Upcoming SwRI Boulder Colloquia

Colloquia are normally on Tuesdays at 11:00 am in the 4th-floor conference room, except as indicated below in bold text.
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For questions or suggestions for speakers, please contact the SwRI colloquium organizers:
Raluca Rufu, 303-226-0879 or raluca(at)boulder.swri.edu
Julien Salmon, 720-208-7203 or julien(at)boulder.swri.edu
Kelsi Singer, 303-226-5910 or ksinger(at)boulder.swri.edu
Sierra Ferguson, sierra.ferguson(at)swri.org
Rogerio Deienno, rogerio.deienno(at)swri.org
Sam Van Kooten, 303-226-5909 or svankooten(at)boulder.swri.edu

To be added to the SwRI Boulder Colloquia email list, please contact Kelsi Singer, ksinger(at)boulder.swri.edu

Suggest a New Speaker HERE

Tue Nov 5, 2024
In Room 424 11:00 am Thomas Gomez TBD

Tue Nov 12, 2024
In Room 424 + Webex 11:00 am Jun Du Purdue University How to Model Realistic Lunar Craters?

Tue Dec 3, 2024
In Room 424 + Webex 11:00 am Joe DeMartini University of Maryland TBD

Tue Jan 7, 2025
In Room 424 + Webex 11:00 am Sebastien Charnoz IPGP. Université Paris Cité, France Origin of the first solids in the Solar System by non-equilibrium condensation: making the chondrites families and oxidizing without adding oxygen.

Abstract: Primitive meteorites (chondrites) are composed of an out-of-equilibrium assemblage of components whose precursors may have condensed inside the protoplanetary disk that gave birth to our planets. However, the conditions under which these precursors condensed are unclear as a result of their subsequent alteration by nebular or asteroidal processes. Chondrites are separated into three classes, enstatite (EC), ordinary (OC), and carbonaceous (CC) distinguished by their bulk chemical composition and increasing, but discontinuous, degree of oxidation. The condensation of a solar gas at equilibrium reproduces the mineralogy of some chondritic components, but it is unknown why there are only three distinct classes. Given the dynamic nature of young protoplanetary disks, equilibration is unlikely to have prevailed. Here, we simulate non-equilibrium condensation from a solar gas. We show that condensation at different cooling rates and pressures produces condensates that evolve towards only three mineralogical classes, which, on the basis of the Urey-Craig diagram, correspond to EC, OC and CC. A higher degree of nonequilibrium condensation produces more oxidized and water-rich minerals. Phyllosillicates and magnetites found in CCs, mimicking an oxygen-rich formation environment, can be produced under reducing conditions by direct non-equilibrium condensation, without adding water or oxygen.

Tue Nov 5, 2024 In Room 424	11:00 am	Thomas Gomez		TBD
Tue Nov 12, 2024 In Room 424 + Webex	11:00 am	Jun Du	Purdue University	How to Model Realistic Lunar Craters?
Tue Dec 3, 2024 In Room 424 + Webex	11:00 am	Joe DeMartini	University of Maryland	TBD
Tue Jan 7, 2025 In Room 424 + Webex	11:00 am	Sebastien Charnoz	IPGP. Université Paris Cité, France	Origin of the first solids in the Solar System by non-equilibrium condensation: making the chondrites families and oxidizing without adding oxygen.
	Abstract:	Primitive meteorites (chondrites) are composed of an out-of-equilibrium assemblage of components whose precursors may have condensed inside the protoplanetary disk that gave birth to our planets. However, the conditions under which these precursors condensed are unclear as a result of their subsequent alteration by nebular or asteroidal processes. Chondrites are separated into three classes, enstatite (EC), ordinary (OC), and carbonaceous (CC) distinguished by their bulk chemical composition and increasing, but discontinuous, degree of oxidation. The condensation of a solar gas at equilibrium reproduces the mineralogy of some chondritic components, but it is unknown why there are only three distinct classes. Given the dynamic nature of young protoplanetary disks, equilibration is unlikely to have prevailed. Here, we simulate non-equilibrium condensation from a solar gas. We show that condensation at different cooling rates and pressures produces condensates that evolve towards only three mineralogical classes, which, on the basis of the Urey-Craig diagram, correspond to EC, OC and CC. A higher degree of nonequilibrium condensation produces more oxidized and water-rich minerals. Phyllosillicates and magnetites found in CCs, mimicking an oxygen-rich formation environment, can be produced under reducing conditions by direct non-equilibrium condensation, without adding water or oxygen.