Geology, mineralogy, and isotope (Sr, S) geochemistry of the Likak celestite deposit, SW Iran

Ehya, Farhad; Shakouri, Behnaz; Rafi, Mehrdad

doi:10.1007/s13146-013-0137-6

Cited by 11 publications

(16 citation statements)

References 29 publications

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“…It is possible that the celestine geodes formed as a replacement of such nodules and the sulphate in celestine is derived from in situ dissolution of Ca-sulphate. Anhydrite inclusions in celestine are commonly attributed to these replacement processes, further corroborating the replacement hypothesis (Salter & West, 1965; Wood & Shaw, 1976; Carlson, 1987; Ehya, Shakouri & Rafi, 2013). Euhedral quartz is a common diagenetic mineral in evaporites and Ca-sulphate nodules (Nissenbaum, 1967; Chowns & Elkins, 1974; Tucker, 1976; Friedman & Shukla, 1980; Elorza & Rodriguez-Lazaro, 1984; Chafetz & Zhang, 1998).…”

Section: Discussionsupporting

confidence: 75%

“…The source of Sr in celestine has also been attributed to dissolution of Ca-sulphates in nearby sedimentary formations (Carlson, 1987; Matsubara, Kato & Hashimoto, 1992) and leaching of Sr from other rocks by groundwater (Wood & Shaw, 1976; Scholle, Stemmerik & Harpøth, 1990; Ehya, Shakouri & Rafi, 2013). Both the Ardon Formation and the underlying Mohilla Formation host abundant Ca-sulphates, which could undergo dissolution and transport by percolating meteoric water.…”

Section: Discussionmentioning

confidence: 99%

“…1990; Scholle, Stemmerik & Harpøth, 1990; Yan & Carlson, 2003; de Haller et al . 2011; Ehya, Shakouri & Rafi, 2013), sometimes by as much as 20‰. This disparity is sometimes explained by enrichment of the heavier isotope due to sulphate reduction (although no solid evidence is provided for such processes) and, in other cases, it remains unaccounted for.…”

Section: Discussionmentioning

confidence: 99%

“…In the Ardon geodes the difference is only 3‰, so this issue is less pronounced. There is an absence of experimental studies on sulphur isotope fractionation during celestine precipitation (as particularly stressed by Ehya, Shakouri & Rafi, 2013), but a similar study on gypsum precipitation has shown that its δ 34 S value is higher by c. 1.6‰ relative to sulphate remaining in solution (Raab & Spiro, 1991). Likewise, it is possible that the 3‰ measured difference of δ 34 S between celestine and the precursor gypsum is due to either Rayleigh-type fractionation or a higher fractionation factor.…”

Section: Discussionmentioning

confidence: 99%

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

et al. 2013

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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.

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Section: Discussionsupporting

confidence: 75%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

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

et al. 2013

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“…This feature confirms that celestite replaced the host rock lithologies (limestone, gypsum), and it was followed by massive celestite precipitation. The host rock dissolution could be realized during atmospheric condition driven by uplifting of the carbonate platform in the late diagenesis and/or deep brines entered into underlying sediments, and they leached considerable amounts of strontium from host sediments Once these Sr-enriched fluids discharged backup into overlying beds containing gypsum and carbonate material (Tekin et al 2001;Ehya et al 2013), and formed both replacive and cementing celestite in the host rock (Fig. 9).…”

Section: Discussionmentioning

confidence: 99%

Cretaceous-Tertiary (K-T) boundary evaporites in the Malatya Basin, eastern Turkey

Ayyıldız

Varol

Önal

et al. 2015

Carbonates Evaporites

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The Malatya basin is situated on the AnatolidTorid plate of the Neo-Tethys Sea. Evaporites were deposited in the northwestern part of the Malatya basin, which is referred to as the Hekimhan sub-basin. Although the Gün-düzbey sub-basin in the southeastern Malatya basin has coeval deposits, it contains no evaporate deposits. The evaporite is most likely the result of the last transgressiveregressive cycle of the Late Cretaceous Sea. The pre-evaporitic unit is represented by the carbonate platform deposit of the Loftusia banks, which partly underwent dolomitization and overlies the deep marine sediments. Celestite-bearing algal limestone was deposited directly below the gypsumdominated evaporate unit in association with the organicrich mudstone. Evaporite sedimentation took place in various types of environments, such as marginal shallow subaqueous with the association of sabkha-coastal lagoon and deeper subaqueous. It is assumed that the tectonic evolution of the basin margin, which occurred during the latest stage of the Cretaceous regression, was responsible for the environmental restriction leading to evaporate sedimentation under arid/semiarid climatic conditions. The 87 Sr/ 86 Sr ratios obtained from 38 samples of the gypsum and celestitebearing limestones (11 samples) range between 0.707817 and 0.707980 and between 0.707783 and 0.707864, respectively. The d 34 S values range from ?19.5 to ?22.4 %, and the d 18 O values range from ?9.6 to ?12.7 %. These isotopic signatures correspond to that of Late Cretaceous/ Early Paleocene (Cretaceous-Tertiary boundary) marine water. However, celestite exhibit(s) relatively higher d 34 S and 87 Sr/ 86 Sr values than expected marine values, which could be a result of contribution of diagenetic fluid into the celestite-precipitated environment.

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The occurrence and origin of celestite in the Abolfares region, Iran: Implications for Sr-mineralization in Zagros fold belt (ZFB)

Pourkaseb

Zarasvandi

Rezaei

et al. 2017

Journal of African Earth Sciences

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Geology, mineralogy, and isotope (Sr, S) geochemistry of the Likak celestite deposit, SW Iran

Cited by 11 publications

References 29 publications

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

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

Cretaceous-Tertiary (K-T) boundary evaporites in the Malatya Basin, eastern Turkey

The occurrence and origin of celestite in the Abolfares region, Iran: Implications for Sr-mineralization in Zagros fold belt (ZFB)

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