Unraveling the Secrets of Radioactive Decay

Formation of Protostars

Star formation begins with vast molecular clouds – regions containing primarily hydrogen and helium gas, along with traces of heavier elements. These clouds are not uniform; density fluctuations exist within them.

Slight overdensities within a cloud can trigger gravitational collapse. As material falls inward, it concentrates into denser clumps.

Protostar Formation

As the clump collapses, its density and temperature increase dramatically. This collapsing cloud forms a rotating disk around a central core – a protostar.

The inward pressure from gravity is balanced by outward radiation pressure as the material heats up. Accretion of surrounding gas onto the protostar further fuels this process.

T ∝ (m/r), where T is temperature, m is mass, and r is radius.

Nuclear Fusion Ignition

Eventually, the core of the protostar reaches a critical temperature – approximately 10 million Kelvin. At this point, nuclear fusion begins: hydrogen nuclei fuse to form helium, releasing immense energy.

This outward pressure from fusion balances the inward force of gravity, establishing hydrostatic equilibrium and marking the birth of a true star.

4H → He + Energy ≈ 27 MeV

Stellar Evolution

The newly formed star enters its main sequence phase, fusing hydrogen into helium for billions of years. Its subsequent evolution depends on its initial mass.

More massive stars burn through their fuel much faster and end their lives in spectacular supernova explosions, while smaller stars gradually become white dwarfs.

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