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Interaction of the lithospheric mantle and crustal melts for the generation of the Horoz Pluton (Nigde, Turkey): whole-rock geochemical and Sr-Nd-Pb isotopic evidence/Litosfaarilise vahevoo ja maakooretekkega magmade suhted Horozi intrusiooni (Turgi) tekkes kivimi geokeemiliste ning Sr-Nd-Pb isotoopgeoloogiliste andmete alusel.

INTRODUCTION

Mafic microgranular enclaves (MMEs) are common in metaluminous to peraluminous granitoid plutons (Cantagrel et al. 1984; Bacon 1986; Didier & Barbarin 1991), and are also abundant in most of the Alpine granitoids of Turkey (e.g. Kocak 1993, 2006, 2008; Cevikbas et al. 1995; Kadioglu & Guleg 1996; Arslan & Aslan 2006; Aydogan et al. 2008; Kaygusuz & Aydincaktr 2009; Kocak et al. 2011). They contain mafic mineral assemblages, are relatively fine-grained and have general ellipsoidal shape with unique microstructures commonly interpreted as being igneous as reported in many petrological papers (e.g. Didier 1973; Vernon 1984, 1990; Frost & Mahood 1987; Bedard 1990; Dodge & Kistler 1990; Srogi & Lutz 1990; Poli & Tommasini 1991; Barbarin & Didier 1992; Silva et al. 2000; Waight et al. 2001; Barbarin 2005).

Mafic microgranular enclaves provide significant information on the nature of source rocks, the genesis of granitic magma (Pin et al. 1990; Didier & Barbarin 1991; Barbarin & Didier 1992; Anderson et al. 1998; Waight et al. 2001), the coexistence of two contrasting magma types (Dorais et al. 1990; Vernon 1990), the rheology of host magmas and the tectonic environments of granitoid rocks, as well as on the interaction between the continental crust and the mantle (Didier et al. 1982). Therefore, their origin is of essential significance in interpreting the history of plutons. The Horoz pluton (HP) is a typical example of bimodal magmatism on the northern margin of the Tauride belt. We present detailed whole-rock chemical and Sr-Nd-Pb isotopic data of the MMEs and host granitoids from the HP, and use these data to constrain in granitic plutonism.

GEOLOGICAL SETTING

Turkey is an essential east-west trending constituent of the Alpine-Himalayan orogenic system and contains several continental and oceanic fragments assembled due to the closure of different Tethyan oceanic basins during the Late Cretaceous-Early Tertiary period (Fig. 1a). One of these basins in southern Turkey, namely the Inner Tauride Ocean (Gorur et al. 1984; Dilek et al. 1999; Ozer et al. 2004), was formed between the Central Anatolian Crystalline Complex (CACC) and the Tauride carbonate platform. The CACC is the largest metamorphic block exposed in Turkey and consists of Upper Palaeozoic (Kocak 1993; Kocak & Leake 1994) interlay ered metacarbonate and metapelitic rocks. The ocean was then consumed as a result of north-dipping subduction and closed during the latest Cretaceous to early Cenozoic times (Parlak et al. 2013a), as evidenced by the existence of discontinuous exposures of the Cenomanian-Turonian suprasubduction zone ophiolites (i.e. Alihoca, Aladag) and melanges by latest Cretaceous time (Clark & Robertson 2002) along the Inner-Tauride Suture Zone (Fig. 1a, b). Though the ophiolitic exposures along the suture zone are covered by the Ulukisla Basin strata, the existence of high positive magnetic anomalies corresponding to the Inner-Tauride Suture Zone (Kaynak & Akgakaya 2006) also supports the development of the Inner Tauride Ocean and associated oceanic lithosphere through the late Mesozoic and thus the derivation of the Tauride ophiolites from this oceanic root. The collision of Tauride and CACC continental blocks during the Palaeocene led to the southward transport of the already-emplaced ophiolites and melanges and flysch formation together with folding.

[FIGURE 1 OMITTED]

The NE-SW trending HP is situated in the eastern part of the Bolkar Mountains as a part of the Tauride Platform (Fig. 1b). The pluton formed nearby the Inner-Tauride Suture Zone and intruded into the Bolkar Mountain units, which include variably metamorphosed, Upper Permian-Upper Triassic platform carbonates with siliciclastic intercalations. The HP contains granite and granodiorite members (Fig. 2) and has sharp and discordant contacts, with hornfels formation, which suggests a shallow-crustal emplacement depth. The HP is intruded by two types of mafic dykes with sharp contacts: (i) the blackish-coloured dyke closely associated with granitoids and dismembered in places, forming smaller angular enclaves and (ii) the greenish-coloured dyke forming relatively alteration-resistant, higher topographic levels in the northwestern part of the study area. It contains also some small felsic enclaves and has sharp contacts with their granitoid host rocks, representing possibly the youngest magmatic unit in the pluton. The HP was intruded into the Upper Cretaceous Alihoca ophiolites, which include ultrabasic rocks, volcano-sedimentary rocks, volcanic rocks, diabases, spilite and glaucophane-bearing schists. In comparison with the felsic granite, the granodiorite is relatively coarse-grained, less fractured/altered and has more enclaves. Based on the existence of pebbles of the Horoz granitoid (Alan et al. 2007) in the Middle Eocene clastic rocks of the Ulukisla-Camardi basin, the age of the Horoz granitoid is constrained as the Palaeocene-early Eocene. Geochronological studies suggest a crystallization age between 49 and 56 Ma by U-Pb zircon dating (Kadioglu & Dilek 2010; Kuscu et al. 2010; Parlak et al. 2013b) and [sup.40]Ar-[sup.39]Ar dating (Kuscu et al. 2010). The HP was unroofed due to crustal uplift and erosion throughout the Palaeogene by 23.6 [+ or -] 1.2 Ma (Dilek et al. 1997). However, a recent study (Whitney et al. 2015) suggests that the Horoz granitoid records two main pulses of cooling: (1) an initial stage at ~38-31 Ma, possibly linked with a regional event that is recorded in other crystalline rocks in Central Anatolia and (2) a later stage that may correspond to at least ~2 km of erosion-related exhumation associated with late Miocene uplift of the southern margin of the Central Anatolian Plateau.

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Rounded MMEs in the pluton have usually fine-grained margins and different sizes, from several centimetres up to metres. The geometry of the enclave-host contact varies from sharp/crenulate to diffuse/veined. The contact also varies from lobate to cuspate (Fig. 3a, b). The MMEs in the dioritic dykes may include a 'double enclave' structure where they partially or fully contain smaller, finer-grained, more mafic enclaves. The MMEs sometimes show core-tail structures, in which the tail displays an S-shaped bend, suggesting that they were at least partly plastic when introduced into the felsic magma.

