Lithos 114 (2010) 307–326

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Podiform chromitites and mantle peridotites of the Antalya ophiolite, Isparta Angle(SW Turkey): Implications for partial melting and melt–rock interaction in oceanicand subduction-related settings

Şemsettin Caran a,⁎, Hakan Çoban a, Martin F.J. Flower b, Chris J. Ottley c, Kamil Yılmaz a

a Department of Geology, Suleyman Demirel University, Isparta 32600, Turkeyb Department of Earth and Environmental Sciences, University of Illinois at Chicago (UIC, 845 W. Taylor St. (M/C 186)), Chicago, IL 60607-7059, USAc Northern Centre for Isotopic and Elemental Tracing, Department of Earth Sciences, University of Durham, Durham DH1 3LE, UK

⁎ Corresponding author. Tel.: +90 246 2111328; fax:E-mail addresses: sems@mmf.sdu.edu.tr (Ş. Caran), c

(H. Çoban), flower@uic.edu (M.F.J. Flower), c.j.ottley@dkyilmaz@mmf.sdu.edu.tr (K. Yılmaz).

0024-4937/$ – see front matter © 2009 Elsevier B.V. Aldoi:10.1016/j.lithos.2009.09.006

a b s t r a c t

a r t i c l e i n f o

Article history:Received 23 August 2008Accepted 16 September 2009Available online 27 September 2009

Keywords:Podiform chromititeDunite envelopeHarzburgiteSpinel lherzoliteAntalya ophioliteIsparta Angle

The Antalya ophiolites (AO) in SW Turkey comprise remnants from the southern branch of the Neotethyanoceanic basins. The mantle peridotites of the AO include spinel lherzolite, harzburgite, and dunite. Harzburgitesare dominant over spinel lherzolites in the AO, whereas dunites occur exclusively as ‘envelopes’ surroundingchromitite pods hosted by harzburgite. Petrographic and geochemical data from the peridotites show aprogression from fertile to ultra-refractory character, reflected by a progressive decrease in bulk rock contents ofAl2O3, CaO, SiO2, TiO2, Sc, V and Y, modal clinopyroxene, Al2O3 content of pyroxenes, and an increase in maficphaseMg#s and spinel Cr#s (Cr#: 18.0–39.6% in spinel lherzolites, 33.2–77.8% in harzburgites, and 68.7–72.2% indunites). The chondrite-normalized REE patterns of the AO spinel lherzolites have LREE depleted signatureshowing steep slopes fromHREE to LREE, and are compatible with the residue of a low degree (8–18%) of partialmelting of N typeMORmantle. Theirmineral composition,whole-rock chemistry and oxygen fugacities betweenFMQ −1.01 and FMQ −0.57 are consistent with mid-ocean ridge-type mantle. On the other hand, the AOharzburgites have slight enrichment in LREE relative to the patterns expected for residues of partial maltingthereby indicating reaction with a LREE-enriched melt. Thus, their chondrite-normalized REE patternsshow ‘V-shaped’ REE distributions similar to those of forearc harzburgites. The AO harzburgites have oxygenfugacities between FMQ −1.08 and FMQ +0.72. The correlation of spinel Cr# and oxygen fugacity valuesindicates polygenetic association in the AO harzburgites as encountered in modern forearcs (e.g. Izu–Bonin–Mariana and South Sandwich forearc complexes). The spinel Cr# and oxygen fugacity correlation and the LREEenrichment, despite their ultra-refractory character, confirm thenotion that the AOharzburgites couldbe residuefrom interaction of a previously melted mantle source (the AO spinel lherzolites) with an ascending LREE-enrichedmelt in a supra-subduction environment. The interactionmust have causedmodestmelt fractions of thepre-existing mantle lithosphere. Therefore, the harzburgites experienced higher degree partial melting (17 to25%) than the spinel lherzolites. The AO dunites, themost ‘refractory’ of the peridotites, appear to have formed atoxygen fugacities between FMQ+0.72 and FMQ+1.72, and showV-shaped REE distributions similar to those ofsupra-subduction zone (SSZ) dunites. Phase equilibria,field evidence andpetrographic features show that theAOdunites are formed by dissolution of pyroxene from host harzburgites during the melt–mantle interaction.Focused melt flow caused the highest of melt fractions around the reaction zone. The AO podiform chromititescomposed of a very refractory olivine–spinel assemblage (Fo: 94.8 and 96.1 – Cr#: 72.2–81.2%), corroborating aboninitic parentage. Therefore, the chromitites are considered to be the product of boninitic melt evolved bymelt–rock interaction in a supra-subduction environment. Our results support amodel involving bothmelt–rockinteraction and differential partial melting to explain (a) precipitation of podiform chromitite from boniniticmagma and (b) peridotites showing a sequence from MORB-like to subduction-related affinity.

+90 246 2370859.oban@mmf.sdu.edu.trurham.ac.uk (C.J. Ottley),

l rights reserved.

© 2009 Elsevier B.V. All rights reserved.

1. Introduction

Ophiolite complexes are regarded as fragments of oceanic litho-sphere ‘obducted’ onto continental margins, prior to or during anorogeny. However, it is nowaccepted that ophiolitesmay be formed in avariety of tectonic settings, as indicated by characteristic mineralogical,geochemical, and structural attributes (e.g. Pearce, 1980). For example,

308 Ş. Caran et al. / Lithos 114 (2010) 307–326

layered ophiolite sequences including sheeted dikes and showing‘fertile’ (MORB-type) mantle character, Al-rich spinels, and relativelylow oxygen fugacities may suggest a mid-ocean ridge provenance (e.g.Dick and Bullen, 1984; Dilek and Thy, 1998;Morishita et al., 2007; Uysalet al., 2007; Dare et al., 2009), whereas calcalkaline magmatic affinity,refractory mantle character, Cr-rich spinels, and indications of highoxygen fugacity imply subduction-related origins (e.g. Miyashiro, 1973,1975a,b, 1977; Pearce et al., 1981; Pearce et al., 1984; Dick and Bullen,1984; Zhou et al., 1998; Uysal et al., 2007; Dare et al., 2009). Theparadoxical coexistence of both compressional and extensional tectonicsettings — sometimes referred to as the ‘ophiolite conundrum’ (e.g.Moores et al., 2000) bears critically on the problem of a meaningfulclassification of ophiolites, while establishing their petrogenetic andgeodynamic significance. To date, classification schemes have beenmostly restricted to so-called MORB-like- and ‘SSZ’(supra-subductionzone) types (e.g. Pearce et al., 1981, 1984) (equivalent respectively tothe ‘lherzolitic’ and ‘harzburgitic’ types of Nicolas and Boudier, 1991).‘SSZ’ ophiolites have been further subdivided into ‘Tethyan’ and‘Cordilleran’ categories (e.g. Moores, 1982; Beccaluva et al., 2004).

Ophiolite complexes in the Turkish segment of the Alpine-Himalayan orogenic system are of variable age, mostly east-west-oriented and presumably reflect discrete Neotethyan closure events,mostly during the Jurassic and Late Cretaceous (Şengör and Yılmaz,1981; Şengör et al., 1984; Robertson, 2002; Elitok and Drüppel, 2008)(Fig. 1A). Most of these bodies have been designated as ‘SSZ’ types (e.g.Parlak et al., 1996; Yaliniz et al., 1999; Parlak and Delaloye, 1999;Robertson, 2002; Parlak et al., 2002; Parlak et al., 2004; Celik andDelaloye, 2006; Parlak et al., 2009) associated, by implication, with

Fig. 1. A. Distribution of ophiolites, ophiolitic melanges and suture zones in Turkey (modifieAnkara Suture, AES: Ankara-Erzincan Suture, ITS: Inner Tauride Suture, AS: Antalya Suture, SEarea (in Central-Western Taurides) (modified from Alpan et al. (1964), Gutnic et al. (1979)

volcanic arcs, forearcs, and backarc basins. However, it is well knownthat examples of a single ophiolite body may include both MOR- andSSZ-types due to multistage histories of the ophiolite body as mostophiolites (e.g. Dick and Bullen, 1984; Meffre et al., 1996; Portnyaginet al., 1997; Parkinson and Pearce, 1998; Pearce et al., 2000; Hoeck et al.,2002; Flower, 2003; Flower and Dilek, 2003; Saccani and Photiades,2004; Beccaluva et al., 2004). This observation highlights the need for afundamental assessment of exposed all parts of an ophiolite.

Previous studies of the Antalya ophiolite (Fig. 1A) have focusedmostly on its structural and tectonic associations, the geochemistry ofits extrusive rocks, dikes, and plutonic lithologies (Robertson andWoodcock, 1981; Robertson and Waldron, 1990; Celik and Delaloye,2003; Bağcı et al., 2006; Bağcı and Parlak, 2009), magmatic histories(e.g. Juteau, 1975; Reuber, 1984), radiometric andpaleontological ages(Thuizat et al., 1978; Yılmaz, 1984), and the origin of metamorphicsoles (Celik and Delaloye, 2003). In this study, we present acomprehensive data set for bulk rock andmineral phases frommantlelithologies, namely spinel lherzolites, harzburgites, dunite envelopesand chromitites. The data for mantle sequences offer definitiveevidence for establishing the variable affinities of the Antalya ophiolitefragments in termsof hypothetical ocean ridge and subduction-relatedsettings, and a possible analogue to intra-oceanic forearcs.

2. Geological setting

Turkish Neotethyan ophiolites are located on east-west-orientedophiolite belts appearing to mark micro continent collision suturesresulting from discrete Neotethyan basin closure events (Şengör and

d from Alpan et al. (1964) and Robertson (2002)). IPS: Intra Pontid Suture, IAS: Izmir-TS: SE Turkish Suture, MS: Mommonia Suture. B. Simplified geological map of the study, and Poisson et al. (2003)).

Fig. 2. Synthetic logs of the Antalya ophiolites (not to scale). Dismembered but nearlyintact ophiolite sequences. See text for data sources.

309Ş. Caran et al. / Lithos 114 (2010) 307–326

Yılmaz, 1981; Şengör et al., 1984; Robertson, 2002) (Fig. 1A). Thepresent study focuses on the compositional character of mantle phasesfrom ophiolites of the Antalya complex nappe system in the IspartaAngle regionof SWTurkey. TheAntalya complexhas been interpreted as

Table 1Modal % of mineral phases, summary compositional data and oxygen fugacity values for m

Sample Rocktype

Texture Modal ratio of mineral phases% Whole rock

Ol Opx Cpx Cr-sp Amp %LOI Al2O3 wt.%

AN-8 Lhz Porph 77.3 15.2 6.0 1.5 – 0.8 1.33AN-9 Lhz Porph 75.8 15.0 8.0 1.2 – 0.1 1.89AN-13 Lhz Porph 68.4 20.0 9.6 2.0 – 0.4 2.39Kzl-26G Lhz Porph 69.5 23.0 6.0 1.5 – 2.7 1.25AN-3B Hz Porph 85.9 10.5 2.6 1.0 – 0.4 0.67AN-6 Hz Porph 78.8 17.0 2.9 1.3 – 0.6 0.90AN-7B Hz Porph 82.3 14.0 3.0 0.7 – na naAN-21 Hz Porph 82.0 15.0 2.2 0.8 – 2.8 0.60AN-27B Hz Porph 84.5 12.0 2.2 1.3 – 0.3 0.40Kzl-16 Hz Porph 78.0 18.0 3.0 1.0 – 1.2 0.80Kzl-23 Hz Porph 77.7 18.5 2.8 1.0 – 0.3 0.79Kzl-28B Hz Porph 79.2 18.0 1.8 1.0 – 0.9 0.38Kzl-29B Hz Porph 84.0 13.3 1.2 1.0 0.5 0.3 0.21Kzl-32C Hz Porph 76.7 20.0 2.8 0.5 – 2.2 0.55Kzl-1C Du Mesh 99.0 – – 1.0 – 4.5 0.11AN-7U Du Mesh 98.5 – 0.5 1.0 – na naKzl-18 Du Mesh 98.5 – 0.5 1.0 – 7.0 0.14Kzl-26B Du Mesh 98.3 – 0.7 1.0 – 11.2 0.18Kzl-32A Du Mesh 98.0 – – 1.0 1.0 6.8 0.23AN-7C Chr Cum 10.0 – – 90.0 – na naAN-27C Chr Cum 8.0 – – 90.0 2.0 na naKzl-1A Chr Cum 18.0 – – 80.0 2.0 na naKzl-17A Chr Cum 15.0 – – 85.0 – na naKzl-26E Chr Cum 8.0 – – 90.0 2.0 na naKzl-32B Chr Cum 5.0 – – 95.0 – na na

