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Formation of the Solar System
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Formation of the Solar System
A nebula forms billions of years after the Big Bang, this nebula contained hydrogen and helium, as well as larger atoms formed in stars or supernovae.
- Some of these atoms combined together to make molecules. These molecules would later combine with a heavier element's molecules to make small particles of ice and dust.
- Heat dispersion caused by these particles decreased the thermal pressure of the collapsing nebula, allowing for the nebula to collapse to a point in which it reached a density suitable for a star to form
- The collapse of the nebula causes the material around it to rotate around an axis, to form what's called an accretion disk.
- The center of this accretion disk became the Sun, while the flattened outer part became a protoplanetary disk, the region in which planets would eventually form
- The collapse of the nebula causes the material around it to rotate around an axis, to form what's called an accretion disk.
- Heat dispersion caused by these particles decreased the thermal pressure of the collapsing nebula, allowing for the nebula to collapse to a point in which it reached a density suitable for a star to form
- Some of these atoms combined together to make molecules. These molecules would later combine with a heavier element's molecules to make small particles of ice and dust.
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- Description
- Descriptor of the early formation of our solar system
- Created by
- Jackson DeBorde
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