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PETROGRAPHY

The host rocks and their enclaves are usually equigranular and holocrystalline, but porphyritic texture also exists in the enclaves. The main constituents in the granitoids are plagioclase ([An.sub.17-55]), quartz, biotite (mostly eastonitic), orthoclase and amphibole (magnesio-hornblende and edenite), with accessory acicular apatite and zircon in a hipidiomorphic granular texture (Kocak et al. 2011). The MMEs have similar mineralogy with their host. Major components are plagioclase ([An.sub.18-64], 75-85%), amphibole (5-15%), biotite (5-10%), orthoclase (0-5%) and minor quartz, titanite and acicular and stubby prismatic apatite. The texture is mostly equigranular and fine-grained, but sometimes porphyritic and poikilitic. The greenish dyke is predominantly made up of plagioclase, hornblende, chlorite and minor quartz in a holocrystalline porphyritic texture.

ANALYTICAL METHODS

Whole-rock major and trace element analyses of 29 samples were performed at Acme Lab. Ltd. (Vancouver, Canada). Major oxide and trace element compositions were determined by the inductively coupled plasma emission spectrometer from pulps after 0.2 g rock powder was fused with 1.5 g LiB[O.sub.2] and then dissolved in 100 [mm.sup.3] 5% HN[O.sub.3]. Rare earth elements (REEs) were analysed by inductively coupled plasma mass spectrometry from pulps after 0.25 g rock powder was dissolved with four acid digestions. Analytical uncertainties vary from 0.1% to 0.04% for major elements, from 0.1% to 0.5% for trace elements and from 0.01 to 0.5 ppm for REEs.

Sr, Nd and Pb isotope compositions were determined using a Finnigan Mat 262 mass spectrometer at the GEOMAR research centre (Kiel, Germany). Replicate analyses of Sr-Nd-Pb isotopes on the same samples at GEOMAR were within the analytical uncertainties. Sr was measured in static mode and [sup.87]Sr/[sup.86]Sr normalized withinrun to [sup.86]Sr/88Sr = 0.1194. NBS 987 gave an [sup.87]Sr/[sup.86]Sr ratio of 0.710240[+ or -]0.000008. The acid washed samples were boiled in 6N HCL for 1 h. The [sup.143]Nd/[sup.144]Nd ratio was normalized within-run to [sup.146]Nd/[sup.144]Nd = 0.7219 and measured in static mode where the Nd standard La Jolla yielded an average ratio of [sup.143]Nd/[sup.144]Nd = 0.51196276. All Pb isotope analyses were corrected to NBS 981 (Todt et al. 1996) for fractionation. Sample reproducibility is estimated at [+ or -] 0.02, [+ or -] 0.015 and [+ or -] 0.03 (2c) for [sup.206]Pb/[sup.204]Pb, [sup.207]Pb/[sup.204]Pb and [sup.208]Pb/[sup.204]Pb ratios, respectively.

RESULTS

Whole-rock geochemistry

The whole-rock chemical compositions of representative samples from HP host rocks and their MMEs are listed in Table 1.

The granitic rock samples of the HP plot mostly in the granite, monzogranite (adamellite) and granodiorite fields with minor tonalite, whereas samples of MMEs primarily plot in the fields of quartz monzodiorite/ monzogabbro, quartz diorite/gabbro (Fig. 4a) with minor quartz monzogabbro/monzodiorite. The chemical compositions of the greenish dyke in the HP are similar to MME, and samples of these dykes plot in the quartz monzodiorite/monzogabbro and quartz diorite/gabbro fields. In the A/NK versus A/CNK diagram (Fig. 4b), most of the samples from the HP rocks and MMEs plotted in the metaluminous field, only a few Horoz host rocks are found in the peraluminous field. All HP samples show in the high-K calc-alkaline features in the [K.sub.2]O versus Si[O.sub.2] diagram (Fig. 4c). Besides, the granite member of the HP displays a slightly more potassic character by plotting within the shoshonite field.

[FIGURE 4 OMITTED]

In comparison with the MMEs and their host rocks, the greenish dyke samples show more enrichment in MgO, Cr, Co, Pb, Sr, Ba, La and more depletion in [Na.sub.2]O, Nb, Ta, Yb and Lu. With increasing Si[O.sub.2] (Fig. 5), a negative correlation exists in CaO, MgO, FeOt, Ti[O.sub.2] and [P.sub.2][O.sub.5] (not shown). However, the samples are scattered in Si[O.sub.2] versus trace element diagrams (Fig. 5).

The primitive mantle-normalized trace element diagrams show consistent patterns for the HP and its MMEs (Fig. 6). The dyke samples differ from the MMEs and their host in having positive Pb anomaly and no Eu anomalies. Both the host rocks and MMEs have usual consistent patterns, with well-developed negative Ba, Nb, Ti and P anomalies. Chondrite-normalized REE patterns of all rocks are light REEs (LREEs) enriched relative to heavy REEs (HREEs). The [(La/Yb).sub.N] values of all rocks are in the same range, indicating similar sources. However, the patterns are relatively fractionated due to the fractionation of hornblende and/or feldspar phases. The REE patterns of the granitic rocks [[(La/Yb).sub.N] 8.2-18] are slightly concave-upward, suggesting amphibole fractionation (Fig. 7a, b). They have negligible Eu anomalies, but a few samples display significant negative Eu anomalies (e.g. Eu/[Eu.sup.*] = 0.71). The MMEs are less fractionated [[(La/Yb).sub.N] 1.7-12.7] than the granitic rocks.

[FIGURE 5 OMITTED]

[FIGURE 6 OMITTED]

Sr-Nd-Pb isotopes

Host rocks have a low and variable initial [sup.87]Sr/[sup.86]Sr ratio (0.7047) and negative epsilon values (Fig. 8a). A range of initial ratios (0.7046-0.7058) for the MMEs was obtained by calculating the measured ratios for the inferred emplacement age (50 Ma). In general, the MMEs have an initial [sup.87]Sr/[sup.86]Sr ratio and Nd isotope ratios similar to those of their hosts. Host rocks and their MMEs have Nd model ages relative to a depleted mantle reservoir ([T.sub.DM]) of 0.74-0.84 and 0.75-1.38 Ga, respectively.

[FIGURE 7 OMITTED]

The [sup.206]Pb/[sup.204]Pb ratios are between 19.333 and 19.362 in host rocks and between 19.691 and 19.829 in the enclaves. In the Pb-isotope ratios (Fig. 8b) diagram, although MME seems to plot in the mid-ocean ridge basalt (MORB) field, those samples are also at the Northern Hemisphere Reference Line (NHRL), indicating that the subduction-related component was dominated by the material contributed by aqueous fluids rather than by sediments. The MMEs are found on the area of Pacific MORB, while host rocks plot into the field of oceanic sediments and at the boundary of enriched mantled-II.