All percentages of mineral phases except serpentine are primary values. LOI: loss-on-igncumulate, Lhz: spinel lherzolite, Hz: harzburgite, Du: dunite, Chr: chromitite, Ol: olivine, Fo:observed, na: not analyzed.

a series of remnants of one of several possible southern branches ofNeotethys, other members of which also include the Troodos ophiolitesin Cyprus, other Tauride ophiolites in southern Turkey (e.g. Mersin,Pozanti-Karsanti, Hatay), and the Bitlis-Zagros ophiolite complex insoutheast Turkey and Iran (Yaliniz et al., 2000; Robertson, 2000). In theAntalya-Turkish sector, the ophiolites are located within a beltextending northward from Çavuşköy-Antalya to Aksu-Isparta(Fig. 1B). In some places, dismembered nearly complete ophiolitesuccessions are exposed especially betweenÇavuşköy andKemer, in thesouth-west part of the Antalya complex (Juteau, 1980; Yılmaz, 1984;Robertson, 2002) (Fig. 1A). Synthetic pseudo-stratigraphies of these arepresented in Fig. 2, and summarized below. From south to north, theyinclude the Çavuşköy (Adrasan) area, comprising harzburgitic mantle,the Tekirova area, where harzburgitic mantle and overlying cumulatesare exposed, and the Kemer area, represented by cumulates, isotropicgabbros, sheeted dikes, minor plagiogranites, and pegmatitic gabbros.To the west of Antalya, the Y.Karaman area contains both spinellherzolites and harzburgites. The AO mantle sequences are cut bynumerous isolated dikes, although no exposures of metamorphic solesor extrusive lithologies are present (Juteau, 1980; Yılmaz, 1984;Robertson, 2002). However, dismembered fragments of the crustalsequence are found in associated ophiolitic mélange lithologies. To thewest, the dismembered Gödene (Altınyaka) zone ophiolites comprisesequences of serpentinized harzburgite, subordinate cumulate andisotropic gabbros, and sheeteddikes, and locally, small (poorly exposed)slices of metamorphic sole (Juteau, 1980; Robertson and Woodcock,1981; Yılmaz, 1984; Celik and Delaloye, 2003). To the northeast, theAksu ophiolite consists of harzburgitic mantle cut by diabase dikeswarms, although ophiolitic crustal sequences are missing. Chromititepods surrounded by dunitic envelopes are commonly present in theharzburgites throughout the whole area.

2.1. Mantle rocks

The apparent thickness of the Antalya ophiolite (AO) peridotitesvaries from about 0.1 to 1 km. The ophiolites have been tectonically

antle peridotites and podiform chromitites from Antalya ophiolites.

Ol Cpx Opx Sp Sp ƒO2 ΔlogFMQ

MgO wt.% Fo % Al2O3 wt.% Al2O3 wt.% Cr# % TiO2 wt.%

41.68 91.1 3.00 3.66 29.2 0.05 −0.9040.27 90.5 4.85 3.87 18.0 0.05 −0.5739.65 90.3 4.40 3.14 19.0 0.07 −1.0140.35 90.4 3.08 2.73 37.8 0.06 −0.7944.24 91.5 2.79 1.96 40.5 0.05 −0.5945.09 91.8 1.53 2.7 39.2 0.06 −0.84na 92.0 2.42 2.74 43.4 0.07 −1.0843.57 91.7 1.16 1.72 59.6 0.05 −0.4943.15 91.7 0.85 0.97 68.2 0.07 −0.3143.86 91. 7 1.58 2.37 47.9 0.06 −0.2043.67 91.2 2.15 2.08 33.3 0.04 −0.4844.07 91.4 1.00 1.14 66.1 0.06 +0.5145.67 91.9 0.52 0.48 77.8 0.06 +0.8942.95 92.3 1.67 1.83 56.4 0.07 −1.0648.35 92.4 – – 72.0 0.11 +0.24na 93.4 0.99 – 68.9 0.17 +0.7249.27 93.6 0.55 – 69.0 0.12 +1.7248.44 92.8 1.07 – 67.7 0.21 +1.6048.85 93.2 – – 71.1 0.18 +1.24na 95.9 – – 71.3 0.12 +0.86na 95.2 – – 71.5 0.12 +0.84na 95.8 – – 72.9 0.14 +0.78na 96.1 – – 76.0 0.19 +1.47na 95.8 – – 78.3 0.10 +1.01na 95.7 – – 72.2 0.17 +0.89

ition. LOI gives the estimated percentage of alteration. Porph: porphyroclastic, Cum:forsterite, Cpx: clinopyroxene, Opx: orthopyroxene, Sp: spinel, Amp: amphibole, –: not

Table 2Whole-rock major, trace and REE element compositions.

Sample AN-8 AN-9 AN-10 AN-13 SAM-24 Kzl26G AN-2 AN-3B AN-5 AN-6 AN-7 AN-21 AN-22 AN-27A AN-27B AN-27Y Kzl-5B Kzl-6 Kzl-12 Kzl-16 Kzl-22

Rock type Spinel lherzolites Harzburgites

SiO2 wt.% 44.90 45.06 45.60 44.77 45.66 46.92 42.61 43.98 43.49 42.58 42.03 44.19 43.32 44.16 45.16 45.37 43.61 43.05 43.32 43.78 42.32AL2O3 1.33 1.89 1.03 2.39 1.27 1.25 0.46 0.67 1.12 0.90 0.54 0.60 0.51 0.49 0.40 0.50 0.27 0.62 0.36 0.80 0.52Fe2O3 9.10 9.10 9.30 8.97 8.77 8.43 9.15 8.46 8.59 8.34 8.12 9.28 8.62 8.77 8.85 8.89 9.47 8.59 8.61 8.94 8.94MgO 41.68 40.27 41.95 39.65 42.01 40.35 45.29 44.24 43.92 45.09 46.80 43.57 44.83 43.73 43.15 42.76 44.63 45.21 45.52 43.86 45.70CaO 1.50 1.94 1.05 2.24 1.33 1.42 0.65 0.63 1.04 0.84 0.47 0.64 0.70 0.66 0.53 0.73 0.34 0.61 0.33 0.96 0.42Na2O 0.01 0.02 0.01 0.04 0.04 0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01K2O <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01TiO2 0.01 0.03 0.01 0.04 0.01 0.01 <0.01 <0.01 0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01P2O5 0.02 0.03 0.03 0.01 0.01 <0.01 0.02 0.01 0.03 0.02 0.03 <0.01 0.03 0.03 0.03 0.20 <0.01 0.02 0.02 0.02 0.02MnO 0.12 0.12 0.12 0.13 0.12 0.12 0.12 0.11 0.12 0.12 0.11 0.12 0.12 0.12 0.12 0.12 0.12 0.11 0.11 0.12 0.11Cr2O3 0.417 0.408 0.433 0.409 0.457 0.467 0.421 0.421 0.412 0.407 0.365 0.415 0.439 0.439 0.447 0.437 0.297 0.385 0.404 0.475 0.392TOTAL 99.37 99.16 99.82 99.24 99.97 99.24 99.16 99.04 99.03 99.06 98.81 99.17 98.87 99.11 99.18 99.14 99.06 98.89 98.99 99.25 98.92LOI 0.8 0.1 0.7 0.4 1.9 2.7 0.1 0.4 0.1 0.6 4.7 2.8 2.9 0.5 0.3 0.1 3.8 5.5 2.0 1.2 6.4Sc (ppm) 12.47 13.88 10.63 14.69 11.97 13.69 9.62 9.01 11.35 10.31 6.90 10.31 10.50 10.93 10.51 11.77 7.81 8.64 7.32 10.56 6.57Ti 129 249 121 357 110 99 53 74 86 74 63 34 21 23 27 18 29 37 26 53 34V 47.12 54.91 37.33 57.31 43.35 51.53 24.72 28.62 39.26 35.21 18.18 32.64 32.79 25.85 26.98 27.77 19.02 30.25 21.74 37.78 20.63Ni 1435 1359 1409 1261 1496 1532 1550 1521 1467 1498 1621 1463 1401 1474 1436 1454 2350 2143 2153 1937 1934Co 111.90 118.40 117.70 106.10 106.60 78.60 81.67 116.40 118.50 114.00 105.10 106.30 107.20 122.50 121.40 137.80 115.20 99.39 102.20 99.11 88.97Cu 14.44 17.44 19.15 17.45 15.53 20.61 3.36 1.90 5.16 10.06 3.41 4.57 8.31 12.63 14.79 15.51 2.05 7.08 2.31 2.22 4.09Zn 10.70 40.18 42.07 36.55 41.85 36.64 47.42 39.99 39.75 39.69 31.98 39.05 37.36 34.72 39.03 34.95 43.65 41.12 43.15 43.41 40.97Ga 1.0860 1.4900 0.7991 1.7170 1.0970 0.9561 0.4205 0.6080 0.8749 0.7073 0.3828 0.5297 0.4125 0.3510 0.3784 0.3601 0.2376 0.5050 0.3303 0.6837 0.4034Rb 0.0073 0.0120 0.0197 0.0152 0.0150 0.0251 0.0192 0.0118 0.0125 0.0118 0.0303 0.0675 0.0355 0.0785 0.0288 0.0181 0.0221 0.0516 0.0123 0.0276 0.0076Sr 0.0655 0.0663 0.1145 0.0828 0.1660 0.1378 0.1150 0.0709 0.0472 0.0551 0.1975 0.0662 0.1290 0.2833 0.1251 0.1210 0.3768 0.0548 0.0889 0.0728 0.0780Y 0.4942 1.0950 0.2825 1.6140 0.5290 0.2528 0.0738 0.1190 0.2592 0.2000 0.1207 0.0527 0.0309 0.0353 0.1469 0.0282 0.3340 0.0623 0.0260 0.1199 0.0577Zr 0.0887 0.1178 0.1044 0.1845 0.0430 0.0901 0.1283 0.3210 0.0981 0.0917 0.1744 0.0956 0.1090 0.1052 0.0946 0.1375 0.0870 0.0871 0.9830 0.0901 0.1176Nb 0.0173 0.0335 0.0230 0.0239 0.0101 0.0197 0.1599 0.0322 0.0363 0.0208 0.0114 0.0096 0.0148 0.0346 0.0377 0.1193 0.0231 0.0147 0.0190 0.0158 0.0083Cs 0.0016 0.0017 0.0023 0.0014 0.0030 0.0023 0.0022 0.0018 0.0019 0.0020 0.0029 0.0099 0.0039 0.0206 0.0034 0.0030 0.0035 0.0044 0.0022 0.0039 0.0011Ba 0.0852 0.0851 0.0881 0.0893 0.1280 0.1390 0.1550 0.0991 0.1092 0.0682 0.2160 0.0781 0.1170 0.2086 0.1179 0.2703 0.9612 0.1472 0.1671 0.1092 0.0941Pb 0.0833 0.1908 0.1615 0.1067 0.1330 0.1893 0.1333 0.1283 0.1351 0.0947 0.0440 0.0413 0.0859 0.2661 0.2461 0.2991 0.135 0.0218 0.0240 0.0208 0.0207Th 0.0015 0.0017 0.0018 0.0016 0.0030 0.0023 0.0037 0.0025 0.0020 0.0022 0.0016 0.0018 0.0020 0.0030 0.0017 0.0023 0.0018 0.0015 0.0023 0.0016 0.0014U 0.0012 0.0013 0.0010 0.0007 0.0010 0.0012 0.0012 0.0011 0.0009 0.0008 0.0009 0.0007 0.0008 0.0020 0.0011 0.0017 0.0008 0.0010 0.0015 0.0009 0.0013La 0.0027 0.0039 0.0029 0.0034 0.0040 0.0028 0.0101 0.0076 0.0050 0.0063 0.0083 0.0041 0.0045 0.0085 0.0031 0.0056 0.0068 0.0036 0.0057 0.0037 0.0032Ce 0.0159 0.0351 0.0096 0.0275 0.0100 0.0130 0.0931 0.0878 0.0586 0.0882 0.0207 0.0347 0.0127 0.0834 0.0107 0.0473 0.0164 0.0118 0.0157 0.0124 0.0156Pr 0.0006 0.0010 0.0007 0.0015 0.0010 0.0007 0.0020 0.0013 0.0009 0.0011 0.0019 0.0008 0.0010 0.0015 0.0008 0.0011 0.0012 0.0008 0.0011 0.0008 0.0007Nd 0.0047 0.0126 0.0061 0.0285 0.0060 0.0054 0.0094 0.0065 0.0046 0.0049 0.0111 0.0040 0.0055 0.0071 0.0039 0.0051 0.0057 0.0043 0.0050 0.0046 0.0043Sm 0.0055 0.0198 0.0051 0.0397 0.0080 0.0053 0.0020 0.0016 0.0012 0.0013 0.0047 0.0007 0.0013 0.0013 0.0009 0.0009 0.0009 0.0009 0.0007 0.0010 0.0017Eu 0.0028 0.0102 0.0023 0.0200 0.0040 0.0025 0.0007 0.0005 0.0005 0.0005 0.0022 0.0002 0.0004 0.0003 0.0004 0.0002 0.0003 0.0003 0.0003 0.0003 0.0008Gd 0.0230 0.0672 0.0150 0.1178 0.0250 0.0190 0.0030 0.0030 0.0057 0.0047 0.0099 0.0010 0.0016 0.0010 0.0018 0.0007 0.0012 0.0014 0.0007 0.0019 0.0040Tb 0.0068 0.0176 0.0041 0.0284 0.0070 0.0055 0.0010 0.0012 0.0025 0.0019 0.0024 0.0005 0.0005 0.0004 0.0006 0.0004 0.0005 0.0006 0.0004 0.0010 0.0012Dy 0.0603 0.1447 0.0338 0.2229 0.0650 0.0453 0.0082 0.0111 0.0256 0.0198 0.0166 0.0041 0.0026 0.0027 0.0047 0.0018 0.0032 0.0054 0.0023 0.0107 0.0076Ho 0.0171 0.0379 0.0096 0.0564 0.0170 0.0133 0.0026 0.0039 0.0085 0.0068 0.0044 0.0017 0.0010 0.0011 0.0016 0.0009 0.0012 0.0022 0.0009 0.0040 0.0021Er 0.0603 0.1227 0.0335 0.1781 0.0590 0.0452 0.0105 0.0167 0.0346 0.0267 0.0140 0.0089 0.0052 0.0061 0.0065 0.0052 0.0055 0.0106 0.0045 0.0199 0.0075Tm 0.0123 0.0235 0.0073 0.0335 0.0110 0.0098 0.0025 0.0041 0.0080 0.0064 0.0029 0.0025 0.0017 0.0019 0.0017 0.0017 0.0016 0.0028 0.0013 0.0048 0.0017Yb 0.0900 0.1590 0.0523 0.2218 0.0850 0.0733 0.0201 0.0334 0.0620 0.0511 0.0219 0.0246 0.0171 0.0191 0.0160 0.0175 0.0144 0.0254 0.0127 0.0400 0.0144Lu 0.0174 0.0289 0.0100 0.0396 0.0160 0.0137 0.0044 0.0073 0.0127 0.0105 0.0044 0.0059 0.0042 0.0047 0.0038 0.0042 0.0035 0.0058 0.0032 0.0086 0.0033Hf 0.0047 0.0118 0.0045 0.0239 0.0040 0.0046 0.0038 0.1734 0.0030 0.0030 0.0072 0.0024 0.0028 0.0027 0.0026 0.0034 0.0024 0.0025 0.0026 0.0025 0.0040Ta 0.0257 0.0578 0.0390 0.0372 0.0090 0.0320 0.0294 0.0324 0.0415 0.0287 0.0112 0.0113 0.0183 0.0571 0.0596 0.0983 0.0219 0.0121 0.0172 0.0209 0.0096

