This project applies a simple phenomenological fitting function to galaxy rotation curves. The model adds an angular-momentum-dependent acceleration term to the baryonic contribution and tests whether this improves fits to 175 SPARC disk galaxies.
The total circular velocity is modelled as:
where the extra acceleration term is:
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$k$ — coupling constant [kg⁻¹ m⁻¹ s²], fitted per galaxy or globally -
$J_\text{vis}$ — visible-matter angular momentum computed from baryonic components only ($v_\text{gas}$ ,$v_\text{disk}$ ,$v_\text{bulge}$ ), evaluated at the half-mass radius — not from the observed curve -
$r_0 = 2 \times r_\text{half}$ per galaxy (robustness-scan optimum; previously fixed at 0.5 kpc)
Per-galaxy fit — primary result:
| Metric | Value |
|---|---|
| Galaxies | 175 SPARC |
| Mean error | 18.52% ± 14.96% |
| Median error | 15.76% |
| Best fit | UGC 00731 (1.86%) |
| Worst fit | UGC 02455 (107.91%) |
Global model comparison:
| Model A (universal |
Model B (power-law) | |
|---|---|---|
| Parameters | 1 | 2 |
| 0 | −0.652 | |
| Mean error | 32.60% | 34.52% |
| Median error | 29.62% | 23.34% |
| ΔAIC | — | −141,371 (B preferred) |
Two-population structure: ~11% of galaxies (20/175) converge to
Morphological correlations (weak):
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$\log_{10} k$ vs$\log_{10} J_\text{vis}$ :$r = -0.405$ ,$R^2 \approx 0.16$ -
$\log_{10} k$ vs disk scale length$h$ :$r = -0.249$ -
$\log_{10} k$ vs B/T: not significant
Cluster test: Mean error 72.5% on 6 galaxy clusters — model correctly fails for pressure-supported systems.
Lense-Thirring comparison: Fitted
Clone and install:
uv syncIf you use this code or model in your research:
@software{spinning-space-2026,
title={Spin-Mediated Acceleration as a Phenomenological Fitting Function for Galaxy Rotation},
author={Kherki, M.},
year={2026},
version={2.0},
url={https://github.com/Alpha-Centauri-00/a_extra}
}This work is licensed under a Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.
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Open an issue on GitHub
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Discussions welcome!