[FIGURE 8 OMITTED]

DISCUSSION

Source characteristics and origin of the MMEs and dykes

The MMEs and dykes show low Ni (4-14 ppm and 4753 ppm, respectively) and Cr (mostly < 30 ppm and 190-200 ppm) values, which are lower than the Ni-Cr concentrations (Ni = 250-300 ppm, Cr = 500-600 ppm) expected for a primitive basaltic magma derived from a mantle peridotite source (e.g. Wilson 1989). All these features suggest that the studied MME and dyke magmas could have undergone fractional crystallization (Taylor & McLennan 1985) and/or crustal contamination. In the MME samples, Si[O.sub.2] shows a negative correlation with MgO, FeOt, CaO and Ti[O.sub.2], suggesting crystal fractionation of hornblende ([+ or -]pyroxene) and Fe-Ti oxide (Fig. 5).

The MMEs and dykes have relatively low Si[O.sub.2] contents (54-63% and 55-57%) and intermediate to high molar Mg# (34-56 and 56-58), which is inconsistent with the partial melting of the mafic lower crustal rocks and requires a mantle-derived component. The Nb/Ta ratio is a good indicator of pressure, and the ratio decreases as pressure increases (Azizi et al. 2015). Accordingly, the Nb/Ta and Zr/Sm ratios of the MMEs and dyke samples can also be used to discriminate their formation under eclogite-facies or amphibolite-facies conditions (Hoffmann et al. 2011). The fairly low Nb/Ta (10-20) and Zr/Sm (11-51) ratios for the MME rocks from the HP suggest that they formed under garnet amphibolite-facies rather than under eclogite-facies conditions.

Most of the samples with no Eu anomalies accompanied by positive Sr anomalies (Fig. 6b) could reflect melting at pressures above the plagioclase stability field (>15 kbar, >~55 km) or plagioclase accumulation. The high Sr abundances (389-1149 and 892-909 ppm, respectively) in the MMEs and dykes also support this suggestion. However, the samples have high Y (23-76 and 21-22 ppm) and correspondingly low Sr/Y (9-24 and 41-42 ppm), which indicates that plagioclase was possibly in the residue. Unfractionated HREE (and Y) patterns generally suggest that the mafic magma was possibly produced outside the garnet stability field (i.e. plagioclase stable without garnet; Drummond & Defant 1990; Rapp et al. 1991; Springer & Seck 1997; Martin 1999; Pe-Piper et al. 2002). But, garnet as a residual mineral would be able to produce (Gd/Yb)N ratios > 1 (e.g. Martin 1999; Klein et al. 2000; Martin et al. 2005). Therefore garnet may exist in the source of the mafic rocks. Accordingly, the experimental melting of metabasalts under fluid-absent conditions (Rapp et al. 1991; Rapp & Watson 1995) indicates that pressures >0.8 GPa are required to stabilize garnet, and [greater than or equal to] 1.2 GPa for garnet throughly replaces plagioclase. Alternatively, most of the mafic rocks may have been derived from sources located at depths between 30 and 44 km by assuming 1 kbar = 3.7 km for the continental crust (Tulloch & Challis 2000). The amphiboles from the enclaves yield a maximum pressure of 4.1 [+ or -] 0.6 kbar at 730 [degrees]C (Kocak et al. 2011), suggesting the crystallization of the mafic magma at least at 15 km.

The existence of the greenish-coloured dyke resembling enclaves in adjacent granitoids in the HP may suggest that the magma of the MMEs can exist either independently of, or as a separate layer in, their host granitoid magma bodies. In general, the dykes exhibit a similar pattern to that of the host rocks, with a high [(La/Lu).sub.N] ratio (10.4-11.3). In comparison with the scattered smaller MMEs, the dykes seem to be less differentiated (more enrichment in MgO, Cr, Co), but more enriched in Pb, Sr, Ba and LREEs. This may indicate either distinct parental magmas, or different mechanisms or degrees of interaction of the mafic magma with the partially crystallized host-granite, or both. Along with their identical occurrences with the MMEs, this precludes that the dykes correspond to several pulses of mafic magmas. The higher content of large ion lithophile elements (LILEs) and LREEs in the dykes could suggest stronger interactions with the granites, diffusion of water and alkalis, etc. A pronounced negative Nb, P, Ti anomaly (Fig. 6b) may also support this suggestion.

Magma mixing versus restites or autoliths

Based on their mafic composition, the MMEs could have a cumulate or autolith origin (e.g. Noyes et al. 1983; Chappell et al. 1987; Clemens & Wall 1988; Shellnutt et al. 2010; Dahlquist 2002; Donaire et al. 2005), which ignores the grain size differences between the MMEs and host granitoids. Some major and trace elements, such as [Al.sub.2][O.sub.3], [Na.sub.2]O, Rb, Ba, Sr and Zr (Fig. 5) exhibit nonlinear variations. Among these, Si[O.sub.2] versus Ba and Sr (Fig. 5) is of particular interest, in which Ba and Rb contents change significantly for little change in Si[O.sub.2] in the MMEs. Dispersion on the diagrams is of paramount evidence of biotite 'cumulus'. The small amount of biotite may induce an increase in Ba and Rb contents in mafic samples due to their high partition coefficients (KD) for Ba (6.36, Philpotts & Schnetzler 1970) and for Rb (3.53, Matsui et al. 1977). Plagioclase and K-feldspar have low KD for Ba (0.36, Lopez-Ruiz & Cebria 1990) and for Rb (0.07-0.76, Icenhower & London 1996), respectively, therefore they are unlikely to cause this enrichment. However, the MMEs are fine-grained, 10 to 20 times smaller in comparison with the same phases in the host granitoid and have low Ni and Cr, which suggests that the enclaves as a whole cannot be a cumulate of the pluton itself. It is also remarkable that all the enclaves and host rocks have similar total REE concentrations and sub-parallel REE patterns, which are inconsistent with the autolith model. The presence of MMEs in the granitoids could also be indicative of the evolution of the HP through the restite unmixing mechanism (Chappell et al. 1987; Chen et al. 1989; Chappell & White 1992; Chappell 1996; White et al. 1999). The field characteristics of the MMEs, and lack of linear trends for [K.sub.2]O (Fig. 4c), Ba, La, Zr with Si[O.sub.2] (Fig. 5) exclude restite origin. Therefore, the MMEs in the studied HP could have developed mostly by mingling/mixing between near-contemporaneous mafic and felsic magmas (e.g. Vernon 1984; Wiebe et al. 1997; Barbarin 2005; Hawkesworth & Kemp 2006; Kocak 2006; Feeley et al. 2008; Chen et al. 2009; Kocak et al. 2011; Liu et al. 2013).

