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Water Transport and the Evolution of CM Parent BodiesMeteorites have amino acids and hydrated minerals which constrain the peak temperature ranges they have experienced. CMs in particular have a narrow range (273‐325K). Bulk fluid motion during hydration constrained to small scales (less than mm). Some asteroids are known to have hydrated minerals on their surfaces. It is presumed these two facts may be related. Problem: hydration only occurs (significantly) with liquid water; melting water only occurs early on in nebula (1‐10 Myrs ANC); in nebula asteroid surface temperature very cold (approximately 150K). Can indigenous alteration produce CMs and/or surface hydration?
Document ID
20140012521
Acquisition Source
Marshall Space Flight Center
Document Type
Presentation
Authors
Coker, Rob (NASA Marshall Space Flight Center Huntsville, AL, United States)
Cohen, Barbara (NASA Marshall Space Flight Center Huntsville, AL, United States)
Date Acquired
September 24, 2014
Publication Date
June 30, 2014
Subject Category
Lunar And Planetary Science And Exploration
Report/Patent Number
M14-3802
Meeting Information
Meeting: Asteroids Comets Meteors (ACM) 2014
Location: Helsinki
Country: Finland
Start Date: June 30, 2014
End Date: July 4, 2014
Sponsors: Helsinki Univ.
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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