The Unraveling of Atoms: Radioactive Decay Explained

Protoplanetary Disks

The process begins with a molecular cloud – vast regions of space containing hydrogen gas and dust. These clouds, often triggered by events like supernova explosions, begin to collapse under their own gravity.

As the cloud collapses, it spins faster and flattens into a rotating disk called a protoplanetary disk. This disk is where most planets form.

Accretion – Building Blocks of Planets

Within the protoplanetary disk, dust grains collide and stick together through electrostatic forces. This process, called accretion, gradually builds larger clumps of material.

These clumps grow into planetesimals – bodies ranging from a few kilometers to hundreds of kilometers in diameter. The more massive a planetesimal becomes, the stronger its gravitational pull.

μ = GmM/r² (where μ is gravitational force, G is the gravitational constant, m is mass, and r is distance)

From Planetesimals to Planets

Planetesimals continue to collide and merge through a process called accretion. Larger planetesimals sweep up smaller ones, eventually forming protoplanets.

The inner regions of the disk are hotter, preventing volatile substances like water ice from condensing. This results in the formation of rocky planets like Mercury, Venus, Earth, and Mars.

Formation of Gas Giants

Further out in the protoplanetary disk, temperatures are cooler, allowing volatile compounds like water ice and methane to condense. This material then accumulates around a core of rock and metal.

This process leads to the formation of gas giants like Jupiter and Saturn, which grow by accreting vast amounts of gas from the surrounding disk.

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