The magma mixing process could take place before or after the injection of the enclave-forming magma into the felsic host magma. Since the MME samples are mostly non-porphyritic, fine-grained and enclosed in another enclave, the mixing process probably happened prior to the injection of the enclave-forming magma. Furthermore, the mafic enclaves are characterized by relatively low Mg, Ni and Co, suggesting that they were much evolved before their injection into the host felsic magmas. This implies that significant fractionation of hornblende ([+ or -] pyroxene) had occurred before and during the process of crustal contamination/magma mixing at depth. The MMEs are characteristically enriched in P, Ti, Y, Nb, and HREEs, possibly due to selective inter-diffusion of these elements into the less polymerized magmas. These elements were consequently concentrated in apatite, titanite and hornblendes due to their high Kd for these elements (Lopez-Ruiz & Cebria 1990; Klein et al. 1997), keeping their low activity in the melt. Such low activity in the mafic melt gives rise to the continuity of 'Uphill' diffusion, as described for K due to crystallization of biotite by Johnston & Wyllie (1988). Selective diffusion of these elements may be attributed to the crystallization of biotite as cumulate. The Ba depletion in most enclaves could be connected to the complicated feldspar transfer processes at the contact with host magmas and somewhat to the dilution effect induced by the inward migration of Si and alkalis as suggested by some researchers (Bussy 1991; Debon 1991; Orsini et al. 1991).

In general, MME samples have higher [[epsilon].sub.Nd] than their hosts (Fig. 8a, Table 2), suggesting isotopic equilibration between mafic and felsic magmas, which is usually more easily achieved than chemical equilibration since isotopic exchanges proceed more quickly than chemical exchanges (Lesher 1990). The MMEs have generally [sup.87]Sr/[sup.86]Sr values close to or in the range of that for the respective host granite, suggesting a granite-enclave interaction (Fourcade & Javoy 1991). The MMEs and host rocks have distinct [sup.206]Pb/[sup.204]Pb, but similar [sup.208]Pb/[sup.204]Pb values (Fig. 8b). Small variations in the amount and composition of Pb contributed to the mafic melt by the relatively elevated [sup.206]Pb/[sup.204]Pb of zircon compared to [sup.208]Pb/[sup.204]Pb would result in large relative changes in [sup.206]Pb/[sup.204]Pb with only small changes in [sup.208]Pb/[sup.204]Pb.

Source characteristics and genesis of the host granitic rocks

The host granitic rocks are characterized by pronounced negative Nb, Ba, P and Ti anomalies but are enriched in Rb, Th and K. These features are in accordance with those of typical crustal melts, e.g., Himalayan granites (Harris et al. 1986) and granitoids of the Lachlan Fold belt (Chappell & White 1992), and the subduction component. However, the host rocks have relatively low [Sr.sub.(t)] (0.7067) and high eNdW values (-0.2 to 1.8) (Table 2, Fig. 8a), suggesting mantle material involved in the generation of the HP. Similarly, the MMEs in general, have an initial [sup.87]Sr/[sup.86]Sr ratio and Nd isotope ratios similar to those of their hosts, suggesting significant input of a lithospheric mantle-derived component during magma generation. The granitoids show high-K-shoshonitic and I-type characteristics with a wide range of silica content (SiO2 = 64-74 wt%), relatively low-intermediate Mg# (22-41) and low Ni content (1.4-10.0 ppm), all of which may indicate that they could be developed from the mixing of the lower crust and mantle-derived magmas (e.g. Barbarin 1999). Hence average Nb/Ta ratios are 17.5 for mantle-derived and 11-12 for crustal-derived magmas (Green 1995), Nb/Ta ratios for the felsic samples vary between 10.05 and 18.12, suggesting crustal- and mantle-derived magmas in the generation of the HP.

Both MMEs and felsic samples show colinear variation in the Harker diagrams, suggesting that the host granites and MMs/dykes are possibly variably differentiated products of the same parent magma which derived from mixing melts of lithospheric mantle and crustal components. Si[O.sub.2] increases with decreasing MgO, Fe[O.sub.t], CaO and Ti[O.sub.2] and [P.sub.2][O.sub.5], suggesting fractionation of hornblende ([+ or -] pyroxene), Fe-Ti oxide and apatite. Amphibole has a high [K.sub.D] for heavy REEs, but even higher for the medium and heavy REEs (such as Dy); therefore, amphibole fractionation can be traced by decreasing Dy/Yb ratios with differentiation (Davidson et al. 2007a, 2007b, 2008). Accordingly, the amphibole fractionation is indicated by concave-upward REE patterns without significant Eu anomalies (see Tepper et al. 1993, Fig. 7a, b). In the host rocks, Zr and [P.sub.2][O.sub.5] show negative correlation with Si[O.sub.2], suggesting zircon and apatite fractionation. Aplitic suites on the HP most probably represent such comagmatic highly differentiated late-stage melts.

The existence of MMEs with mode of occurrence and mineralogical (Kocak et al. 2011) and geochemical characteristics suggest mafic-felsic interaction and mingling (Barbarin & Didier 1992; Barbarin 1999; Ferre & Leake 2001; Kocak 2006) by the injection of hot mafic magma into felsic magma (source mixing). Langmuir et al. (1978) showed that in the ratio-ratio and ratio-element plots, data consistent with mixing lie along a hyperbolic curve for both isotopic and elemental ratios, while a linear array forms when the ratios of the concentrations of the two denominators are the same for all data points. In the samples, these characteristic hyperbolic mixing arrays are observed in plots of [Al.sub.2][O.sub.3]/CaO versus [Na.sub.2]O/[K.sub.2]O, Ti/Ba versus Ti, and a linear trend is observed in a plot of [Al.sub.2][O.sub.3]/CaO versus [Na.sub.2]O/CaO (Fig. 9a-c). Accordingly, mafic (lithospheric mantle) and felsic (crustal component) magma mixing may alter both the elemental and isotopic compositions of magmas prior to the assimilation/fractionation processes.

[FIGURE 9 OMITTED]

It has also been suggested that I-type granites most likely form by the mixing of crustal materials and mantle-derived magmas rather than by the remelting of ancient meta-igneous crustal rocks (Kemp et al. 2007; Li et al. 2009; Zhu et al. 2009; He et al. 2010). Besides, relative heterogeneity of the initial Sr ratios (0.7046-0.7051) in the host rocks could be attributed to a difference in the degree of contamination of magmas with upper crustal materials.

