The planets in the inner part of the Solar System are made...

The planets in the inner part of the Solar System are made primarily of refractory materials; the planets in the outer Solar System are made primarily of volatiles. The difference occurred because a. refractory materials are heavier than volatiles, so they sank farther into the nebula. b. there were no volatiles in the inner part of the accretion disk. c. the volatiles on the inner planets were lost soon after the planet formed. d. the outer Solar System has gained more volatiles from space since formation.

The planets in the inner part of the Solar System are made primarily of refractory materials; the planets in the outer Solar System are made primarily of volatiles. The difference occurred because
a. refractory materials are heavier than volatiles, so they sank farther into the nebula.
b. there were no volatiles in the inner part of the accretion disk.
c. the volatiles on the inner planets were lost soon after the planet formed.
d. the outer Solar System has gained more volatiles from space since formation.

Key Concepts

Planetary Formation Process in a Nebular Context

The formation of planets occurs within a rotating disk of gas and dust around a newborn star, known as a protoplanetary disk. The distribution of materials within this disk, influenced by its temperature profile, plays a crucial role in determining the composition of the resulting planets. Inner planets, formed in hotter regions, lose or fail to accrete volatiles, while outer planets, forming in colder regions, can capture and retain these lighter compounds.

Protoplanetary Disk Temperature Gradient

The protoplanetary disk surrounding a young star has a temperature gradient, with higher temperatures near the star and cooler conditions further away. This gradient influences the condensation and retention of materials; only substances with high condensation temperatures (refractory materials) could remain solid close to the star, while substances that condense at lower temperatures (volatiles) can be preserved only in the colder, outer regions of the disk.

Refractory and Volatile Materials

Refractory materials are chemical compounds that remain solid at high temperatures, making them prevalent in regions close to the star. In contrast, volatile materials have low condensation temperatures and tend to evaporate or remain gaseous in warmer environments, leading to their accumulation in the cooler outer regions. This fundamental difference explains the variance in planetary composition within a solar system.

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