Cosmology β˜…β˜…β˜… Advanced

πŸ•ΈοΈ Cosmic Web

Watch the large-scale structure of the Universe emerge spontaneously. Tiny density fluctuations grow under gravity into the stunning web of filaments, voids, and galaxy clusters we observe today.

Time: 0.0
Particles: 200
Clusters: β€”
Largest: β€”
Void fraction: β€”

Gravitational Instability & the Cosmic Web

The large-scale structure of the Universe β€” filaments, walls, voids and clusters β€” grew entirely from gravitational amplification of tiny quantum fluctuations (~10βˆ’5 amplitude) imprinted during inflation.

This simulation solves Newton's direct-summation N-body problem with softened gravity: a_i = GΒ·Ξ£_j m_jΒ·(r_jβˆ’r_i) / (|r_jβˆ’r_i|Β² + Ρ²)^(3/2), where Ξ΅ prevents singularities when particles approach each other. Periodic boundary conditions wrap particles at the box edges, mimicking a representative volume of the Universe.

Initial conditions use a uniform grid plus small sine-wave density perturbations (Zel'dovich approximation) to seed the collapse. The density field (colour map) is computed by counting particles per grid cell β€” brighter regions host more mass. Over time, matter streams from voids into filaments and collapses into dense nodes.