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Our workshop program provides training and teaching in topics across geochemistry and related fields. We are currently liaising with the workshop organisers to ascertain if any workshops can become virtual. Any updates will be added to this page.
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Extraction of Life-Essential Volatiles via Melting of Rocky Planetary Mantles of Variable Redox
Dasgupta R, Chowdhury P, Eguchi J, Sun C & Saha S
Dasgupta R, Chowdhury P, Eguchi J, Sun C & Saha S (2020) Goldschmidt Abstracts, 2020 525
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01a: Room 1, View in program
Listed below are questions that have been submitted by the community that the author will try and cover in their presentation. To submit a question, ensure you are signed in to the website. Authors or session conveners approve questions before they are displayed here.
Can your results be extended to Io? There seems to be a lot of basaltic/komatiitic volcanism wth very S-rich composition. So, is Io very reduced? And if yes, is that expected for a body in the outer Solar System?
This is a very interesting question. I am not sure whether this can be answered with certainty without additional data on Io. It is certain that Io exhibits degassing of sulfur-rich plume but do we know the composition of Io's crust (e.g., S budget of the crust) well? Without such it may be difficult to assess whether S-rich plume compositions can be taken as an evidence of S-rich basaltic crustal composition. If Io's crust is indeed very S-rich, similar to Mercury's, I might speculate that Io's interior is reduced. It may also be that when it comes to the interior oxidation state of rocky interiors, the exact monotonic oxidation with increasing heleocentric distance does not hold. In other words, I don't think we can rule out some outer Solar System bodies being more reduced, although that may not be the norm.
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