Sample SKzl-23 Kzl-24 Kzl-28B Kzl-29A Kzl-29B Kzl-31A Kzl-32C Kzl-33 Kzl-34A Kzl-1B Kzl-1C Kzl-2A Kzl-11 Kzl-15 S Kzl-15Y Kzl-18 Kzl-20 Kzl-26B Kzl-27B Kzl-32A

Rock type Harzburgites Dunites

Values in wt.% (oxides) and ppm (trace element and REE). The major element data were normalized to anhydrous totals. < below detection limit, LOI: loss-on-ignition.

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Table 2 (continued)

Sample SKzl-23 Kzl-24 Kzl-28B Kzl-29A Kzl-29B Kzl-31A Kzl-32C Kzl-33 Kzl-34A Kzl-1B Kzl-1C Kzl-2A Kzl-11 Kzl-15 S Kzl-15Y Kzl-18 Kzl-20 Kzl-26B Kzl-27B Kzl-32A

Rock type Harzburgites Dunites

SiO2 wt.% 44.45 44.20 44.09 42.81 43.23 44.62 45.01 43.11 45.41 40.32 40.84 40.07 40.52 40.08 39.69 40.57 39.85 40.33 39.99 39.95AL2O3 0.79 0.46 0.38 0.28 0.21 0.67 0.55 0.55 0.47 0.11 0.11 0.12 0.15 0.12 0.13 0.14 0.25 0.18 0.04 0.23Fe2O3 8.58 8.73 9.11 8.91 8.74 8.79 9.07 7.95 8.35 8.20 8.64 8.12 8.67 8.24 8.12 7.66 9.09 8.84 9.76 8.55MgO 43.67 44.21 44.07 45.92 45.67 43.59 42.95 46.14 43.61 49.38 48.35 49.61 47.69 49.07 49.60 49.27 48.39 48.44 48.02 48.85CaO 0.74 0.76 0.55 0.22 0.30 0.58 0.80 0.40 0.50 0.17 0.16 0.09 0.18 0.12 0.15 0.13 0.23 0.13 0.19 0.15Na2O <0.01 <0.01 0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01K2O <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01TiO2 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01 <0.01P2O5 0.03 0.03 <0.01 0.04 0.03 0.01 0.03 0.01 0.02 <0.01 <0.01 0.01 0.02 0.02 0.02 0.02 0.02 0.02 0.03 0.02MnO 0.12 0.12 0.13 0.12 0.12 0.11 0.12 0.11 0.11 0.10 0.10 0.10 0.10 0.10 0.10 0.09 0.11 0.10 0.12 0.10Cr2O3 0.376 0.432 0.507 0.429 0.437 0.407 0.410 0.372 0.417 0.406 0.384 0.492 0.330 0.409 0.404 0.412 0.339 0.423 0.363 0.497TOTAL 99.04 99.24 99.14 99.02 99.03 99.09 99.24 98.95 99.16 99.06 98.94 98.89 98.27 98.52 98.57 98.68 98.62 98.82 98.85 98.72LOI 0.3 1.0 0.9 0.4 0.3 2.8 2.2 3.4 1.7 3.6 4.5 3.3 10.8 8.1 7.5 7.0 7.0 11.2 9.1 6.8Sc (ppm) 9.60 9.97 10.40 7.18 9.26 9.22 10.72 6.68 9.95 4.10 4.18 3.74 5.15 3.65 3.69 3.31 4.11 3.84 5.13 4.25Ti 59 31 26 28 22 50 40 71 30 11 7 17 13 12 14 13 15 22 12 14V 34.57 29.71 28.16 17.23 17.20 30.31 33.13 19.25 26.76 1.78 3.40 3.68 5.65 2.06 2.34 3.13 10.16 7.66 6.97 4.87Ni 1755 1825 1710 1746 1718 1686 1568 1560 1581 2907 2735 2876 2348 2390 2468 2572 2226 2200 2012 1974Co 94.31 90.53 92.69 99.68 88.75 81.42 95.44 75.18 79.64 112.90 119.10 116.40 96.97 102.80 98.92 92.85 97.84 85.70 93.94 78.06Cu 1.10 39.49 7.56 3.91 2.03 13.65 9.11 2.65 6.46 2.10 1.05 2.94 4.24 1.62 1.85 1.03 2.45 1.38 2.95 1.42Zn 41.65 37.17 36.82 33.29 36.57 41.16 37.52 35.65 33.87 31.36 52.37 34.19 54.61 36.33 57.36 28.28 41.27 33.82 42.94 21.47Ga 0.6928 0.4017 0.3397 0.2234 0.2294 0.5504 0.4745 0.3707 0.3647 0.0529 0.0585 0.1309 0.0916 0.0406 0.0505 0.0816 0.3417 0.2340 0.0806 0.1195Rb 0.0063 0.0122 0.0641 0.0204 0.0139 0.0197 0.0305 0.0217 0.0268 0.0065 0.0061 0.0113 0.0594 0.0062 0.0080 0.0079 0.0073 0.0143 0.0145 0.0104Sr 0.0722 0.1094 0.0848 0.1815 0.1346 0.0766 0.0810 0.0419 0.1181 0.2864 0.0624 0.2350 0.1258 0.2058 0.1015 0.2072 0.0552 0.1002 0.0703 0.0572Y 0.1144 0.0462 0.0345 0.0233 0.0342 0.0833 0.0620 0.1204 0.0521 0.0386 0.0127 0.0276 0.0347 0.0334 0.0334 0.0270 0.0742 0.0123 0.0239 0.0295Zr 0.0896 0.1111 0.0839 0.1112 0.0972 0.4065 0.0864 0.1345 0.0949 0.0905 0.0950 0.1017 0.1381 0.0947 0.0932 0.0780 0.0955 0.0741 0.1086 0.1024Nb 0.0216 0.0144 0.0215 0.0400 0.0203 0.0124 0.0142 0.0125 0.0149 0.0172 0.0163 0.0236 0.0159 0.0145 0.0123 0.0082 0.0100 0.0079 0.0065 0.0118Cs 0.0015 0.0019 0.0057 0.0028 0.0021 0.0020 0.0057 0.0050 0.0024 0.0018 0.0013 0.0021 0.0069 0.0022 0.0016 0.0020 0.0090 0.0016 0.0021 0.0020Ba 0.1469 0.2109 0.1284 0.2711 0.2330 0.1032 0.1000 0.0856 0.1021 0.4346 0.1511 0.3312 0.3390 0.1884 0.1254 0.1098 0.0750 0.0572 0.1401 0.1104Pb 0.0255 0.0270 0.0535 0.0238 0.0257 0.0232 0.0205 0.0233 0.0231 0.0216 0.0258 0.0320 0.0367 0.0325 0.0241 0.0187 0.0202 0.0189 0.0256 0.0283Th 0.0020 0.0020 0.0014 0.0017 0.0018 0.0018 0.0022 0.0018 0.0022 0.0016 0.0017 0.0018 0.0025 0.0016 0.0017 0.0018 0.0015 0.0012 0.0016 0.0020U 0.0018 0.0008 0.0013 0.0018 0.0015 0.0011 0.0013 0.0008 0.0010 0.0013 0.0010 0.0010 0.0014 0.0012 0.0012 0.0012 0.0011 0.0011 0.0014 0.0009La 0.0034 0.0046 0.0028 0.0042 0.0039 0.0033 0.0062 0.0047 0.0061 0.0038 0.0039 0.0045 0.0084 0.0065 0.0063 0.0031 0.0037 0.0026 0.0035 0.0062Ce 0.0082 0.0100 0.0058 0.0090 0.0089 0.0076 0.0825 0.0573 0.0733 0.0118 0.0100 0.0103 0.0201 0.0152 0.0192 0.0092 0.0100 0.0071 0.0100 0.0174Pr 0.0007 0.0010 0.0006 0.0010 0.0009 0.0007 0.0011 0.0008 0.0010 0.0007 0.0008 0.0009 0.0019 0.0014 0.0013 0.0007 0.0009 0.0005 0.0008 0.0010Nd 0.0035 0.0058 0.0033 0.0056 0.0048 0.0038 0.0044 0.0038 0.0049 0.0037 0.0043 0.0049 0.0097 0.0069 0.0063 0.0037 0.0049 0.0029 0.0046 0.0051Sm 0.0007 0.0013 0.0008 0.0014 0.0011 0.0008 0.0007 0.0027 0.0010 0.0007 0.0008 0.0009 0.0021 0.0014 0.0012 0.0009 0.0015 0.0005 0.0012 0.0008Eu 0.0002 0.0004 0.0002 0.0004 0.0003 0.0003 0.0002 0.0014 0.0002 0.0003 0.0002 0.0003 0.0007 0.0004 0.0004 0.0002 0.0006 0.0001 0.0003 0.0002Gd 0.0015 0.0016 0.0009 0.0018 0.0015 0.0018 0.0009 0.0114 0.0015 0.0014 0.0007 0.0011 0.0027 0.0017 0.0016 0.0012 0.0035 0.0004 0.0011 0.0010Tb 0.0009 0.0006 0.0005 0.0005 0.0006 0.0008 0.0006 0.0030 0.0006 0.0005 0.0003 0.0005 0.0007 0.0006 0.0006 0.0005 0.0011 0.0003 0.0004 0.0005Dy 0.0097 0.0043 0.0032 0.0026 0.0036 0.0071 0.0052 0.0190 0.0047 0.0037 0.0011 0.0026 0.0042 0.0035 0.0034 0.0024 0.0085 0.0007 0.0019 0.0029Ho 0.0038 0.0017 0.0012 0.0008 0.0011 0.0027 0.0021 0.0042 0.0018 0.0013 0.0004 0.0010 0.0012 0.0012 0.0011 0.0009 0.0026 0.0004 0.0008 0.0010Er 0.0182 0.0078 0.0058 0.0036 0.0051 0.0128 0.0103 0.0126 0.0079 0.0059 0.0025 0.0045 0.0048 0.0053 0.0052 0.0047 0.0105 0.0028 0.0047 0.0045Tm 0.0048 0.0022 0.0016 0.0010 0.0014 0.0035 0.0027 0.0024 0.0021 0.0015 0.0008 0.0012 0.0012 0.0013 0.0014 0.0014 0.0026 0.0011 0.0015 0.0012Yb 0.0401 0.0202 0.0151 0.0106 0.0125 0.0303 0.0256 0.0182 0.0198 0.0136 0.0085 0.0115 0.0109 0.0120 0.0119 0.0118 0.0204 0.0117 0.0160 0.0110Lu 0.0088 0.0048 0.0037 0.0027 0.0030 0.0068 0.0057 0.0037 0.0048 0.0032 0.0023 0.0027 0.0027 0.0027 0.0028 0.0029 0.0046 0.0032 0.0043 0.0026Hf 0.0025 0.0030 0.0024 0.0030 0.0026 0.0028 0.0023 0.0063 0.0026 0.0025 0.0026 0.0028 0.0038 0.0026 0.0038 0.0022 0.0028 0.0020 0.0029 0.0029Ta 0.0352 0.0199 0.0345 0.0627 0.0309 0.0141 0.0185 0.0166 0.0254 0.0210 0.0200 0.0359 0.0071 0.0172 0.0358 0.0100 0.0528 0.0056 0.0088 0.0114

