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24 October 2008
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Karin Oberg (Leiden)
"The evolution of ices around solar-type protostars"
Ice chemistry matters. In the densest star forming regions, most molecules
(except for H2) are frozen out on dust grains. Understanding the evolution
of ices is hence crucial to constrain the chemical evolution at large during
star- and planet-formation. In this talk I will address some of the fundamental
questions concerning this ice evolution: What is the ice inventory around
young solar-type stars? Why do some ices exist at almost constant abundances,
while others are highly variable? What is the maximum amount of chemical
complexity reached in circumstellar ices? Under which conditions and by
which processes are ice species released back into the gas phase? The answers we
have so far build on a combination of Spitzer ice observational data together
with laboratory studies on ice photochemistry and ice photodesorption. These
questions can also be addressed using millimeter observations and I will finish
with how ice abundances may be indirectly observed in protostellar envelopes
using gas phase diagnostics.
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