Einternal>Wcom|E_{\rm internal}|>|W_{\rm com}| (all points)

reservoir dwarfs potential

PASS

EinternalE_{\rm internal} identical EFF vs King (same key)

controlled comparison

PASS

reservoir fraction EFF >> King

environment effect

PASS

The environment comparison

The same realistic Moe & Di Stefano population is laid into a young EFF and a concentrated King (W0=7W_0=7) potential using the same random key, so the masses and orbital elements — and therefore EinternalE_{\rm internal} — are byte-identical between the two. Only the cluster structure differs:

Cluster

rhr_h

Einternal|E_{\rm internal}|

Wcom|W_{\rm com}|

Einternal/Wcom|E_{\rm internal}|/|W_{\rm com}|

EFF (young)

5.32 pc

2.965×1052.965\times10^{5}

6.7×1026.7\times10^{2}

440

King W0=7W_0=7 (GC-like)

3.26 pc

2.965×1052.965\times10^{5}

9.9×1029.9\times10^{2}

298

The concentrated King is more tightly bound (Wcom|W_{\rm com}| larger), so the same primordial binary population is a relatively larger energy store in the young, puffy cluster — the global importance of the binary reservoir depends on the birth environment. This is the Heggie (1975) hard/soft intuition at the level of the total energy budget; a per-binary hard/soft classification (Ebind|E_{\rm bind}| vs the local kTkT) is a related but distinct quantity and is not claimed here.

Figures

EFF young-cluster sweeps (scripts/demo_binary_energy_budget.py). (a)
Hardness sweep: Q_{\rm com} pinned at 0.5 (blue) while Q_{\rm resolved}
(vermilion) scatters around it — the resolved ratio is not the cluster’s. (b)
|E_{\rm internal}| (green) towers over |W_{\rm com}| (purple) and grows three
orders as binaries harden. (c, d) Binary-fraction sweep: same Q_{\rm com}
pinning, and the reservoir fraction rising with f_b, with the realistic
Moe & Di Stefano population marked (★).

Figure 1:EFF young-cluster sweeps (scripts/demo_binary_energy_budget.py). (a) Hardness sweep: QcomQ_{\rm com} pinned at 0.5 (blue) while QresolvedQ_{\rm resolved} (vermilion) scatters around it — the resolved ratio is not the cluster’s. (b) Einternal|E_{\rm internal}| (green) towers over Wcom|W_{\rm com}| (purple) and grows three orders as binaries harden. (c, d) Binary-fraction sweep: same QcomQ_{\rm com} pinning, and the reservoir fraction rising with fbf_b, with the realistic Moe & Di Stefano population marked (★).

Birth-environment comparison (same Moe population, same key). (a)
|E_{\rm internal}| is identical between EFF and King (the controlled comparison);
|W_{\rm com}| is larger for the concentrated King. (b) The reservoir fraction
|E_{\rm internal}|/|W_{\rm com}| is therefore larger in the young EFF cluster.
r_h for each cluster is annotated.

Figure 2:Birth-environment comparison (same Moe population, same key). (a) Einternal|E_{\rm internal}| is identical between EFF and King (the controlled comparison); Wcom|W_{\rm com}| is larger for the concentrated King. (b) The reservoir fraction Einternal/Wcom|E_{\rm internal}|/|W_{\rm com}| is therefore larger in the young EFF cluster. rhr_h for each cluster is annotated.

Caveats

How to run

env -u VIRTUAL_ENV uv run --no-sync python scripts/demo_binary_energy_budget.py

References

The EFF young-cluster profile is Elson et al. (1987); the King model King (1966); the binary statistics follow Moe & Di Stefano (2017); the COM/internal scale separation is the McLuster convention Küpper et al. (2011); the hard/soft intuition is Heggie (1975). The budget API and its vis-viva / scale-separation tests live in progenax.binaries.diagnostics.

References
  1. Küpper, A. H. W., Maschberger, T., Kroupa, P., & Baumgardt, H. (2011). McLuster: A tool for making star clusters. Monthly Notices of the Royal Astronomical Society, 417, 2300. 10.1111/j.1365-2966.2011.19412.x
  2. Elson, R. A. W., Fall, S. M., & Freeman, K. C. (1987). The structure of young star clusters in the Large Magellanic Cloud. The Astrophysical Journal, 323, 54–78. 10.1086/165807
  3. King, I. R. (1966). The structure of star clusters. III. Some simple dynamical models. The Astronomical Journal, 71, 64–75. 10.1086/109857
  4. Moe, M., & Di Stefano, R. (2017). Mind your Ps and Qs: The interrelation between period (P) and mass-ratio (Q) distributions of binary stars. The Astrophysical Journal Supplement Series, 230, 15. 10.3847/1538-4365/aa6fb6
  5. Heggie, D. C. (1975). Binary evolution in stellar dynamics. Monthly Notices of the Royal Astronomical Society, 173, 729–787. 10.1093/mnras/173.3.729