Physico‐chemical modeling of condensation in the early Solar system:
Why are condensation models needed?
- The planet‐forming inner region in a physical model of solar nebula introduced by Cameron (1963) was totally vaporized.
- Therefore, before making planets nebular gas had to condense and accumulate into planetary building blocks or planetesimals (@ meteorite parent bodies) made up of chondritic meteorites.
- While now it is clear that neither of these postulates is correct, modeling nebular condensation still remains a powerful tool for understanding and, in some cases, predicting both mineralogical and chemical evolution of nebular reservoirs in which the Solar System objects have formed.
- Another important application of such models is to evaluate mineralogy and chemistry of extrasolar planets orbiting stars chemically different from our Sun.
- The purpose of this presentation is to overview existing condensation models and to discuss their strengths and weaknesses using several examples
- First, I will introduce you in mineralogy and chemistry of chondritic meteorites
- Then describe equilibrium and non-equilibrium condensation models based on my own work
- Specifically discuss the concept of 50% condensation temperatures that is widely used in planetary studies, including exoplanets
- And describe application of condensation models to understanding origin and evolution of meteoritic objects and Moon
Refreshments at 3:30 p.m./Lecture at 3:45 p.m.
This event is free and open to the public.
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Physics and Astronomy Department