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Understanding the Life Cycle of Stars
Apr 16, 2025
Life Cycle of Stars
Nebula
Begins with a cloud of dust and gas known as a
nebula
.
Gravity
pulls these materials together to form a
protostar
.
Protostar
As particles collide and join:
Protostar
gets larger.
Gravity strengthens, attracting more dust and gas.
Increased density leads to more frequent particle collisions and raises temperature.
High temperature and pressure cause:
Nuclear fusion
: Hydrogen nuclei fuse to form helium, releasing energy.
Forms a
main sequence star
.
Main Sequence Star
Balance
:
Outward pressure from energy release via nuclear fusion.
Inward pressure from gravity.
Sustains a long stable period, can last billions of years.
Example: Our Sun is in this stage.
Exhaustion of Hydrogen
Once hydrogen runs out, nuclear fusion ceases.
Gravity contracts the star into a small ball:
Temperature and density increase.
Nuclear fusion resumes, forming heavier elements (up to iron).
Evolution of the Star
Red Giant
:
If the star is small to medium-sized (like the Sun), it becomes a red giant.
Becomes unstable and expels outer layers of dust and gas.
Leaves a hot, dense core called a
white dwarf
.
White dwarf
cools and darkens, eventually becoming a
black dwarf
.
Red Supergiant
:
If the star is very large, it becomes a red supergiant.
Undergoes cycles of expansion and contraction.
Supernova
: Explodes, creating heavier elements than iron.
Distributes these elements across the universe.
Outcomes Post-Supernova
Neutron Star
:
Forms if the initial star was very big.
Extremely dense core.
Black Hole
:
Forms if the initial star was truly massive.
Gravity is so strong that even light cannot escape.
Recap
Stars form from nebulae.
Transition from protostar to main sequence star with nuclear fusion.
Hydrogen depletion leads to either red giant or red supergiant phase.
Red giants become white dwarfs, then black dwarfs.
Red supergiants result in supernovae, followed by neutron stars or black holes.
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