Abstract Details
(2020) The Physical Chemical Frontiers of Mass Independent Isotope Effects
Thiemens M
https://doi.org/10.46427/gold2020.2589
The author has not provided any additional details.
14h: Plenary Hall, Wednesday 24th June 05:33 - 05:36
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Submitted by Jingjun Liu on Wednesday 24th June 23:01
Hi Mark, very enlightening talk! I have a question though: I am a bit confused about the temperature effect in the nebula. You said a small temperature change can lead to 10% increases in fractionation. But according to Janssen et al. 2003 CPL paper where they measured the temperature effect of 5 suit of ozone recombination reactions from 250K to 350K, the deepest temperature gradient is 0.1 per 100k for Q + O2 --> QOO (Q stands for 18O). Are the 10% you mentioned the same as this one? Interestingly, that isotopic ozone recombination reaction is 8% slower than the normal recombination reaction. The least temperature dependent is for O + OQ --> OOQ, and the value is 0.002 per 100K. I am curious if these measured temperature effects on lab behave differently in solar nebula?
Hi Mark, very enlightening talk! I have a question though: I am a bit confused about the temperature effect in the nebula. You said a small temperature change can lead to 10% increases in fractionation. But according to Janssen et al. 2003 CPL paper where they measured the temperature effect of 5 suit of ozone recombination reactions from 250K to 350K, the deepest temperature gradient is 0.1 per 100k for Q + O2 --> QOO (Q stands for 18O). Are the 10% you mentioned the same as this one? Interestingly, that isotopic ozone recombination reaction is 8% slower than the normal recombination reaction. The least temperature dependent is for O + OQ --> OOQ, and the value is 0.002 per 100K. I am curious if these measured temperature effects on lab behave differently in solar nebula?
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