The Crooked Seed That Spawned the Universe ✛

Original: "Enhancement of Weak Interactions in Phase Transitions"
· V. V. Flambaum
arXiv:2509.14701 · 2025-09-18 · CC BY 4.0 · 1 min
The tiny difference between left and right gets amplified billions of times during crystallization, and perhaps explains why matter beat antimatter.

The weak interaction, the most elusive of fundamental forces, creates a tiny imbalance between left- and right-handed versions of molecules. The difference is so small that in a solution it gets lost in thermal chaos, just as the curvature of a tiny seed goes unnoticed for a time.

But during crystallization, a seed forms first — a microscopic 'grain' of many atoms. If it reaches a critical size, the asymmetry of each molecule adds up to a mighty force. Much like a barely bent seed grows into a tree with a noticeable curve, the seed dictates the shape of the entire crystal. Experiments with electric and magnetic fields recorded an amplification of billions of times, allowing scientists to measure that critical number of atoms.

The seed of a new phase behaves like a seed: even its elusive asymmetry is passed on to the whole grown crystal.

In the early universe, after the Big Bang, a series of phase transitions could have repeatedly amplified the initial difference between matter and antimatter. Thus, a microscopic asymmetry in the fabric of existence turned into a grand imbalance that decided the fate of the cosmos.

The energy difference between left- and right-handed amino acids is so tiny that it's comparable to the energy a coin gains when lifted above a table by the thickness of a single atom.

This idea echoes Ray Bradbury's story 'A Sound of Thunder,' where a crushed butterfly changes the course of history — only here, the weak interaction plays the butterfly's role.

P \approx -\frac{N_c \Delta E}{2kT}
The relative difference in nucleation rates of left- and right-handed nuclei is proportional to the number of particles in the critical nucleus and the microscopic energy difference.
\Delta E \sim 10^{-12}\,\text{eV} \approx 10^{-8}\,\text{K}
Typical weak interaction energy in a molecule, converted to a temperature scale.
Scientists
Emmy NoetherWolfgang PauliEnrico FermiPaul DiracChien-Shiung WuEugene Wigner
Concepts
parity violation weak force cross section chirality interaction critical threshold particle interaction cp symmetry CP violation cosmological phase transition power law critical mass chemical potential scale factor coupling constant parity correlation coefficient carbon to oxygen ratio pion error threshold