Adakitic versus TTG

Kadioglu & Dilek (2010) suggested that the HP shows chemical characteristics of high-Al adakitic compositions, which could have formed by the partial melting of the hydrated lithospheric mantle and the amphibolitic mafic lower crust that was triggered by delamination-induced asthenospheric upwelling. However, all samples from the HP usually have lower Mg# [(molar 100 x MgO/ (MgO + FeOt)) < 0.41], Ni (~4 ppm) and Cr (~9 ppm) (Fig. 10a), and higher K (~3.6 wt%), Ba (~712 ppm) and Rb (~86 ppm) contents than that of adakites. The samples have also high Sr contents and are found on the TTG area, rather than on the arc one in Fig. 10b.

It is widely accepted that TTG magmas were created by the partial melting of hydrous metabasaltic rocks transformed into garnet-bearing amphibolite or eclogite, under a variety of fluid conditions (Sen & Dunn 1994; Zamora 2000). Experimental studies show that the partial melting of the mafic lower crust could produce metaluminous granitic magmas regardless of the degree of melting (Sen & Dunn 1994; Wolf & Wyllie 1994; Rapp & Watson 1995). High abundances of [Al.sub.2][O.sub.3] ([greater than or equal to] 19 wt%) in an amphibolite-derived liquid are the result of high [H.sub.2]O (water-saturated) and/or high anorthite contents in the mafic protolith source (e.g. fig. 13 in Beard & Lofgren 1991; fig. 9 in Wolf & Wyllie 1994). Nevertheless, host rocks have lower [Al.sub.2][O.sub.3] contents (13.17-16.4 wt%) than the liquids developed during H2O-saturated amphibolite partial melting experiments. Accordingly, granitoids from the HP were possibly formed under fluid-absent/vapour-absent conditions (with the only [H.sub.2]O derived from the breakdown of hydrous minerals) and/or low anorthite contents in the mafic source. Figure 11 shows that the granitoids, particularly granites, could have formed by low-pressure (100-700 MPa), 20-50% dehydration melting of a basaltic/amphibolitic source. Both the mafic rocks and dykes contain high [Al.sub.2][O.sub.3] and plot (Fig. 11) between the fields of 'low water basalt melting' and '1000 Mpa, no-water melting of a basaltic/amphibolitic source', suggesting relatively higher-pressure conditions in comparison with their host rocks during the partial melting event.

[FIGURE 10 OMITTED]

The TTGs require two main mechanisms to account for their petrogenesis: (1) the partial melting of the subducted oceanic crust (i.e. slab melts) in a convergent margin with usually higher Mg# values and Cr and Ni concentrations (e.g. Martin 1986, 1999; Drummond & Defant 1990; Foley et al. 2002; Kamber et al. 2002; Smithies et al. 2003) due to the interaction of the slab-derived melt with the overlying mantle wedge during ascent (Rapp et al. 1999) or (2) the melting of the thickened mafic crust or underplated basalt with low Mg# values and low Cr and Ni concentrations (e.g. Atherton & Petford 1993; Petford & Atherton 1996; Rapp et al. 1999; Smithies 2000; Condie 2005; Smithies et al. 2009). In Fig. 12a, b, samples fall mostly in the field of adakites derived from the partial melting of the thick lower crust and metabasaltic and eclogite fields, rather than in that of adakite rocks derived from the partial melting of the delaminated lower crust. The data for adakites worldwide exhibit that typical slab melts have low Rb/Sr ratios (0.01-0.05); this is in contrast with the wide range of Rb/Sr ratios (0.01-0.4) for the adakitic rocks that developed from the thickened continental lower crust (Huang et al. 2009). Hence, the relatively higher Rb/Sr ratios (0.09-0.3 in host rocks, 0.04-0.16 in MMEs) of the samples from the HP are in accordance with their derivation from the thickened lower continental crust.

[FIGURE 11 OMITTED]

[FIGURE 12 OMITTED]

Tectonic setting

I-type post-collisional granitoids with mantle-crust signature develop in many tectonic settings, such as intracontinental rifting (Vorontsov et al. 2004; Li et al. 2005; Shu et al. 2005), back-arc basins (Hochstaedter et al. 1990; West et al. 2004), island arc (Geist et al. 1995; Qian & Wang 1999), active continental margins (Donnelly & Rogers 1980) and the rifting of the passive margin (Oberc-Dziedzic et al. 2005). All MMEs and greenish dyke have lower Nb/U (average 5.9 and 5.1) than an average continental crust (Nb/U = 8.4; Rudnick & Fountain 1995). Both MMEs and granitic rocks are characterized by pronounced negative Nb anomalies, positive Pb anomalies (Fig. 6) and enrichment in LILEs and LREEs. The negative anomalies in Nb, Ti and P are characteristic of subduction-related magmas, usually thought to have resulted from the relative enrichment of the mantle source by influx of LILEs through slab dehydration (e.g. McCulloch & Gamble 1991). Similarly, the host granite displays spikes in Cs, Rb, K and troughs in Nb and Ti (Fig. 6), which may represent the continental crust developed by the chemical differentiation of arc-derived magmas (Taylor & McLennan 1995). Besides, low La/Th (1.2-5.1) and medium-high Ba/Nb (24-145) are also typical for the rocks formed in relation with the subduction zone (Sun 1980).

[FIGURE 13 OMITTED]

The most mafic compositions in the granite (lowest in Si[O.sub.2], and highest in MgO and Co) have the highest [K.sub.2]O and [Na.sub.2]O contents as well as anomalously high LREE, P, Zr and Th contents and slight negative Eu anomalies, which are characteristic of A-type granites. However, they differ from A-type granites in their unelevated Rb/Sr contents or intermediate-high Ca and Sr contents (Kemp & Hawkesworth 2003) as well as unelevated Zr + Nb + Ce + Y contents (mostly <350 ppm).

In the plot of Y + Nb versus Rb of Pearce et al. (1984), all granitoid samples are clearly found in 'postorogenic granite' (POG) fields (Fig. 13a). In the plot of SiO2 versus Rb/Zr (Harris et al. 1986), the samples are also concentrated in the 'post-collisional' (Post-COLLG) area in Fig. 13b. In the Harris et al. (1986) Hf-Rb/30-Ta*3 triangle (Fig. 13c), the samples straddle mostly the boundary of the volcanic-arc granite (VAG) and L/P-COLLG fields, showing a trend to the L/P-COLLG, which is similar to the other granitoids of the CACC (Goncuoglu et al. 1991; Akiman et al. 1993; Boztug 1998, 2000; Kadioglu et al. 2003, 2006; Isik & Kocak 2005; Boztug et al. 2007).