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emplaced over the Alakırçay and Tahtalıdağ nappes, which includebasic volcanic and sedimentary units within the overall Antalyacomplex. The contact between cumulates and the upper mantlelithologies ranges between ‘transitional’ and ‘tectonic’ character. TheAO mantle sequence is mostly characterized by spinel lherzolite,harzburgite, dunite, and associated chromitite pods. The spinellherzolite is the dominant lithology in the Y.Karaman area, whereasthe harzburgite dominates elsewhere. The peridotites are reddish-brown, green, to yellowish-green in color, and show rugged topog-raphy. They are cut by isolated diabase and pyroxenite dykes. Thespinel lherzolites and the harzburgites at several exposures (e.g. Aksu,Y.Karaman, Tekirova and Çavuşköy) are notably fresh, whereas others(e.g. Serik, Altınyaka and Kemer) are highly serpentinized.

The AO dunites are always associated with podiform chromitites,which enclose the latter as ‘envelopes’, regardless of their shape andsize. The chromitites and their dunitic envelopes are found exclusivelyin harzburgite. The chromitites occur as discontinuous dike-likelenses, ranging between 10 and 20 m in length, 1 and 5 m in width,and 0.2 and 1 m in thickness. The dunite ‘envelopes’ tend to be moreserpentinized than their host harzburgites and are several centi-meters thick, mostly showing sharp contacts with the chromitite podsand, locally, more diffuse margins with the surrounding harzburgite.

3. Analytical methods

A representative range of samples of dunite, harzburgite, spinellherzolite and chromitite were collected from the Antalya ophiolitemantle sequences for petrographic study of textures and modalcompositions (Table 1). Despite the inevitable difficulties caused bystrong serpentinization a selection of samples was made for analysisof whole-rock major, trace and rare earth element contents, and theirconstituent mineral phases. Given the highly mobile character of Ca,Mg, Na, K, etc, only the least serpentinized, and least weathered,samples were analyzed. The whole-rock samples were crushed andpowdered in a clean agate mill in the clean laboratory of the Researchand Application Center for Geothermal Energy, Ground Water andMineral Resources at the Süleyman Demirel University. Because of thelow concentrations of many elements analyzed, sample contamina-tion was meticulously avoided and the samples were finely ground toallow for representative sampling for analysis.

Major elements were analyzed using ICP-ES at ACME AnalyticalLaboratories Ltd, Canada, following fusion with lithium metaborate/tetraborate and digestion by nitric acid. Detection limits of ICP-ES lietypically between 0.04 and 0.01% for the major elements analyzed.REE and trace elements were also analyzed by ICP-MS, using a ThermoScientific X-series II in the ultra-clean laboratories of the NorthernCentre for Isotopic and Elemental Tracing at Durham University (UK),following the procedures of Ottley et al. (2003). Due to the lowconcentration of many of the elements of interest, special care isrequired to minimize sample contamination with sample preparationwork being undertaken in clean air laminar flow hoods.

Briefly the procedure is as follows; into a Teflon vial 4 ml HF and1 ml HNO3 (SPA, ROMIL Cambridge) is added to 100 mg of powderedsample, the vial is sealed and left on a hot plate at 150°C for 48h. Theacid mixture is evaporated to near dryness, the moist residue has 1 mlHNO3 added and is again evaporated to near dryness. A second 1 mlHNO3 is again added and evaporated to near dryness. These stepsconvert insoluble fluoride species into soluble nitrate species. Thesample finally has 2.5 ml HNO3 added and is diluted to 50 ml after theaddition of an internal standard giving a final concentration of 20 ppbRe and Rh. The internal standard is used to compensate for anyanalytical drift and matrix suppression effects.

Modifying these procedures with the use of high purity acids, thedetection limits for most REE were less than 1 ng g−1. ICP-MScalibration was achieved by comparison of data for internationalrock standards (BHVO-1, AGV-1, W-2, NBS688) in addition to an ‘in-

house’ peridotite standard (GP13) (Ottley et al., 2003). Both standardand analytical blanks were prepared using the same technique as thatfor the analyzed samples. International reference standards were alsoanalyzed as unknowns within the analysis sequence for the Antalyasamples, to check for calibration drift. To improve the signal-to-noisethreshold, detector dwell times for low abundance elements wereincreased. The low concentrations and sample heterogeneity inperidotites can lead to poor reproducibility. The good detection limitsand care in sample crushing and preparation has reduced thisvariability. Replicate measurements of individual digestions of GP13run via ICP-MS showmeasurement uncertainties of 5–10% at these lowconcentrations (Ottley et al., 2003). The whole-rock analytical data ofthe AO mantle peridotites are given in Table 2.

Electron microprobe analysis of mineral phases was conducted onpolished thin sections of representative lherzolite, harzburgite, duniteand chromitite samples, using a JEOL 8600 electron microprobe at theUniversity of Georgia, USA. In addition to the Antalya samples, micro-probe analyses were executed on natural and synthetic mineralstandards using WDS spectrometers at a 15kV accelerating voltageand 15 nA beam current. The element abundances were computedusing the PRZ matrix correction. Analytical precision and accuracywere monitored by repeated analyses of mineral standards treated asunknowns. In particular, the standards for olivine 5 (UofOre), Cr-augite (NMNH), hypersthene (USNM 746) and chromite 5 (Taylor)were each analyzed 12 times over the course of the study — roughlycomparable to the number of analyses for a given mineral reportedhere. Precision of our mean analyses of these four mineral standardsshows that the precision for major elements is in the range of 1–2%(1 S.D.) for most major elements (>2 wt.% oxide). Fe+2 and Fe+3

proportions of spinel were calculated on the basis of assumedstoichiometry. Representative data for olivines, pyroxenes and spinelsfrom the AO mantle sequence are given in Tables 3–6.

4. Petrography

Asnoted, theAntalyamantle peridotites range fromspinel lherzolite,through harzburgite to dunite. The harzburgites contain (by volume)76.7–85.9% olivine (Ol), 10.5–20.0% orthopyroxene (Opx), 1.2–3.0%clinopyroxene (Cpx), 0.7–1.3% spinel (Sp) and (rare) 0.5–1.0% amphi-bole (Amp), whereas the spinel lherzolites consist of 68.4–77.3% Ol,15.0–23.0% Opx, 6.0–9.6% Cpx and 1.2–2.0% Sp (Table 1). Both typesshow mainly porphyroclastic textures typical of ‘residual’ mantle(Fig. 3A and C), characterized by millimeter-sized porphyroclasts of OlandOpx embedded in a fine-grained neoblasticmatrix. Amore or lesswell-developed mosaic texture of neoblasts with sharp grainboundaries is also locally observed. The olivine porphyroclasts inboth spinel lherzolites and harzburgites show deformation lamellae,undulose extinction, and lobate grain boundaries. Themineral grainsare corroded, anhedral, elongate and preferentially aligned. Theyoften contain Cr-sp and (unidentified) inclusions, possibly ofentrapped melt. Olivine also occurs as small neoblasts, the finerolivine grains usually rimming both Ol and Opx porphyroclasts,forming ‘lobate’ textures. Orthopyroxenes range from anhedral tosubhedral, with large crystals exhibiting kink bands along withubiquitous Cpx exsolution lamellae (Fig. 3C). Accessory clinopyrox-enes in the harzburgites contain both exsolution products and small(~0.5 mm) isolated neoblasts. In contrast, Cpxs in the spinellherzolites occurs only as deformed irregular grains (1–2 mm) withexsolution lamellae of Opx. Spinels in the lherzolites and harzbur-gites appear as brown anhedral crystals and occur both as isolatedgrains among silicate minerals and as inclusions in the latter. Theyalso usually contain olivine as inclusions. Scarce amphiboles (<1%)are found in some dunites and in the most refractory of harzburgites.

