Block 3: N-body
Halo formation simulations with entropic friction, generating Burkert profiles.
The Cusp-Core Problem
Problem in ΛCDM
The standard model (ΛCDM) predicts dark matter halos with NFW profiles that have a “cusp” at the center: the density diverges as ρ ∝ 1/r.
However, observations show flat cores in dwarf and LSB galaxies.
MCMC proposal (earlier corpus)
In the proposal of the earlier corpus, entropic friction slowed particles in regions of high density, which prevented the formation of cusps and produced flat cores in those simulations (historical record, not reproduced today: FE-08-2026, E7).
Entropic Friction
The friction coefficient depends on the local density:
Where α = 0.1 is the friction parameter and ρc is the critical density.
Burkert Density Profile
Entropic friction generates Burkert-type profiles:
Unlike the NFW profile, this one has a flat core (ρ → ρ₀ as r → 0).
Core-Mass Relation
The core radius scales with the halo mass:
Parameters
| Parameter | Value | Description |
|---|---|---|
| α (friction) | 0.1 | Entropic friction coefficient |
| exponent | 1.5 | Density exponent |
| r_s (NFW) | ~20 kpc | Typical NFW scale radius |
Comparison: NFW vs Burkert
Physical Interpretation
Why Does It Work?
Entropic friction acts as a “brake” that disperses the kinetic energy of dark matter particles in dense regions:
- At the center of the halo, where ρ is high, the friction is maximal
- The particles lose speed and cannot concentrate any further
- A core of constant density forms
Connection with Philosophy
Entropic friction is the mechanism by which the “resistance of space” limits the excessive concentration of mass, maintaining cosmic equilibrium.
Implementation in Python
📁 File: simulations/bloque3_nbody.py