Oxygen fugacity is a measure of rock oxidation that influences planetary structure and evolution. Most rocky bodies in the Solar System formed at oxygen fugacities approximately five orders of magnitude higher than a hydrogen-rich gas of solar composition.
Volatile molecules are critical to habitability, yet difficult to observe directly at the optically thick midplanes of protoplanetary disks, where planets form.
The increasing number of newly detected exoplanets at short orbital periods raises questions about their formation and migration histories.
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