Oxygen solar system photochemistry

In this chapter, I wish to explore the possible role of photochemistry (an inherently disequilibrium process) in formation of the planets and smaller bodies in the solar system. As was seen in the planetary examples above, the small differences in chemical properties of the stable isotopes of abundant light elements, especially carbon, nitrogen, and oxygen, provide key information regarding nebular chemistry. The rapid attenuation of light in a cloud of dust and gas requires that the irradiation region be continuously replenished, so that chemistry and dynamics are intimately interrelated. 

Photochemistry appears to be well established for oxygen and nitrogen in the early Solar System. Consideration should also be given to the possibility of analogous effects in hydrogen. 

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