GEODYNAMIC IMPLICATION

Horoz granitoids have lower radiogenic ([sup.87]Sr/[sup.86]Sr = 0.7045-0.7051) and higher eNd values (-0.085 to -1.75) than granitoids from the CACC ([sup.87]Sr/[sup.86]Sr = 0.7080-0.7096; [[epsilon].sub.Nd] = -4.8, -6.7, Ilbeyli et al. 2004), probably owing to a combination of upper crustal contamination and heterogeneity of the magma source. Large differences in isotopic data of granitoids from the HP and Karamadaz pluton, and granitoids from the CACC may imply that two groups of magma developed in relation with the closure of the Inner Tauride Ocean and the Izmir-Ankara-Erzincan Ocean, respectively (Kocak 2008). The Inner Tauride Ocean started to develop as early as the Jurassic between the CACC to the east and the Taurides to the west, and consumed by an intra-oceanic subduction northwards (Gorur et al. 1998) along the Inner-Tauride Suture Zone during the latest Cretaceous to early Cenozoic times. Parlak et al (2013b) suggest that the HP could have been formed as a result of hard collision (continent-continent collision) after soft collision (collision of the passive margin with the subduction trench and subsequent slab break-off). However, we suggest that the HP was emplaced after the last stage of oceanic subduction, or at a hiatus of the oceanic subduction at ~50 Ma. The pluton then possibly underwent cooling in two main pulses, ~38-31 Ma and late Miocene (Whitney et al. 2015).

CONCLUSIONS

From combined field, geochemical and isotopical studies it has been concluded that the mantle-derived mafic magmas from which the MMEs crystallized were likely mostly formed by mafic-felsic interaction and mingling, or prior to the mixing crystal fractionation of hornblende ([+ or -] pyroxene) and Fe-Ti oxide. The MMEs usually underwent geochemical and Nd-Sr isotopic equilibration with their host granitoids, with resultant K, P, Ti, Y, Nb and HREE enrichments. The greenish dykes are distinct from the MMEs and display stronger interactions with the granites.

The granitoids have both crustal (distinct negative Nb, Ba, P and Ti anomalies but enriched in Rb, Th and K) and lithospheric mantle [low S% (0.7067) and high [[epsilon].sub.Nd(t)] values (-0.2 to 1.8)] geochemical and isotopic signatures. They exhibit geochemical characteristics of TTGs, which were possibly created by the dehydration melting of a basaltic/amphibolitic source in a thickened lower crust. The parental granitic magma underwent the mixing of mantle-derived mafic magma and crustal felsic magma, coupled with fractional crystallization during magma ascent before emplacement. Relative heterogeneity of the initial Sr ratios (0.7046-0.7051) in the granitoids could also indicate contamination of magmas with upper crustal materials.

The HP granitoids differ from granitoids of the CACC in their lower radiogenic ([sup.87]Sr/[sup.86]Sr = 0.7045-0.7051) and higher eNd values (-0.085 to -1.75), in relation with the combination of upper crustal contamination and/or heterogeneity of the magma source.

doi: 10.3176/earth.2016.14

Acknowledgements. This work was financially supported by the Office of Scientific Research (BAP; Project No. 5401041, Selcuk University, Turkey). The authors are grateful to Mehmet Arslan and Alvar Soesoo for their helpful comments and suggestions on the manuscript.

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Kerim Kocak (a) and Veysel Zedef (b)

(a) Department of Geological Engineering, Selcuk University, Campus, 42075 Konya, Turkey; kkocak@yahoo.com

(b) Department of Mining Engineering, Selcuk University, 42070 Konya, Turkey

Received 31 March 2016, accepted 7 July 2016
Table 1. Major (wt%), trace and rare-earth element (ppm) analyses
of the Horoz pluton

Sample                                     Enclave

                         12        15       23      h36      11b

Si[O.sub.2]              56       55.8     56       58.9     57.9
Ti[O.sub.2]               0.72     0.65     0.75     0.37     0.6
[Al.sub.2][O.sub.3]      17.3     18.7     16.9     19.2     18.2
[Fe.sub.2][O.sub.3]t      8.09     6.95     7.06     5.58     6.61
MgO                       3.28     3.25     4.37     1.47     2.66
MnO                       0.18     0.19     0.28     0.1      0.16
CaO                       5.05     4.86     5.89     4.5      4.92
[Na.sub.2]O               5.04     4.98     4.57     4.81     5.49
[K.sub.2]O                1.2      1.5      0.92     2.65     0.98
[P.sub.2][O.sub.5]        0.42     0.25     0.19     0.38     0.25
LOI                       2.5      2.9      3        1.9      2.1
Total                    99.8    100       99.9     99.9     99.9
Ni                        3.7      4.5     14.1      3.2      5.7
Cr                      bdl       20      100      bdl       20
Co                       11       11       19        6       18
Ga                       21       23       20       19       20
Rb                       46       40       40       72       35
Sr                     1149      509      389      807      436
Ba                      222      267      157      373      163
Zr                      124      142       97      120      143
Nb                       24       31       32       30       30
Ta                        2        2        2        3        2
Th                       15        7        9        6       10
U                         5       11        4        3        4
Y                        50       44       44       76       42
La                       79.2     13.1     18.4     15.4     17.2
Ce                      174       36.9     52.4     44.9     51.6
Pr                       20.2      5.22     6.87     6.81     7.07
Nd                       74.7     22       26       33.3     27.6
Sm                       11.1      5.04     5.18     9.36     5.79
Eu                        2.83     1.22     1.85     1.67     1.87
Gd                        7.04     4.9      4.74     9.62     4.75
Tb                        1.34     1.02     0.97     2.06     1.02
Dy                        6.32     5.03     4.98    10.2      4.84
Ho                        1.31     1.13     1.13     2.22     1.07
Er                        4.22     3.89     3.79     6.84     3.71
Tm                        0.66     0.58     0.59     0.99     0.58
Yb                        4.2      4.08     4.24     6.04     3.82
Lu                        0.71     0.71     0.73     0.89     0.65