The textural features of these rocks are similar to those of manyfoliated ocean floor and ophiolitic peridotites. They may reflect partialmelting followed by deformation and static recrystallization in the

Table 4Clinopyroxene analyses from spinel lherzolites, harzburgites and dunites of the AO mantle peridotites.

Sample AN-8 An-9 AN-9 AN-13 Kzl-26G AN-3B AN-3B AN-6 AN-7B An-21 An-21 AN-27B AN-27B Kzl-16 Kzl-16 Kzl-22 Kzl-23 Kzl-28B Kzl-29B Kzl-32C Kzl-32C AN-7U Kzl-18 Kzl-26B

No. of analyses (4) (5) (1) (4) (5) (3) (2) (4) (5) (2) (1) (6) (6) (3) (2) (3) (5) (5) (3) (2) (2) (3) (3) (8)

Rock type Lhz Lhz Lhz Lhz Lhz Hz Hz Hz Hz Hz Hz Hz Hz Hz Hz Hz Hz Hz Hz Hz Hz Du Du Du

Cpx type(pr) (pr) (ex) (pr) (pr) (pr) (ex) (pr) (pr) (pr) (ex) (pr) (ex) (pr) (ex) (pr) (pr) (pr) (pr) (pr) (ex) (pr) (pr) (pr)

SiO2 52.77 51.84 51.68 52.29 52.41 53.02 53.29 52.39 52.26 54.83 54.23 54.33 53.93 53.61 52.81 55.22 53.37 54.55 55.32 53.40 52.90 53.77 55.80 54.38TiO2 0.08 0.20 0.16 0.18 0.12 0.12 0.04 0.07 0.08 0.00 0.07 0.01 0.00 0.03 0.09 0.01 0.08 0.00 0.04 0.04 0.03 0.03 0.03 0.07Al2O3 3.00 4.85 4.18 4.40 3.08 2.79 1.95 2.50 2.42 0.89 1.16 0.85 0.97 1.58 2.51 0.90 2.15 1.00 0.52 1.67 1.95 0.99 0.55 1.07Cr2O3 0.70 0.71 0.93 0.85 0.48 0.67 0.71 0.55 0.81 0.19 0.27 0.32 0.39 0.30 0.90 0.37 0.61 0.28 0.49 0.40 0.54 0.57 0.34 0.27FeO 1.98 2.11 2.30 2.01 2.00 1.76 1.55 1.88 1.80 1.95 1.93 1.90 2.24 2.02 2.19 2.03 1.74 2.07 1.68 2.33 2.22 1.53 1.12 1.72MnO 0.00 0.15 0.02 0.06 0.12 0.13 0.02 0.06 0.06 0.02 0.05 0.15 0.01 0.12 0.17 0.00 0.15 0.03 0.03 0.04 0.06 0.05 0.03 0.00MgO 17.07 16.15 16.66 16.18 17.58 17.58 18.81 17.55 17.85 18.57 18.68 18.30 18.23 18.32 17.61 18.68 17.82 17.97 18.29 18.64 18.66 18.14 18.15 17.86CaO 24.06 23.62 23.80 24.46 23.44 24.31 23.58 24.32 23.92 24.98 24.61 24.52 24.83 24.28 24.05 24.08 24.05 24.14 23.52 23.61 23.74 25.02 25.08 25.10Na2O 0.12 0.29 0.27 0.24 0.10 0.09 0.05 0.05 0.13 0.02 0.02 0.03 0.05 0.01 0.06 0.07 0.00 0.00 0.20 0.00 0.08 0.26 0.10 0.05Total 99.78 99.93 100.00 10.66 99.27 100.86 99.96 99.38 99.33 101.45 101.02 100.42 100.64 100.27 100.39 101.38 99.97 100.04 100.10 100.13 100.180 100.36 101.20 100.61WO 48.75 49.36 48.78 50.34 47.30 48.38 46.25 48.40 47.64 47.72 47.19 47.53 47.80 47.20 47.72 46.653 47.79 47.54 46.86 45.94 46.12 48.59 48.95 48.94EN 48.13 46.96 47.51 46.334 49.36 48.68 51.34 48.59 49.47 49.36 49.84 49.36 48.83 49.55 48.62 50.356 49.27 49.24 50.70 50.46 50.44 49.02 49.29 48.45FS 3.12 3.69 3.71 3.32 3.34 2.95 2.41 3.01 2.89 2.92 2.97 3.11 3.38 3.25 3.65 2.99 2.93 3.23 2.44 3.60 3.45 2.39 1.75 2.61Mg# 93.9 93.1 92.9 93.5 94.0 94.7 95.6 94.4 94.6 94.5 94.6 94.5 93.6 94.2 93.5 94.4 94.8 93.9 95.5 93.5 93.7 95.5 96.6 94.9

The major elements are in wt.%. Mg#: 100⁎ [Mg/(Mg+FeTotal)]. Total iron as FeO. Lhz: spinel lherzolite, Hz: harzburgite, Du: dunite, Chr: chromitite, ex: exsolution lamella, pr: primary grain.

Table 3Olivine analyses of mantle peridotites and chromitites from the Antalya ophiolites.

Sample AN-8 AN-9 AN13 Kzl-26G AN-3B AN-6 AN-7B An-21 AN-27B Kzl-16 Kzl-23 Kzl-28B Kzl-29B Kzl-32C AN-7U Kzl-1C Kzl-18 Kzl-26B Kzl-32A AN-7C Kzl-1A Kzl-17A Kzl-26E Kzl-32B AN-27C

No. of analyses (6) (6) (7) (5) (8) (6) (6) (6) (6) (4) (8) (7) (7) (7) (5) (6) (7) (8) (7) (3) (8) (8) (8) (6) (7)

Rock type Lhz Lhz Lhz Lhz Hz Hz Hz Hz Hz Hz Hz Hz Hz Hz Du Du Du Du Du Chr Chr Chr Chr Chr Chr

SiO2 40.38 41.14 40.67 40.23 41.25 41.21 41.07 41.54 40.90 40.77 40.96 40,88 41.81 40.72 41.13 41.27 41.71 41.14 40.93 41.44 41.32 41.27 41.52 42.01 41.89TiO2 0.00 0.00 0.02 0.00 0.01 0.00 0.00 0.00 0.00 0.00 0.05 0,00 0.04 0.00 0.00 0.00 0.00 0.00 0.01 0.03 0.00 0.00 0.00 0.00 0.00Al2O3 0.04 0.01 0.01 0.00 0.07 0.00 0.02 0.00 0.00 0.00 0.02 0,01 0.00 0.03 0.01 0.00 0.03 0.00 0.02 0.00 0.00 0.01 0.01 0.01 0.01Cr2O3 0.00 0.08 0.00 0.00 0.05 0.05 0.07 0.07 0.05 0.16 0.02 0,00 0.08 0.08 0.00 0.05 0.06 0.00 0.09 0.01 0.21 0.00 0.05 0.01 0.00FeO 8.82 9.28 9.40 8.82 8.22 8.10 7.87 8.20 8.10 8.23 8.05 8,46 7.91 7.59 6.46 7.48 6.33 7.03 6.68 4.15 4.28 3.88 4.78 4.30 4.79MnO 0.17 0.21 0.09 0.19 0.15 0.13 0.04 0.00 0.10 0.04 0.14 0,18 0.18 0.02 0.02 0.06 0.06 0.18 0.00 0.08 0.05 0.05 0.00 0.05 0.00NiO 0.42 0.42 0.44 0.43 0.55 0.41 0.41 0.40 0.40 0.39 0.32 0,50 0.41 0.46 0.32 0.57 0.35 0.44 0.39 0.36 0.67 0.64 0.50 0.57 1.00MgO 50.26 49.43 49.41 49.79 49.78 50.58 50.91 51.14 50.36 50.67 49.98 50,44 50.19 50.87 51.64 51.06 52.12 50.81 51.12 53.53 53.97 53.38 53.82 52.92 53.54CaO 0.02 0.03 0.00 0.02 0.01 0.00 0.00 0.02 0.03 0.00 0.02 0,00 0.01 0.03 0.04 0.12 0.07 0.02 0.03 0.00 0.03 0.02 0.02 0.05 0.02Total 100.11 100.61 100.05 99.48 100.08 100.48 100.39 101.37 99.94 100.27 99.56 100,47 100.63 99.79 99.62 100.61 100.75 99.62 99.27 99.60 100.53 99.25 100.70 99.92 101.25Fo 91.1 90.5 90.3 90.4 91.5 91.8 92.0 91.7 91.7 91.7 91.7 91.4 91.9 92.3 93.4 92.4 93.6 92.8 93.2 95.9 95.8 96.1 95.3 95.7 95.2

The major elements are in wt.%. Fo=Mg#: 100⁎ [Mg/(Mg+Fe+2)]. Total iron as FeO. Lhz: spinel lherzolite, Hz: harzburgite, Du: dunite, Chr: chromitite, Fo: forsterite.

313Ş.Caran

etal./

Lithos114

(2010)307

–326

Table 5The chemical composition of orthopyroxenes in lherzolites and harzburgites of the AO mantle peridotites.

Sample AN-8 An-9 AN-9 AN-13 AN-13 Kzl-26G AN-3B AN-6 AN-7B An-21 AN-27B AN-27B Kzl-16 Kzl-22 Kzl-23 Kzl-28B Kzl-29B Kzl-32C

No. ofanalyses

(2) (5) (1) (5) (1) (5) (6) (4) (5) (3) (3) (2) (5) (4) (10) (10) (7) (4)

Rock type Lhz Lhz Lhz Lhz Lhz Lhz Hz Hz Hz Hz Hz Hz Hz Hz Hz Hz Hz Hz

Opx type(pr) (pr) (ex) (pr) (ex) (pr) (pr) (pr) (pr) (pr) (pr) (ex) (pr) (pr) (pr) (pr) (pr) (pr)

SiO2 53.85 55.31 53.78 55.53 54.63 55.91 56.74 55.85 55.38 56.68 57.12 57.10 56.41 57.12 56.55 56.98 58.73 56.43TiO2 0.03 0.09 0.03 0.02 0.04 0.04 0.02 0.04 0.03 0.04 0.01 0.00 0.02 0.01 0.01 0.00 0.03 0.02Al2O3 3.66 3.87 4.94 3.14 4.48 2.73 1.96 2.70 2.74 1.72 1.11 1.05 2.37 1.11 2.08 1.09 0.52 1.83Cr2O3 0.86 0.41 0.71 0.30 0.48 0.53 0.55 0.87 0.89 0.51 0.43 0.43 0.72 0.43 0.34 0.69 0.18 0.53FeO 6.33 6.59 7.29 6.74 7.24 6.13 5.48 5.59 5.67 5.61 5.57 5.87 6.18 5.57 5.81 5.92 5.76 5.47MnO 0.21 0.13 0.11 0.01 0.01 0.14 0.00 0.08 0.10 0.11 0.10 0.22 0.03 0.10 0.16 0.14 0.12 0.13MgO 34.23 33.40 32.45 33.87 32.62 34.44 34.97 34.02 34.81 34.51 35.01 35.14 33.01 35.01 34.84 35.48 35.90 34.82CaO 0.56 0.75 0.47 0.48 0.43 0.37 0.49 0.62 0.73 0.52 0.57 0.55 0.76 0.57 0.53 0.64 0.38 0.61Na2O 0.01 0.03 0.01 0.01 0.00 0.00 0.00 0.01 0.00 0.01 0.01 0.00 0.01 0.01 0.00 0.00 0.00 0.02Total 99.74 100.57 99.77 100.25 99.93 100.29 100.21 99.78 100.35 99.71 99.93 100.36 99.51 99.93 100.32 100.94 101.63 99.86WO 1.05 1.43 0.91 0.91 0.84 0.70 0.77 0.98 1.36 0.98 1.06 1.02 1.48 1.06 0.99 1.17 0.69 1.14EN 89.37 88.57 87.85 88.93 88.17 90.10 90.79 90.19 90.25 90.59 90.70 90.21 89.12 90.70 90.33 90.19 90.95 90.68FS 9.58 10.00 11.24 10.17 10.99 9.20 8.45 8.83 8.39 8.43 8.24 8.78 9.41 8.24 8.69 8.64 8.36 8.18Mg# 90.6 90.0 88.8 90.0 88.9 90.9 91.6 91.3 91.7 91.6 91.8 91.4 90.5 91.8 91.5 91.4 91.7 91.9

The major elements are in wt.%. Mg#: 100⁎ [Mg/(Mg+FeTotal)]. Total iron as FeO. Lhz: spinel lherzolite, Hz: harzburgite, ex: exsolution lamella, pr: primary grain.

