Retrieving "Volatile Compounds" from the archives
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Geological History
Linked via "volatiles"
The initial phase, termed the Hadean Eon (approximately $4.54$ to $4.0$ billion years ago, Ga), commenced with the accretion of the proto-Earth from the solar nebula. Geophysical modeling suggests that during this period, the planet experienced intense bombardment, leading to substantial thermal retention. A defining, though theoretical, feature of the Hadean is the "Magmatic Ocean Phase," where much of the su…
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Planetary Differentiation Processes
Linked via "volatile compounds"
The Role of Volatiles and Surface Layering
Differentiation is not purely a function of high-temperature silicate/metal fractionation. The outgassing and sequestration of volatile compounds (e.g., water ($\text{H}2\text{O}$), carbon dioxide ($\text{CO}2$), and noble gases) define the outer layers of the planet.
On terrestrial planets, volatiles are concentrated in the crust and [atmosphere](/entrie… -
Solar System Formation
Linked via "volatile compounds"
At the inner regions (less than $3$ AU), temperatures exceeded $1,500 \text{ K}$, allowing only high-refractory materials, such as silicates and iron-nickel alloys, to condense into solid grains. This region formed the terrestrial planets.
Beyond the "Frost Line" (or Ice Line), located roughly between $3$ and $5$ AU depending on local pressure, temperatures dropped sufficiently (below $170 \text{ K}$) for [volatile compounds](… -
Solar System Formation
Linked via "Volatiles ($\text{CH}_4, \text{NH}_3$)"
| Fe-Ni Alloy | $800 - 500 \text{ K}$ | Mid Disk | Asteroid Belt |
| Water Ice ($\text{H}_2\text{O}$) | $170 \text{ K}$ | Beyond $3.5$ AU (Frost Line) | Jupiter (planet)/), Saturn (planet)/) Cores |
| Volatiles ($\text{CH}4, \text{NH}3$) | $<100 \text{ K}$ | Outer Disk | Kuiper Belt Objects |
The distinct lack of sufficient rocky…