Abstract Details
(2020) Large Scale Nucleosynthetic Heterogeneities Across the Solar System Identified by Xenon
Avice G, Gilmour J & Moreira M
https://doi.org/10.46427/gold2020.94
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01g: Room 1, Tuesday 23rd June 08:42 - 08:45
Guillaume Avice
View abstracts at 11 conferences in series
Jamie Gilmour View abstracts at 5 conferences in series
Manuel Moreira View all 2 abstracts at Goldschmidt2020
Jamie Gilmour View abstracts at 5 conferences in series
Manuel Moreira View all 2 abstracts at Goldschmidt2020
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Submitted by Emily Worsham on Monday 22nd June 17:33
Hi, the comet-Xe and start-Xe patterns look like a complement to Xe-HL, so are these compositions reflecting a depletion in this component, or do you really need separate r- and p-process carriers? Mo isotopes suggest that there was a homogenized nebular component where r- and p-process isotopes were coupled. Is this inconsistent with Xenon?
Hi, thank you for your question. Indeed Comet-Xe and Start-Xe look like a mirrored HL-Xe. However, U-Xe the starting composition of atmospheric Xe does not present important depletions in p-process 124Xe and 126Xe relative to Solar-Xe. Somehow, we need to add pure p-process to Comet-Xe or Start-Xe to reproduce U-Xe. Adding HL-Xe would lead to a departure for r-process 134Xe and 136Xe.
Hi, the comet-Xe and start-Xe patterns look like a complement to Xe-HL, so are these compositions reflecting a depletion in this component, or do you really need separate r- and p-process carriers? Mo isotopes suggest that there was a homogenized nebular component where r- and p-process isotopes were coupled. Is this inconsistent with Xenon?
Hi, thank you for your question. Indeed Comet-Xe and Start-Xe look like a mirrored HL-Xe. However, U-Xe the starting composition of atmospheric Xe does not present important depletions in p-process 124Xe and 126Xe relative to Solar-Xe. Somehow, we need to add pure p-process to Comet-Xe or Start-Xe to reproduce U-Xe. Adding HL-Xe would lead to a departure for r-process 134Xe and 136Xe.
Submitted by Emily Worsham on Monday 22nd June 17:34
As you point out, there are distinct relative proportions of p- and r-process isotopes in the CC and NC reservoirs, but other elements suggest an r-process enrichment in the CC reservoir, which appears inconsistent with the Xe r-process depletion in comets. How do you explain this discrepancy?
This is indeed puzzling and this remains to be solved. There are two interesting points to take into account: 1) maybe cometary gas comes from much greater distance compared to where carbonaceous chondrites formed ? This would lead to as solar system with r-process depletion / r-process enrichment / r-process depletion when you increase the distance relative to the Sun. I agree that this is not really satisfactory; 2) Rosetta results obtained on 67P/C-G are for gas, not for the refractory component of the comet, which could be CC-like with a r-process enrichment.
As you point out, there are distinct relative proportions of p- and r-process isotopes in the CC and NC reservoirs, but other elements suggest an r-process enrichment in the CC reservoir, which appears inconsistent with the Xe r-process depletion in comets. How do you explain this discrepancy?
This is indeed puzzling and this remains to be solved. There are two interesting points to take into account: 1) maybe cometary gas comes from much greater distance compared to where carbonaceous chondrites formed ? This would lead to as solar system with r-process depletion / r-process enrichment / r-process depletion when you increase the distance relative to the Sun. I agree that this is not really satisfactory; 2) Rosetta results obtained on 67P/C-G are for gas, not for the refractory component of the comet, which could be CC-like with a r-process enrichment.
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