314 Ş. Caran et al. / Lithos 114 (2010) 307–326

asthenosphere (Pearce et al., 2000). The lobate grain boundaries areinterpreted as replacement features, perhaps produced by incongru-ent dissolution of orthopyroxene (Parkinson and Pearce, 1998).

The dunite envelopes, locally grading into harzburgite, have ≥98%modal Ol, ≤0.7% clinopyroxene, 1.0% Sp and 1% Amp (in somesamples) (Table 1). In the dunites, spinel crystals differ morpholog-ically from those in the harzburgites and the spinel lherzolites,occurring mainly as euhedral to subhedral grains associated witholivines (Fig. 3D). The modal volume of spinel from the dunites isgenerally similar to that of the host rocks, but a few thin bands ofdisseminated chromitite are sometimes present. Scarce Cpx in thedunites occurs as small anhedral grains between olivine crystalsalthough Opx is absent. The dunites are the most serpentinized rocksamong the AO mantle peridotites. Thus, they mostly show a ‘mesh’texture of serpentine and olivine. The mesh texture may result fromthe serpentinization of adcumulate olivines, which are crystallizedfrom intercumulus liquid during dunite formation.

Chromitite pods comprising c. 50–95% chromian spinel (Cr-sp)generally include massive and disseminated types. Massive chromi-tites consisting of >80% modal Cr-sp are typically coarse-grained (1–5 mm) and closely packed, whereas the disseminated chromititestypically contain 50–80% Cr-sp, and are finer grained (0.5–2 mm).Interstitial material consists mainly of olivine and rarely amphibole. Insome samples, silicates are mostly replaced by serpentine and/orchlorite. Individual Cr-spinel grains are nearly euhedral or subhedral,partially fractured and show cumulate textures.

5. Geochemistry

5.1. Bulk rock chemistry

Loss-on-ignition (LOI) values indicate that all of the dunites andsome of the harzburgites and spinel lherzolites were variablyserpentinized, although most of the harzburgites and spinel lherzolitesare fresh. Tominimize the effects of serpentinization, themajor elementdata were normalized on a volatile-free basis for better comparisonbetween samples. It is well recognized that correlations both among,and between, major and trace elements allow for relatively robustpetrogenetic interpretations.

Whenplotted againstMgO,major oxides and some trace elements ofthe AO mantle peridotites show excellent correlations (Fig. 4). Threedistinct groups are recognized based on geochemistry and petrography.The first group consists of spinel lherzolite, reflecting less depletion inelements such as Al2O3 (1.03–2.39 wt.%), CaO (1.05–2.24 wt.%), SiO2

(44.77–46.92 wt.%), Ti (99–357 ppm), Sc (10.63–14.69 ppm), V (40.33–54.91 ppm), Ga (0.799–1.717 ppm), and Y (0.252–1.614 ppm), alongwith lower Ni (1261–1532 ppm) contents, for equivalent MgO (39.65–42.01 wt.%). The second group includes harzburgites, which show amore depleted character, i.e. lower contents of Al2O3 (0.21–1.12 wt.%),CaO (0.22–1.04 wt.%), SiO2 (42.32–45.41 wt.%), Ti (18–86 ppm),Sc (6.57–11.31 ppm), V (17.20–39.26 ppm), Ga (0.223–0.875 ppm),Y (0.023–0.259 ppm) and higher Ni (1401–2350 ppm) contents,for equivalent MgO (42.76–46.80 wt.%). The third group is repre-sented by highly depleted dunite ‘envelopes’ with the lowest Al2O3

(0.04–0.25 wt.%), CaO (0.09–0.23 wt.%), SiO2 (39.85–40.84 wt.%), Ti (7–15 ppm), Sc (3.65–5.15 ppm),V (2.06–7.66 ppm),Ga (0.040–0.234 ppm),Y (0.012–0.074 ppm) and the highest Ni (1974–2907 ppm) contents forequivalent MgO (47.69–49.60 wt.%). The three groups correspond,respectively, with 1) mid-ocean ridge peridotites, 2) harzburgites whichare dominant in forearc settings and (rarely) some ‘abyssal’ exposures attransform fracture zones, and 3) SSZ and/or forearc exposures of duniteveins (Fig. 4). Suchvariationamongperidotitesmaybeattributed to1) theeffects of differential (prior) melt extraction from primitive (i.e. ‘fertile’oceanic) mantle (e.g. Flower, 2003), 2) cumulates resulting (at least insomecases) fromall or anyof theabove(e.g. Suhret al., 1998), or3)effectsof interaction between partial melts of varying composition with uppermantle peridotites (e.g. Kelemen et al., 1992).

Elements such as Al, Ca, Si, Ti, Sc, V and Y are all incompatible withrespect to olivine and show negative covariance with MgO contentsbetween spinel lherzolite, harzburgite and dunite. In contrast, compat-ible Ni increases as modal Opx and Cpx decrease at the expense ofolivine (i.e. modal Ol/(Opx+Cpx) ratios increase) (Fig. 4). Thus MgOcontent serve as an index of depletion for the different types ofperidotite. Not surprisingly, mineral phase compositions show analo-gous changes that match those of their host whole-rock compositions,clearly reflecting partial melting and/or fractionation histories of theophiolite peridotites.

The three groups of theAOperidotites are also easily distinguished inplots of REE andMgO contents (Fig. 5). The heavy REEs (Tm, Y, Lu) shownegative correlations with MgO contents in all three lithologies. Themiddle REEs (Sm, Eu, Gd) are also negatively correlated with MgO indunites and lherzolites but showpositive correlation in the harzburgites(Fig. 5). In contrast, the light REEs (La, Ce, Pr) show considerable scatterand no clear correlations are observed. The scatter among the LREEmayreflect metasomatic interaction between the peridotites and slab-derived hydrous fluids and/ormelts because it is expected that residuesof partial melting must be more depleted in LREE for higher degree ofpartial melting. Due perhaps to their lower mobility, the HREEs may

Table6

Spinel

analyses

ofthesp

inel

lherzo

lites,h

arzb

urgites,du

nitesan

dpo

diform

chromitites

from

theAO

man

tlepe

rido

tites.

Sample

AN-8

An-

9AN-13

Kzl-26G

AN-3B

AN-6

AN-7B

An-

21AN-27B

Kzl-16

Kzl-23

Kzl-28B

Kzl-29B

Kzl-32C

AN-7U

Kzl-1C

Kzl-18

Kzl-26B

Kzl-32A

AN-7C

AN27

CKzl-1A

Kzl-17A

Kzl-26E

Kzl-32B

No.

ofan

alyses

(6)

(6)

(6)

(5)

(6)

(3)

(7)

(4)

(6)

(3)

(8)

(7)

(8)

(5)

(5)

(6)

(4)

(5)

(4)

(6)

(5)

(7)

(9)

(7)

(6)

Rock

type

Lhz

Lhz

Lhz

Lhz

Hz

Hz

Hz

Hz

Hz

Hz

Hz

Hz

Hz

Hz

Du

Du

Du

Du

Du

Chr

Hz

Chr

Chr

Chr

Chr

TiO2

0.05

0.05

0.07

0.01

0.05

0.06

0.07

0.04

0.07

0.06

0.08

0.06

0.06

0.07

0.17

0.11

0.12

0.21

0.18

0.12

0.12

0.14

0.19

0.06

0.17

Al2O3

42.56

50.81

50.31

35.81

34.51

35.39

32.05

21.09

16.17

28.46

38.42

17.00

10.63

23.64

15.19

14.02

15.12

15.82

14.48

15.01

14.66

14.03

12.25

11.04

14.28

Cr2O

326

.19

16.63

17.55

32.13

33.60

34.02

36.61

46.33

51.78

38.95

28.63

49.37

55.43

45.67

50.12

53.67

50.26

49.40

53.20

55.65

54.73

56.24

57.91

59.3

55.28

Fe2O

31.44

1.54

1.26

2.01

1.86

1.53

1.39

2.97

2.44

2.42

1.78

4.02

4.75

1.47

3.78

3.14

6.31

6.58

4.22

2.56

2.84

2.45

3.43

2.73

2.70

FeO

13.71

12.37

12.23

15.77

14.46

15.18

15.01

17.84

18.32

15.68

13.32

18.79

19.71

15.83

16.32

17.59

15.42

16.79

14.65

12.53

13.84

13.15

11.99

14.08

12.66

MnO

0.23

0.22

0.19

0.13

0.15

0.17

0.12

0.19

0.27

0.03

0.21

0.26

0.27

0.05

0.21

0.26

0.38

0.34

0.22

0.30

0.13

0.17

0.35

0.14

0.14

MgO

16.36

17.87

17.96

14.25

14.72

14.86

14.30

11.27

10.38

13.39

15.7

10.19

8.95

12.97

11.13

10.66

12.15

11.60

12.62

14.25

13.31

13.75

14.33

12.86

13.97

CaO

0.02

0.00

0.00

0.02

0.02

0.01

0.02

0.04

0.00

0.00

0.02

0.01

0.00

0.02

0.03

0.11

0.00

0.02

0.02

0.02

0.00

0.00

0.00

0.00

0.00

NiO

0.09

0.26

0.30

0.03

0.11

0.08

0.07

0.03

0.00

0.16

0.23

0.01

0.08

0.06

0.03

0.23

0.10

0.22

0.05

0.12

0.19

0.09

0.09

0.13

0.18

Total

100.63

99.75

99.87

100.15

99.48

101.30

99.64

99.80

99.43

99.15

98.39

99.71

99.88

99.78

96.98

99.68

99.86

100.98

99.08

100.56

99.79

100.02

100.54

100.34

99.38

Mg#

68.0

72.0

72.4

59.1

64.5

63.6

62.9

53.0

50.2

60.3

67.8

49.1

44.7

59.3

54.9

51.9

58.4

55.2

60.1

67.0

63.2

65.1

68.1

62.0

66.3

Cr#

29.2

18.0

19.0

37.6

40.5

39.2

43.4

59.6

68.2

47.9

33.3

66.1

77.8

56.4

68.9

72.0

69.0

67.7

71.1

71.3

71.5

72.9

76.0

78.3

72.2

Themajor

elem

ents

arein

wt.%

.Cr#

:10

0⁎[Cr/(C

r+Al)],Mg#

:10

0⁎[M

g/(M

g+

Fe+

2).Se

parating

Fe+

2an

dFe

+3acco

rdingto

perfectstoich

iometry.L

hz:sp

inel

lherzo

lite,

Hz:

harzbu

rgites,C

hr:ch

romitite.

315Ş. Caran et al. / Lithos 114 (2010) 307–326

record partialmeltingprocesses rather thanmelt/fluid–rock interaction.Progressive depletions of MREE and HREE from spinel lherzolites todunites could simply reflect modal inhomogeneity because the bulkrock REE abundances are mostly controlled by the amount of Cpxmodein the AO peridotites. The modal inhomogeneity may result from bothpartial melting and melt–rock interaction.

