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Establishing the liquid phase equilibrium of angrites to constrain their petrogenesis

Tissot, F. L. H. and Collinet, M. and Dauphas, N. and Grove, T. L. (2018) Establishing the liquid phase equilibrium of angrites to constrain their petrogenesis. In: 49th Lunar and Planetary Science Conference, March 19-23, 2018, The Woodlands, TX. https://resolver.caltech.edu/CaltechAUTHORS:20180615-111233078

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Abstract

Angrites are a series of differentiat-ed meteorites, extremely silica undersaturated and with unusally high Ca and Al contents [1]. They are thought to originate from a small planetesimal parent body of ~ 100-200 km in radius ([2-3]), can be either plutonic (i.e., cumulates) or volcanic (often referred to as quenched) in origin, and their old formation ages (4 to 11 Myr after CAIs) have made them prime anchors to tie the relative chronologies inferred from short-lived radionuclides (e.g., Al-Mg, Mn-Cr, Hf-W) to the absolute Pb-Pb clock [4]. They are also the most vola-tile element-depleted meteorites available, displaying a K-depletion of a factor of 110 relative to CIs.


Item Type:Conference or Workshop Item (Paper)
Related URLs:
URLURL TypeDescription
https://www.hou.usra.edu/meetings/lpsc2018/OrganizationConference Website
ORCID:
AuthorORCID
Tissot, F. L. H.0000-0001-6622-2907
Dauphas, N.0000-0002-1330-2038
Additional Information:© 2018 Lunar and Planetary Institute.
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LPI Contribution2083
Record Number:CaltechAUTHORS:20180615-111233078
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20180615-111233078
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:87157
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:15 Jun 2018 18:22
Last Modified:09 Mar 2020 13:18

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