Sample                                     Enclave

                        13a      17b      18a      21a      24a

Si[O.sub.2]             58.5     59.3     62.8     57.3     58.7
Ti[O.sub.2]              0.61     0.48     0.4      0.63     0.58
[Al.sub.2][O.sub.3]     17.7     17.3     17.5     18.1     17
[Fe.sub.2][O.sub.3]t     7.26     7.38     4.5      6.33     5.43
MgO                      2.25     2.38     1.43     3.17     3.44
MnO                      0.14     0.14     0.09     0.19     0.22
CaO                      4.1      3.54     3.84     5.73     5.25
[Na.sub.2]O              4.68     4.59     4.48     5.3      4.97
[K.sub.2]O               2.77     3.12     3.18     1.03     1.92
[P.sub.2][O.sub.5]       0.22     0.2      0.27     0.19     0.2
LOI                      1.7      1.5      1.5      1.9      2.3
Total                   99.9    100      100       99.9    100
Ni                       4.4      8.2      2.5      5.5      5.3
Cr                      20       30      bdl       10       40
Co                       7        8        6       14       11
Ga                      20       19       18       18       18
Rb                      63       75       68       47       57
Sr                     456      481      592      551      433
Ba                     317      411      376      176      209
Zr                     119      144      197      113      101
Nb                      37       28       21       14       22
Ta                       3        2        2        1        1
Th                      11       13       14        7       10
U                        5        5        5        3        6
Y                       51       41       30       23       31
La                      16.6     17.9     14.3     14.3     21.2
Ce                      55.4     50.5     37.6     35.4     58.4
Pr                       7.79     6.78     4.79     4.12     7.36
Nd                      33       27.1     19.2     16.5     28.4
Sm                       6.8      5.85     3.82     3.06     5.2
Eu                       1.94     1.39     1.01     1.08     1.63
Gd                       5.9      5.23     3.56     2.76     4.3
Tb                       1.24     1.1      0.73     0.59     0.83
Dy                       5.96     5.2      3.64     2.86     4.12
Ho                       1.33     1.13     0.8      0.64     0.85
Er                       4.56     3.59     2.67     2.07     2.74
Tm                       0.69     0.55     0.4      0.31     0.4
Yb                       4.44     3.5      2.78     2.01     2.75
Lu                       0.71     0.58     0.48     0.36     0.45

Sample                 Enclave         Dyke           Granodiorite

                         40a       42       43       45       4b

Si[O.sub.2]             57        55.3     56.8     63.84     67.7
Ti[O.sub.2]              0.58      0.71     0.69     0.39      0.26
[Al.sub.2][O.sub.3]     18.3      17.6     17.4     16.89     14.9
[Fe.sub.2][O.sub.3]t     5.79      5.74     6.96     5.08      4.59
MgO                      2.51      3.93     4.47     1.43      0.67
MnO                      0.17      0.08     0.08     0.04      0.05
CaO                      5.43      5.64     5.36     3.25      1.11
[Na.sub.2]O              4.71      4.22     4.14     4.4       3.45
[K.sub.2]O               2.3       1.89     1.67     3.25      5.85
[P.sub.2][O.sub.5]       0.23      0.25     0.23     0.25      0.23
LOI                      2.9       4.4      2        1.1       1.1
Total                   99.9      95.4     99.8     99.93     99.9
Ni                       5.5      53       47.3     10         5
Cr                     bdl       200      190      bdl        20
Co                      12        18       19        5         4
Ga                      19        17       16       19        15
Rb                      85        57       56       87       120
Sr                     549       909      892      498       580
Ba                     420       629      458      592      2072
Zr                     133       140      141      141       156
Nb                      34        11       11       19.1      14
Ta                       2         1        1        2         1
Th                       9         7        7        6        13
U                        7         2        2        5         4
Y                       49        22       21       23        19
La                      12.5      30.6     26.3     26.8      31
Ce                      38.7      61.3     55.9     55.3      63.2
Pr                       5.85      6.64     6.3      5.76      6.6
Nd                      25.8      24.1     23.8     19.9      22.9
Sm                       6.51      4.11     3.89     3.45      3.76
Eu                       1.43      1.24     1.21     0.9       0.99
Gd                       6.06      3.17     3.28     3         2.83
Tb                       1.28      0.65     0.64     0.63      0.54
Dy                       6.38      2.99     2.88     3.13      2.38
Ho                       1.35      0.64     0.61     0.65      0.5
Er                       4.62      1.99     1.87     2.12      1.62
Tm                       0.68      0.28     0.28     0.28      0.25
Yb                       4.48      1.73     1.8      1.89      1.61
Lu                       0.74      0.29     0.27     0.3       0.28

Sample                                   Granodiorite

                         28       29       30       33      40b

Si[O.sub.2]             66.5     68.2     70.5     65.9     65.7
Ti[O.sub.2]              0.32     0.29     0.25     0.34     0.33
[Al.sub.2][O.sub.3]     16.4     15.4     15.7     15.9     16.3
[Fe.sub.2][O.sub.3]t     3.53     4.13     2.53     4.02     4.03
MgO                      1.23     0.99     0.59     0.94     1.13
MnO                      0.08     0.06     0.04     0.07     0.07
CaO                      3.12     3.1      1.6      3.96     3.78
[Na.sub.2]O              4.47     4.3      4.16     4.27     4.15
[K.sub.2]O               2.52     1.97     3.15     2.37     2.71
[P.sub.2][O.sub.5]       0.16     0.13     0.14     0.17     0.17
LOI                      1.7      1.3      1.4      2.1      1.5
Total                  100       99.9    100      100       99.9
Ni                       4        5        1        3        4
Cr                      20       20      bdl       10       10
Co                       5        5        2        6        6
Ga                      17       16       16       17       16
Rb                      71       49       95       54       67
Sr                     479      479      364      599      585
Ba                     463      428      614      611      594
Zr                     145      158      182      161      174
Nb                      14       14       14       14       15
Ta                       1        1        1        1        1
Th                       6        9       15       10       12
U                        2        4        3        2        4
Y                       18       22       21       29       20
La                      28.7     30       38.3     51.4     31.5
Ce                      60.3     63       77.9    102       65.5
Pr                       6.26     6.76     7.94    10.6      6.95
Nd                      21.3     23.8     27.1     35.7     23.2
Sm                       3.35     3.9      4.25     6.06     3.83
Eu                       0.95     0.93     0.99     1.34     0.96
Gd                       2.47     3        3.17     4.55     2.89
Tb                       0.49     0.61     0.63     0.95     0.57
Dy                       2.23     2.88     2.78     4.47     2.67
Ho                       0.51     0.6      0.61     0.91     0.57
Er                       1.58     1.91     1.95     2.6      1.82
Tm                       0.24     0.29     0.3      0.39     0.28
Yb                       1.58     1.81     2.01     2.31     1.82
Lu                       0.26     0.31     0.35     0.36     0.3