As observed in Fig. 6 the chondrite-normalized REE distributionsvary significantly. The AO spinel lherzolites show progressive depletionfromLu(HREE, 0.15–1.5) to Pr (LREE, 0.006–0.06) and slight increases inCe and La. The small Ce anomalymay reflect secondary alteration ratherthan primary magmatic processes (Gruau et al., 1998). Their chondrite-normalized REE patterns display LREE depleted signature. The patternsand the [La/Sm]CN (0.1–0.6) and [La/Yb]CN (0.01–0.06) ratios are typicalof MOR-type peridotites, except for their overall lower total REEabundances. The AO harzburgites have chondrite-normalized HREEabundances of 0.011–0.15 and LREE of 0.006–0.15 (Fig. 6B), somewhatless uniform than the spinel lherzolites, but all display ‘V-shaped’patternswithMREEminima, [La/Sm]CN of 1–10and [La/Yb]CN of 0.1–0.6.These patterns show distributions similar to those of harzburgites frommodern forearcs (e.g. Izu–Bonin–Mariana and South Sandwich forearccomplexes) and may indicate subduction-related contamination (asnoted above). The forearc harzburgites appear to represent residuederived frombothMORand SSZ settings, but both types invariably showthe effects of (presumably) subduction-derived contamination —

relative enrichment in LREE indicating the addition of sediment-derivedpartial melt fractions (e.g. Parkinson and Pearce, 1998; Pearce et al.,2000). It should be pointed out that the harzburgite REE patternsstrongly resemble those of boninites (Fig. 6B), albeit with even lower(i.e. ‘depleted’) absolute concentrations.

The AO dunites also have V-shaped, chondrite-normalized REEpatterns. Normalized contents of HREE are 0.007–0.045, LREE contentsare 0.004–0.05. These patterns resemble those observed in dunitesfrom the Izu–Bonin–Mariana and South Sandwich forearcs, andboninites from numerous locations (Fig. 6C). Dunites sampled fromthe Izu–Bonin–Mariana and South Sandwich forearcs have beeninterpreted as having formed from the interaction of residualharzburgite with subduction-related magmas (Parkinson and Pearce,1998).

5.2. Mineral chemistry

Mineral phase compositions in mantle peridotites are consideredto be reliable petrogenetic indicators. Their compositions aredependent on the degree and conditions of partial melting and theeffects of magma–rock interaction, as exhibited by the Antalyaophiolite spinel lherzolites, harzburgites, dunites and chromitites.Representative microprobe analyses are listed in Tables 3–6. Thecomplete data set for the mineral phases is shown in the plots inFigures (Figs. 7–11). Olivine compositions range between Fo 90.0 and91.5 in the spinel lherzolites, Fo 90.9 and 92.7 in the harzburgites, Fo92.1 and 94.7 in the dunites and Fo 94.8 and 96.8 in the chromitites(Table 3). They have negligible Ti, Al and Ca, but relatively high NiO2

(0.29–0.72 wt.%) contents. Cr2O3 contents rarely exceed 0.21 wt.%.Representative analyses of primary (porphyroclastic, neoblastic)

Cpx grains and lamellae (exsolved fromOpx) are given in Table 4. Cpx inthe spinel lherzolites shows higher contents of Al2O3 (2.22–4.85 wt.%),TiO2 (0.09–0.22 wt.%), FeOt (1.95–2.30 wt.%) andNa2O (0.10–0.29 wt.%)than those from the harzburgites (Al2O3: 0.46–2.23 wt.%; TiO2: up to0.12.wt.%; FeOt: 1.57–2.51 wt.% and Na2O: up to 0.13 wt.%). Likewise,Mg#s [Mg#: 100⁎[Mg/(Mg+Fetot)] and CaO and SiO2 contents of theformer are significantly lower than those of the harzburgites. Cpx in thedunites show restricted covariation of Al2O3 (0.36–1.32 wt.%), TiO2 (upto 0.15 wt.%), FeOt (1.12–1.85 wt.%), Na2O (0.02–0.35 wt.%), SiO2

(53.53–55.80 wt.%) and CaO (24.01–26.07 wt.%), with Mg# of 94.6–96.6. Cpx compositions in the harzburgite and the dunitemostly overlapthose of forearc harzburgites (Fig. 7) although those in thedunites plot in

Fig. 3. Microscopic views of the AO mantle peridotites. Spinel lherzolites and harzburgites commonly show porphyroclastic textures. Millimeter-sized porphyroclasts of olivine(A; B), and orthopyroxene (C) are set in amatrix of fine-grained olivine. Elongated olivine phenocrystals show deformation lamellae and undulose extinction. (D) Dunites havemeshtextures and euhedral spinel crystals. Some of the olivine is partially altered to serpentine.

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themore depleted area. In contrast, those in the spinel lherzolites extendtomore fertile (less depleted) compositions. Such distinctions appear tobe independent of those of porphyroclastic, neoblastic and exsolved Cpxcompositions, given their similarly restricted compositional range.

Selected Opx data for the Antalya peridotites are given in Table 5.Opxs in the spinel lherzolites have higher contents of Al2O3 (2.35–4.94 wt.%), Cr2O3 (0.20–0.86 wt.%) and FeOt (5.72–7.29 wt.%) than thosein the harzburgite (Al2O3: 0.46–2.86 wt.%; Cr2O3: 0.14–0.94 wt.%; FeOt:5.26–6.46 wt.%). In contrast,Mg# (88.8–91.3) andSiO2 contents (53.78–56.40 wt.%) of the lherzolitic Opx phases are lower than those in theharzburgites (Mg#: 90.7–92.3; SiO2: 54.97–58.73 wt.%), with negligibleTiO2 (up to 0.09 wt.%) and low CaO (usually <1 wt.%) contents. TheOpxcompositions are thus analogous to those of their coexisting Cpx crystals,although Opx is essentially absent from the dunites.

Representative spinel compositions in spinel lherzolites, harzbur-gites, dunites and chromitites from the AO are given in Table 6. Thespinel lherzolites show low spinel Cr#s (Cr#: 100⁎ [Cr/(Cr+Al)](13.3–39.6) although the harzburgitic spinels generally have relativelyhigh Cr# (33.2–70.2). The dunitic spinels have markedly higher Cr#(68.9–72.2) and higher TiO2 (0.08–0.17 wt.%) contents than those ofthe harzburgites and the spinel lherzolites (TiO2: up to 0.08 wt.%).Spinels in harzburgites and spinel lherzolites display a positivecovariance between Cr# and Mg#, in contrast to those of dunites(Fig. 8). The spinel data for the harzburgites conformclosely to those offorearc harzburgites, whereas those for the spinel lherzolites closelyreplicate those ofmid-ocean ridge-type peridotites. On the other hand,the dunitic spinels are analogous with those in subduction-relateddunites and boninites.

Spinel Cr# in the Antalya chromitites range between 69.5 and 80.2(Cr2O3 contents between54.49 and 59.53 wt.%, Al2O3, between 9.76 and15.75 wt.%, and TiO2 between 0.05 to 0.19) (Table 6). The chromititesinvariably show higher spinel Cr# and TiO2 contents than those of theirhost rocks (especially with respect to harzburgite). The spinel

compositional relationships for the Antalya chromitites are consistentwith thoseof podiformchromitites in ophiolites elsewhere, as describedby Barnes and Roeder (2001), and those of boninitic magmas (e.g. vander Laan et al., 1992; Sobolev and Danyushevsky, 1994) (Fig. 8). As thespinel Mg# in the peridotitic rocks is lowered substantially that in thechromitite is raised, presumably due to subsolidus Mg-Fe2+ redistribu-tion with respect to olivine, and depending on the volume ratio ofolivine and spinel (Arai, 1980).

Amphiboles in the dunites, harzburgites and chromitites arehornblende characterized by high Cr2O3 (1.11–2.23 wt.%), Al2O3

(5.63–10.38 wt.%), TiO2 (0.11–0·81 wt.%) and Na2O (0.89–2.28 wt.%)contents, and tremolite showing relatively low Cr2O3 (0.31–0.81 wt.%),Al2O3 (0.79–3.14 wt.% wt.%), TiO2 (0.05–0·14 wt.%), Na2O (0.25–0.80 wt.%) and K2O (<0.08 wt.%) contents.

6. Discussion

6.1. ‘Fertile’ vs ‘refractory’ mantle and partial melting

In general, modal abundances and compositions of mineralconstituents in peridotites reflect the extent of prior depletion in‘fusible’ elements such as Ca, Al, and Ti of pre-existing ‘fertile’ mantlecompositions (e.g. Dick and Fisher, 1984). Therefore, bulk rockchemistry, mineral compositions, and modal mineralogy of perido-tites are clearly useful as tools for formulating partial melting modelsand as indicators of prior partial melting histories. It is well knownthat Cpx is the phase consumed initially during anhydrous partialmelting, at least in spinel facies lherzolitic peridotites (Jaques andGreen, 1980; Baker and Stolper, 1994; Parkinson and Pearce, 1998).However, minor amounts of clinopyroxene may persist further inresidue during hydrous melting of a spinel peridotite (Gaetani andGrove, 1998).

Fig. 4.MgO vs Al2O3, CaO, SiO2, Ti, Sc, V, Ga, Y and Ni diagrams for spinel lherzolites, harzburgites and dunites from the AO mantle peridotites. Major elements are in wt.% and traceelements are in ppm. Field of MOR peridotite is from Niu (2004). Fields of forearc harzburgites and SSZ dunites (from Izu–Bonin–Mariana forearcs) are from Parkinson and Pearce(1998).

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Modal Cpx proportions decrease progressively from the AO spinellherzolites (9.6–6.0% Cpx) to the AO harzburgites (3.0–1.2% Cpx). TheAO dunites include small quantities (0.5%) of Cpx. Opx modalproportions also decrease concomitantly (and are absent fromdunites), whereas the modal proportion of olivine increases. Suchchanges are associated with progressively more depleted bulk rockand mineral composition. Progressive increases in whole-rockrefractory character is accompanied by higher Mg# in Ol, Opx andCpx, lower Al2O3 contents in Opx and Cpx, higher Cr# in spinel, lowerCpx mode, higher Ol mode, and reduced Al, Ca, Ti, Si, V, Y, Ga, MREEand HREE contents in their respective bulk rock compositions (Figs. 4,5, 8 and 9). Accordingly, less depleted spinel lherzolites give way tomore depleted harzburgites and highly depleted dunites. Because Al,Ca, Ti, Si, V, Y, Ga, and LREE are preferentially enriched in partial meltsof peridotite or in hybridized melts resulting from the interaction ofprimitive basaltic melts with refractory peridotites, such correlationsmay equally represent residue from varying degrees of melting of acommon source or indicate coexistence of old peridotites previouslymelted and new peridotites derived from the old peridotites by melt–

rock interaction. Given these possibilities, the geochemical range ofboth bulk rock and mineral component compositions in the Antalyaperidotites may reflect a number of different processes, none of whichis mutually exclusive (e.g. Pearce, 2005).

The compositions of mineral phases in host peridotites andpodiform chromitites are considered as a powerful petrogeneticindicator and their compositions are highly dependent on the degreeand conditions of partial melting and of magma/rock interactions(e.g., Dick and Bullen, 1984; Ahmed et al., 2001; Piccardo et al., 2007).High Cr# in spinels may reflect relatively large melt fractions of afertile peridotite (Dick and Bullen, 1984) along with high Fo contentsin olivine as olivine–melt equilibria are not substantially changed byvariations in H2O (Gaetani and Grove, 1998). This relationship isillustrated by plots of spinel Cr# vs coexisting olivine Fo content (the‘olivine–spinel mantle array’ or ‘OSMA’, of Arai, 1994) (Fig. 10A). Here,spinel lherzolite and harzburgite compositions follow partial meltingtrends within the OSMA field. However, dunites show fractionationtrends similar to those of boninitic magmas. According to thisscenario, the spinel lherzolites and the harzburgites from the AO

Fig. 5. Plots of REE against MgO for AO mantle peridotites.

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can be inferred to be the products of progressive partial meltingepisodes, in contrast to the AO dunites.

