A handful of sand in your fist: the grains press against each other, and your hand can't squeeze any further. Ordinary matter behaves similarly. But in a neutron star, compression is billions of times stronger — atoms are crushed, electrons are squeezed into protons, and nearly all space is filled with neutrons. Yet this isn't just a dense packing of balls. At a certain depth, neutrons begin to 'feel' their constituent parts — quarks.

A new study offers a fresh perspective on this process. The authors expanded the popular 'quarkyonic matter' model to include not only light u- and d-quarks but also strange s-quarks, as well as the full set of eight baryons, from the proton to the xi-hyperon. The key idea is that at colossal densities, nucleons (protons and neutrons) cannot occupy low-energy states: those are already taken by quarks. They have to climb higher on the energy ladder. Like passengers in a crowded bus who have to stand even though there are seats, but they're cordoned off. This upward shift increases the nucleons' chemical potential, allowing a neutron star to pile on more mass before hyperons, particles with a strange quark, appear.

The calculations used an effective interaction between baryons that depends on density, momentum, and isospin (the difference between protons and neutrons). It's built on a modern high-order Skyrme potential. Quarks and leptons (electrons and muons) were treated as free. The result was satisfying: the quark mechanism noticeably pushes back the threshold for hyperon production, and the equation of state, the law linking pressure and density, becomes stiffer. In practice, this means the star can be heavier without collapsing into a black hole.

This matters for the 'hyperon puzzle': many models predicted that neutron stars with hyperons are too soft to reach the observed masses of two solar masses. Now there's a chance that quark rearrangement inside the star provides extra stiffness, like a frame embedded in concrete.