Massive stars, which are roughly 8–15 times more massive than the Sun, die and become neutron stars.
The dense inner core is all that is left after a massive star collapses and erupts in a massive supernova explosion.
The core of the dying star becomes increasingly denser as it collapses.
Protons and electrons in the core eventually can no longer withstand gravity and combine to form neutrons.
The core’s entire composition eventually decays into neutrons, and there you have it.
Now in Detail
The gravitational forces that stars exhibit are widely recognized.
This gravitational power is most intense at the star’s core, which is under tremendous pressure due to gravity.
The question arises: why doesn’t the core collapse under this intense gravitational force?
The answer lies in the intricate dance of nuclear fusion, energy, and the balance between opposing forces within the star.
Gravitational Equilibrium
The Marvel of Nuclear Fusion
Balancing Act
This continuous nuclear fusion not only generates substantial energy but also results in intense pressure within the star.
The March to Heavier Elements
As the star progresses in its life cycle, hydrogen fuses into helium, and this process continues with helium forming carbon, carbon transforming into nitrogen, and so on.
The Iron Paradox
However, a turning point arrives when iron production commences.
The Inevitable Collapse
With the depletion of hydrogen, helium, carbon, and other fusion materials, the balance between pressure and gravity is disrupted.
Stellar Endgame
For massive stars, this collapse leads to the core compressing into a singularity, birthing a black hole.
The Role of Electron and Neutron Degeneracy Pressure
With iron-rich cores unable to produce energy to resist further collapse, a different form of pressure intervenes: electron degeneracy pressure.
At this stage, temperatures are incredibly high, causing protons and electrons to combine and form neutrons.
Supernova and Neutron Star Formation
During this process, the immense gravitational pressure gives rise to an outburst of neutrinos, ejecting other materials into space in a spectacular supernova event.
In essence, this is the birth of a neutron star, a celestial body with an extraordinary density, akin to a colossal atomic nucleus, and typically measuring a mere 10 kilometers in width.
Conclusion
The formation of a neutron star is a cosmic ballet involving the interplay of gravitational forces, nuclear fusion, and the intricate balance between various forms of degeneracy pressure.
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