A Cosmic Dance We Didn’t Expect ✛ ✎ ✦

Original: "Constant Scaling Fails for Global Monopole Networks"
· Wakutaka Nakano, Wen Yin
arXiv:2607.05517 · 2026-07-06 · arXiv non-exclusive · independent analysis · 1 min
New simulation: knot-like particles from the early universe don’t vanish: they slowly accumulate.

The expanding universe can be imagined as a dance floor that relentlessly stretches. Monopoles and anti-monopoles are like dancers looking for a partner to vanish in an embrace. It was once thought that over time, all pairs find each other and the hall empties. But a new computer model showed that when the floor becomes too spacious, encounters become rarer, and new singles take the stage — the number of monopoles slowly crawls upward. These knot-like particles, predicted by Gerard ’t Hooft, were born right after the Big Bang, during the era of rapid inflation (an idea by Alan Guth).

This slow growth changes the scenario. If there are more monopoles, they could have become part of dark matter, the invisible substance that gathers galaxies, and link up with dark photons from the hidden sector. Their pull could have spawned primordial black holes, left ripples in gravitational waves, and a trace in the cosmic microwave background. The most unexpected twist: whereas it was once thought that only a handful would survive, now it turns out there could be thousands, and they are capable of bending starlight, betraying themselves to telescopes.

According to old estimates, only a few monopoles would have survived to this day. The new scenario yields thousands, and they can noticeably bend the light of distant stars, like invisible lenses.

E(R) \simeq 4\pi v^2 R
monopole energy grows linearly with the distance R to the antimonopole due to field gradients of Goldstone bosons
\tau_{\rm ann} = D \left( c_0 + c_1 \ln\frac{D}{r_{\rm core}} \right)
The annihilation time depends on the ratio of the distance D to the core size r_core, producing a logarithmic correction to the scaling
Concepts
galaxy growth mechanisms eternal inflation structure growth magnetic monopole Dollo's law scalable Cope's rule large-scale structure of the universe magnetic monopole dark matter Gause's competitive exclusion principle quantum cosmological inhomogeneities galaxy distribution cosmic expansion cosmological constant problem topological pattern formation inflationary cosmology multi field inflation scale factor galactic evolution processes hubble constant