Sample                         Granodiorite            Granite

                         39       44       47       27      10b

Si[O.sub.2]             67.7     68.7     67.9     68.8     71.8
Ti[O.sub.2]              0.31     0.27     0.28     0.27     0.22
[Al.sub.2][O.sub.3]     16.1     15.9     16.3     15.2     14
[Fe.sub.2][O.sub.3]t     4.42     2.91     3.17     3.44     2.46
MgO                      0.75     0.83     0.83     0.86     0.67
MnO                      0.04     0.03     0.04     0.06     0.05
CaO                      2.7      2.78     2.79     1.87     1.34
[Na.sub.2]O              4.26     3.98     4.28     4.28     3.86
[K.sub.2]O               2.1      3.07     3.01     3.83     4.42
[P.sub.2][O.sub.5]       0.16     0.13     0.15     0.11     0.08
LOI                      1.4      1.4      1.1      1.2      1.1
Total                   99.9     99.9     99.9    100      100
Ni                       6        2        2        3.5      1.8
Cr                      20      bdl      bdl       10      bdl
Co                      10        4        3        4        3
Ga                      16       15       16       15       14
Rb                      62       67       71      100      129
Sr                     500      396      471      524      388
Ba                     328      579      557      498      485
Zr                     155      162      168      125      106
Nb                      14       12       12       15       16
Ta                       1        1        1        1        2
Th                       8       10       13       16       21
U                        1        2        4        3        9
Y                       10       17       21       17       17
La                      17.1     22.7     31.2     21.9     24.7
Ce                      38.7     46.7     64.1     46.6     51
Pr                       4.08     4.86     6.61     4.99     5.19
Nd                      14.7     17       22.5     17.6     17
Sm                       2.54     2.81     3.65     2.93     2.53
Eu                       0.8      0.83     0.91     0.78     0.59
Gd                       1.78     2.12     2.82     2.27     1.89
Tb                       0.34     0.44     0.58     0.48     0.4
Dy                       1.56     2.17     2.69     2.2      1.79
Ho                       0.3      0.45     0.57     0.49     0.41
Er                       1.01     1.5      1.9      1.6      1.46
Tm                       0.16     0.23     0.31     0.26     0.25
Yb                       1.04     1.55     1.9      1.8      1.68
Lu                       0.19     0.25     0.34     0.31     0.32

Sample                                Granite

                         1a      21b       3c       4a

Si[O.sub.2]             69.8     73.9     69.7      67.6
Ti[O.sub.2]              0.27     0.15     0.24      0.48
[Al.sub.2][O.sub.3]     14.7     13.3     14.2      13.2
[Fe.sub.2][O.sub.3]t     1.03     2.07     4.07      5.84
MgO                      0.19     0.37     0.83      1.22
MnO                      0.03     0.04     0.04      0.08
CaO                      3.04     1.62     2.09      1.37
[Na.sub.2]O              3.81     3.52     3.69      2.61
[K.sub.2]O               5.11     4.19     3.89      5.85
[P.sub.2][O.sub.5]       0.15     0.11     0.11      0.2
LOI                      1.9      0.8      1.1       1.5
Total                  100      100      100        99.9
Ni                       1.9      1.4      6.7       5.2
Cr                     bdl      bdl       20        10
Co                       1        2        4         8
Ga                      14       13       14        15
Rb                     117      106       85       102
Sr                     552      347      528       473
Ba                     714      380      572      1790
Zr                     152      112      134       234
Nb                      16       11       12        19
Ta                       1        1        1         1
Th                      16       17       14        23
U                        4        2        3         3
Y                       16       16       15        34
La                      19.9     21.2     22.4      70.6
Ce                      51.2     42.2     45       139
Pr                       5.66     4.39     4.73     14
Nd                      18.7     14.9     16.8      47
Sm                       3.12     2.52     2.65      7.24
Eu                       0.71     0.62     0.74      1.39
Gd                       2.31     1.93     1.96      4.99
Tb                       0.45     0.39     0.39      1
Dy                       2.08     1.93     1.85      4.46
Ho                       0.45     0.41     0.38      0.91
Er                       1.4      1.37     1.29      2.91
Tm                       0.23     0.21     0.2       0.41
Yb                       1.54     1.41     1.37      2.63
Lu                       0.26     0.25     0.24      0.44

bdl: Below detection limit

Table 2. Results of the whole-rock Sr, Nd and Pb isotope analyses
of the enclave and hosts

Sample             [sup.87]Rb/   [sup.87]Sr/    [sup.87]Sr/
                   [sup.86]Sr    [sup.86]Sr    [sup.86]Sr(t)

Enclaves     17b     0.4480        0.7050         0.7047
             21a     0.2475        0.7059         0.7058
             13a     0.3691        0.7054         0.7051
             24a     0.3790        0.7054         0.7051
             40a     0.4484        0.7050         0.7047

Granite      21b     0.8855        0.7052         0.7046

Grandorite   40b     0.3295        0.7052         0.7050
             47      0.4370        0.7054         0.7051
             29      0.2951        0.7050         0.7048
             45      0.5085        0.7055         0.7051

Sample             [sup.147]Sm/   [sup.143]Nd/   [[epsilon].sub.Nd(t)]
                   [sup.144]Nd    [sup.144]Nd

Enclaves     17b        --             --                 --
             21a        --             --                 --
             13a     0.12458         0.5126               0.1
             24a      0.1107         0.5126               0.7
             40a     0.15255         0.5126              -0.6

Granite      21b     0.10225         0.5126              -0.2

Grandorite   40b     0.09981         0.5126              -0.2
             47      0.09807         0.5125              -1.8
             29         --             --                 --
             45         --             --                 --

Sample             TDM    [sup.206]Pb/   [sup.207]Pb/   [sup.208]Pb/
                   (Ga)   [sup.204]Pb    [sup.204]Pb    [sup.204]Pb

Enclaves     17b    --         --             --             --
             21a    --         --             --             --
             13a   0.91        --             --             --
             24a   0.75      19.829         15.751         39.543
             40a   1.38      19.691         15.731         39.395

Granite      21b   0.75      19.362         15.718         39.466

Grandorite   40b   0.74      19.333         15.712         39.430
             47    0.84        --             --             --
             29     --         --             --             --
             45     --         --             --             --

Sr/and Nd/isotope initial ratios calculated at 50 Ma. TDM values
calculated using present/day ([sup.147]Sm/[sup.144]Nd)CHUR = 0.1967
and ([sup.143]Nd/ [sup.144]Nd) CHUR = 0.512638.

CHUR: Chondritic Uniform Reservoir.

--, No analyses.
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Author:Kocak, Kerim; Zedef, Veysel
Publication:Estonian Journal of Earth Sciences
Article Type:Report
Geographic Code:7TURK
Date:Sep 1, 2016
Words:12975
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