What specific pressure supports the ultra-dense Neutron Star remnant?

Neutron degeneracy pressure

A Neutron Star forms as the remnant core after a supernova explosion when the core mass falls within a specific range, typically between about $1.4 M_{ ext{odot}}$ and roughly $3 M_{ ext{odot}}$. At this stage, the gravitational pressure is so immense that it forces protons and electrons to combine into neutrons. The resulting object is composed almost entirely of these closely packed neutrons. The final force preventing further gravitational collapse, which would otherwise lead to a black hole, is neutron degeneracy pressure. This pressure arises because the neutrons, like electrons, resist being forced into the same quantum state, providing the structural support for this mind-bogglingly dense object where a single teaspoon would weigh billions of tons.