The atoms in the core of a star fuse together under the intense pressure, producing vast amounts of heat and energy.
When a neutron star is formed, protons and electrons are crushed, they collide and become neutrons.
The strong gravity of the core of a dead high-mass star causes a neutron star to form. When the high-mass star becomes a supernova and leaves a core behind, the core no longer undergo fusion. Without fusion, gravity starts to push the core inward until most protons and electrons are crushed into neutrons, a neutron star forms. If the core is too massive, the neutron star would collapse and become a black hole.
A supernova occurs in a star's lifecycle when it runs out of fuel and its core collapses, causing a massive explosion.
In a neutron star, protons and electrons are indeed fused together through the extreme pressure. This process transforms some protons into neutrons through inverse beta decay, producing a core made mostly of neutrons with a small fraction of protons and electrons.
In all stars, the fusion only occurs in the inner core.
It is extremely unlikely that a neutron star (or any star or planet) will collide with the Earth, so this is not something that you need to worry about, however, if a neutron star were to collide with the Earth, the Earth would be captured by the intense gravitational field of the neutron star, and would be absorbed by the star. Under sufficient pressure, electrons and protons will merge to form neutrons, and so the atomic matter of which the Earth is composed can be converted into pure neutrons.
Stars may collapse to such a degree, perhaps after a supernova, that, in the core, electrons are squashed into the nucleus, reacting with protons to form neutrons. A star of this collapsed state is called neutron stars.
Photodisintegration and neutronizatoin both absorb some amount of energy to be carried forth and so contribute to the rapid cooling of the core, which accelerates the collapse of the star, since the reduced energy output disrupts the hydrostatic equilibrium of the star's layers.
The basic reactions: First 2 hydrogen nuclei (protons) fuse to form deuterium, a hydrogen isotope (1 proton, 1 neutron). Deuterium then fuses with another proton to form a light helium isotope, helium3 (2 protons, 1 neutron. 2 helium3 nuclei fuse to form Helium4 (2 protons 2 neutrons), + 2 hydrogen nuclei (protons).
Before a supernova occurs, a massive star undergoes fusion to produce iron in its core. As fusion progresses, the star creates heavier elements up to iron, which cannot release energy through fusion. When the core becomes predominantly iron, it can no longer support the star against gravitational collapse, leading to a supernova explosion.
After a planetary nebula occurs, the core of the star collapses and becomes a white dwarf. This white dwarf slowly cools down over billions of years until it eventually becomes a cold, dark remnant known as a black dwarf.
The star "burns out" because iron cannot be fused. What happens then depends on the star's remaining mass:low - white dwarfmed. - neutron starhigh - black hole