CaltechAUTHORS
  A Caltech Library Service

^(36)Cl-^(36)S Systematics in Curious Marie: A ^(26)Mg-Rich U-Depleted Fine-Grained CAI from Allende

Tang, H. and Liu, M-C. and McKeegan, K. D. and Tissot, F. L. H. and Dauphas, N. (2016) ^(36)Cl-^(36)S Systematics in Curious Marie: A ^(26)Mg-Rich U-Depleted Fine-Grained CAI from Allende. In: 47th Lunar and Planetary Science Conference, March 21-25, 2016, The Woodlands, TX. https://resolver.caltech.edu/CaltechAUTHORS:20180618-102607087

[img] PDF - Published Version
See Usage Policy.

254Kb

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20180618-102607087

Abstract

Chlorine-36 (t_(1/2)=0.3 Myr) decays to either ^(36)Ar (98%, β-) or ^(36)S (1.9%, ε and β+). This radionuclide can be produced either by local irradiation of gas and/or dust of solar composition [1-2] or by stellar nucleosynthesis in AGB stars or Type II supernovae [3]. Evidence for the presence of 36Cl in the early Solar System (ESS) comes from radiogenic excesses of ^(36)Ar [4] and/or ^(36)S [5-9] in secondary phases (e.g., sodalite and wadalite) in ESS materials such as Calcium, Aluminum-rich inclusions (CAIs) and chondrules. Though the presence of ^(36)Cl in the ESS has been demonstrated, the inferred initial ^(36)Cl/^(35)Cl ratios vary a lot (from 1.0×10^(-7) to 2×10^(-5)) from one inclusion to another [5-9]. Interestingly, all secondary phases measured so far lack resolvable ^(26)Mg excesses that could be due to the decay of ^(26)Al (t_(1/2) = 0.7 Myr), implying that ^(36)Cl and ^(26)Al may not have been derived from the same source. Given that ^(26)Al could have come from a stellar source [10] and that secondary phases should have formed late, we are left with either a very high ^(36)Cl/^(35)Cl initial ratio (~ 10^(-2)) in the ESS, or a late (> 3 Myr after CAI formation) irradiation scenario for the production of ^(36)Cl [9]. ^(36)Cl/^(35)Cl ~10^(-2) far exceeds the predictions from any model (stellar nucleosynthesis or irradiation); therefore, a late irradiation scenario producing ^(36)Cl at the observed level is favored. In this framework, ^(36)Cl is produced in the early solar nebula and incorporated into CAIs via aqueous activities, which could also lead to the formation of sodalite.


Item Type:Conference or Workshop Item (Paper)
Related URLs:
URLURL TypeDescription
https://www.hou.usra.edu/meetings/lpsc2016OrganizationConference Website
ORCID:
AuthorORCID
Tissot, F. L. H.0000-0001-6622-2907
Dauphas, N.0000-0002-1330-2038
Additional Information:© 2016 Lunar and Planetary Institute.
Record Number:CaltechAUTHORS:20180618-102607087
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20180618-102607087
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:87187
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:18 Jun 2018 20:39
Last Modified:09 Mar 2020 13:18

Repository Staff Only: item control page