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The origin of celestine–quartz–calcite geodes associated with a basaltic dyke, Makhtesh Ramon, Israel

Published online by Cambridge University Press:  29 October 2013

MICHAEL ANENBURG ,
OR M. BIALIK ,
YEVGENY VAPNIK ,
HAZEL J. CHAPMAN ,
GILAD ANTLER ,
YARON KATZIR  and
MIKE J. BICKLE
MICHAEL ANENBURG*
Affiliation:
Department of Geological and Environmental Sciences, Ben-Gurion University of the Negev, Beer Sheva, Israel
OR M. BIALIK
Affiliation:
Department of Geological and Environmental Sciences, Ben-Gurion University of the Negev, Beer Sheva, Israel Weizmann Institute of Science, Department of Environmental Sciences and Energy Research, Rehovot, Israel
YEVGENY VAPNIK
Affiliation:
Department of Geological and Environmental Sciences, Ben-Gurion University of the Negev, Beer Sheva, Israel
HAZEL J. CHAPMAN
Affiliation:
Department of Earth Sciences, University of Cambridge, Cambridge, United Kingdom
GILAD ANTLER
Affiliation:
Department of Earth Sciences, University of Cambridge, Cambridge, United Kingdom
YARON KATZIR
Affiliation:
Department of Geological and Environmental Sciences, Ben-Gurion University of the Negev, Beer Sheva, Israel
MIKE J. BICKLE
Affiliation:
Department of Earth Sciences, University of Cambridge, Cambridge, United Kingdom
*
†Author for correspondence: michaela@post.bgu.ac.il
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Abstract

Spectacular celestine geodes occur in a Jurassic peri-evaporitic sequence (Ardon Formation) exposed in Makhtesh Ramon, southern Israel. The geodes are found only in one specific location: adjacent to an intrusive contact with a Lower Cretaceous basaltic dyke. Celestine, well known in sedimentary associations worldwide and considered as a low temperature mineral, may therefore be associated with magmatic-induced hydrothermal activity. Abundant fluid inclusions in celestine provide valuable information on its origin: gas-rich inclusions in celestine interiors homogenized at T≥200°C whereas smaller liquid-rich inclusions record the growth of celestine rims at T≤200°C. Near 0°C melting temperatures of some fluid inclusions and the occurrence of hydrous Ca-sulphate solid crystals in other inclusions indicate that celestine precipitated from variably concentrated Ca-sulphate aqueous solutions of meteoric origin. Celestine crystallized from meteoric water heated by the cooling basaltic dyke at shallow levels (c. 160 m) during a Lower Cretaceous thermal perturbation recorded by regional uplift and magmatism. The 87Sr/86Sr ratio of geode celestine, 0.7074, is similar to that measured in the dolostones of the host Jurassic sequence, but differs markedly from the non-radiogenic ratio of the dyke. Strontium in celestine was derived from dolostones preserving the 87Sr/86Sr of Lower Jurassic seawater, while sulphur (δ34S = 19.9‰) was provided by in situ dissolution of precursor marine gypsum (δ34S = 16.8‰) indicated by relict anhydrite inclusions in celestine. Low-temperature meteoric fluid flow during the Campanian caused alteration of the dyke into secondary clays and alteration of geodal celestine into quartz, calcite and iron oxides.

Keywords

celestinequartzcalcitegeodesalabaster
Type
Original Articles
Information
Geological Magazine , Volume 151 , Issue 5 , September 2014 , pp. 798 - 815
Copyright
Copyright © Cambridge University Press 2013 

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