Chondrite-normalized, whole-rock REE abundances in the variablyrefractory peridotites (assuming their derivation from fertile ‘N-MORB’-like sources under spinel facies conditions; Piccardo et al.,2007), can be used to model the degree of partial melting. Modelingwith relatively immobile HREE (LREE contents in peridotites may bemodified by slab-derived fluids or melts) suggests that 8–18% partialmelting of an N-MORB-like source produces a residue with REEcontent similar to those of the AO spinel lherzolites (Fig. 10B),whereas 17–25% melting of a similar source would be necessary toproduce the AO harzburgites (Fig. 10C). The REE patterns of the AOharzburgites show steeper slopes than that of the partial meltingmodels of MOR mantle. This may be the result of an interaction in asupra-subduction environment between a less depleted MOR mantlelithosphere (the AO spinel lherzolites), that had experienced anearlier partial melting event, with an ascending LREE-enriched melt.The interaction must have caused modest melt fractions of the oldmantle lithosphere, which give way to more depleted harzburgites.

Such hypothetical melting models have been quantified on thebasis of Ti-Yb plots in Fig. 10D (Parkinson and Pearce, 1998). Here, we

compare the observed compositions of spinel lherzolite and harzbur-gite samples from the AO with theoretical batch and fractionalmelting models for garnet and spinel peridotite sources. The plots inFig. 10D illustrate that the AO harzburgite data conform to a calculatedarray of 17–25% fractional melting paths of spinel facies peridotite,whereas the AO spinel lherzolites conform to the array of 8–18%fractional melting. Irrespective of the interpretation adopted, it maybe inferred that both bulk rock and mineral data for the spinellherzolites and the harzburgites are consistent with a systematicprogression in degree of partial melting — whether in one or morestages.

The AO dunites include a very refractory olivine–spinel assem-blage (Fo: 92.1–94.7 – Cr#: 68.9–72.2). The ultra-refractory characterof the Antalya dunites is common to dunites in several modernsubduction-related systems. The SSZ dunites could hypotheticallyresult either from relatively large degrees of partial melting ofdepleted MOR-type mantle in a supra-subduction zone, or aninteraction between highlymagnesianmelts and depleted peridotites,which produces residue of extremely high degrees of partial melting(Parkinson and Pearce, 1998; Pearce et al., 2000). The AO dunitesare found as envelopes surrounding the high-Cr chromitites which

Fig. 6. Chondrite-normalized (Sun and McDonough, 1989) whole-rock REE patterns for (A) spinel lherzolites, (B) harzburgites and (C) dunites from the Antalya ophiolites. Field ofMOR peridotites is from Pearce et al. (2000), Ottenello et al. (1979, 1984a,b), Frey et al. (1985), Bodinier et al. (1988) and Bodinier (1988). Line of oceanic mantle (N-MORB-like) isfrom McCulloch and Bennett (1994). Line of boninites is from Hickey and Frey (1982). Fields of forearc harzburgites and SSZ dunites (from Izu–Bonin–Mariana–South Sandwichforearcs) are from Parkinson and Pearce (1998) and Pearce et al. (2000).

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supports the inference of a boninitic parentage. The dunitic olivine Focontents extend from harzburgite to chromitites, in contrast to thepartial melting trend (Fig. 10A). The data suggest that the duniteenvelopes may be more consistent with a melt–rock interactionhypothesis explaining also the genesis of the boninite and high-Crchromitite (as noted below).

6.2. Melt–mantle interaction

Plots of Cr# vs TiO2 in spinels (Fig. 11A) are particularly effective indistinguishing partial melting effects from those of melt–rockinteraction (Pearce et al., 2000). This diagram shows that the Antalyalherzolitic and harzburgitic spinels approximate themelting curve of afertile MOR-typemantle (FMM). In contrast, the dunitic spinels definea different trend, showing an increase in spinel TiO2 and olivine Fovalues for equivalent Cr# (Figs. 10a and 11a), consistent with melt–mantle interaction. The simplest explanation of the Ti-enrichmenttrend is that the dunitic spinels equilibrated with boninitic melts — ofhigher TiO2 content. Their olivine Fo contents and spinel Cr# alsosupport a boninitic parentage (Fo: 94 – Cr#: 87) (Sobolev and

Danyushevsky, 1994). Therefore, olivines and spinels from the duniteenvelopes deviate compositionally from the model melting trendtowards olivine–spinel compositions of boninitic magma.

The covariation of V and Yb can also be used to discriminatebetween the effects of melt–wall–rock interaction and partial melting,and as a basis for estimating ambient oxygen fugacities (Pearce et al.,2000). Plots in Fig. 11B thus suggest that the conditions for the genesisof the Antalya spinel lherzolites fall between the experimentallydetermined FMQ and FMQ-1 melting curves, representing lessdepleted MOR lithosphere. Accordingly, many of the Antalyaharzburgites fall close to the FMQ melting curve (Pearce et al.,2000), signifying a depleted MOR lithosphere source. On the otherhand, the overlap of some of these with FMQ and FMQ+1 curves mayindicate that melt–rock interaction had occurred within the depletedMOR lithosphere. In contrast, data for the Antalya dunites appear toresemble those of the more oxidizing FMQ+1 melting regime, whichapparently represents arc lithosphere.

It has been proposed that dunites in the mantle sections of manyophiolites were formed by interaction between infiltrating melts andupper mantle peridotites, a process that results in the dissolution of

Fig. 7. Plots of major oxides (wt.%) and Mg#s vs Al2O3 (wt.%) of the AO clinopyroxenes. Field of clinopyroxenes in forearc harzburgite from Izu, Bonin, Mariana and South SandwichIslands is from Parkinson and Pearce (1998) and Pearce et al. (2000).

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pyroxene and precipitation of olivine (e.g. Dick, 1977; Boudier andNicolas, 1977; Quick, 1981; Kelemen et al., 1992; Edwards and Malpas,1995; Kelemen and Dick, 1995; Dick and Natland, 1996). Hence, the AOdunite envelopes may represent replacement of harzburgites inresponse to additional melting due to melt–rock interaction.

The (ortho-) pyroxenes of the AO harzburgites show dissolutionreaction effects. The AO dunite envelopes indicate that Opx isconsumed at the expense of Cpx. The small quantities of Cpx (0.5%)in the dunite envelopes is probably due to refertilization during highdegree hydrous melting in the spinel facies in the presence of ahydrous subduction-derived component because Cpx is expected tomelt out during high degree anhydrous melting in spinel facies

Fig. 8. Cr# vs Mg# diagram for spinels of the AO spinel lherzolites, harzburgites,dunites and chromitites. Field of forearc harzburgites from Izu–Bonin–Mariana andSouth Sandwich Island is from Parkinson and Pearce (1998) and Pearce et al. (2000),field of abyssal peridotites is from Dick and Bullen (1984), field of SSZ dunites from Izu–Bonin–Mariana–South Sandwich forearcs is from Parkinson and Pearce (1998) andPearce et al. (2000), field of boninites is from van der Laan et al. (1992) and Sobolev andDanyushevsky (1994).

(Jaques and Green, 1980; Baker and Stolper, 1994; Gaetani and Grove,1998). This interpretation is supported by the presence of primaryhydrous silicates (amphiboles) in the dunite envelopes. Accordingly,it is inferred that the AO dunite envelopes formed from the interactionbetween the hydrous subduction derived magma and the depletedhost harzburgites (Fig. 12). During the interaction, focused melt flowdissolves pyroxenes around the reaction zone and precipitates olivine.The mesh textures of the AO dunite envelopes may result from thealteration of the olivine formed from the intercumulus hydrous-liquid.

6.3. Chromitite genesis

Although podiform chromitites are common in subduction-relatedmantle settings, as represented in most, if not all, ophiolites, theiroccurrence in other tectonic settings is still subject to debate (e.g.,Roberts, 1988; Nicolas, 1989; Arai and Yurimoto, 1994; Zhou et al.,1998; Ahmed et al., 2001; Ahmed and Arai, 2002; Morishita et al.,2007). However, there is a general consensus that high-Cr chromitites(Cr#>c. 0.60) crystallize from ultramafic boninite magmas, whereashigh-Al chromitites (Cr#<c. 0.60) crystallize from less refractoryMORB-like tholeiite (Zhou and Robinson, 1994; Arai and Yurimoto,1994; Zhou et al., 1996;Matsumoto et al., 1997; Economou-Eliopouloset al., 1999; Zhou et al., 2001; Uysal et al., 2005; Morishita et al., 2007).The high-Cr podiform chromitites are thought to have formed byinteraction of boninite with variably refractory peridotite (Zhou et al.,1998). Moreover, the association of boninites per sewith the inceptionof ‘new’ subduction systems is nowwidely accepted (e.g. van der Laanet al., 1989; Stern and Bloomer, 1992; Flower, 2003; Flower and Dilek,2003). Experimental studies (e.g. Umino and Kushiro, 1989; van derLaan et al., 1989; Klingenberg and Kushiro, 1996; Falloon andDanyushevsky, 2000) suggest that the association of boniniticmagmas and Cr-rich podiform chromitites in strongly refractoryperidotite reflects unusually high temperature, low pressure (0.3–1.04 Pa), and high PH2O conditions.

Fig. 9. Mineral compositional variations for peridotites of the Antalya ophiolite. (A) Cpx Al2O3 content vs spinel Cr#; (B) Opx Al2O3 content vs spinel Cr#; (C) olivine Fo content vsCpx Mg#; (D) olivine Fo content vs Opx Mg#. The Al content of pyroxenes and spinels is sensitive to the degree of mantle melting and decreases systematically with increasingdepletion of peridotites (e.g., Dick and Natland 1996; Zhou et al., 2005). The observed decrease in Al content of both Cpx and Opx from less to more refractory peridotites (AO)matches respective increase in spinel Cr#, Cpx Mg#, Opx Mg# and olivine Fo. Mafic phase Mg#s increase with increasing depletion of peridotites.

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Manyworkers consider that boninites are found exclusively in arc–forearc terrains (e.g. Reagan and Meijer, 1984; Stern and Bloomer,1992; Bloomer et al., 1994) and represent the magmatic products ofsubduction initiation (e.g. Crawford et al., 1981; Crawford et al., 1986;Stern and Bloomer, 1992; Crawford et al., 1997; Hawkins and Castillo,1998). Alternative models for boninite genesis have assumed that 1)they occur in response to reaction of upward-migrating basaltic melts,generated from themantlewedge, with refractory lithosphericmantle(e.g. Kelemen, 1995; Zhou et al., 1996; Dare et al., 2009)— invoked as apossible explanation for ultra-refractory peridotites in forearcs(Parkinson and Pearce, 1998), or 2) that boninites represent magmasproduced during the interaction of thermally-anomalous mantle‘plumes’ with active, hydrous subduction systems (e.g. MacPhersonand Hall, 2001). It has been documented experimentally that melt–rock interaction in the upper mantle may modify the mineralogy andgeochemistry of both wall rock and percolating magmas (Fisk, 1986;Kelemen, 1990; Daines and Kohlstedt, 1994; Kelemen et al., 1995), i.e.continuous reactionmodifies percolating basaltic magmas to boniniticmagmas, dissolves the pyroxenes of the wall peridotites, and leaves adunite residue (Zhou and Robinson, 1994).

The AO podiform chromitites are high-Cr chromitites. They arecomposed of a very refractory olivine–spinel assemblage (olivine Fo:94.8–96.1, spinel Cr#: 72.2–81.2%, spinel Mg#: 62.0–68.1, spinel TiO2:0.06–0.19), in agreement with a boninitic parentage (Figs. 8, 10a and11a). Boninites contain the most Cr-rich spinels recorded, as comparedwith other known mafic terrestrial lavas, a clear indication of theirderivation fromahighly refractory (‘depleted’) peridotite (Crawford andCameron, 1985; Sobolev and Danyushevsky, 1994). Accordingly, the‘average’ parental magma source of high-Cr chromitite from the AO isalmost certainly boninitic, oversaturated with chrome spinel. The

boninitic lithologies are common in the Antalya ophiolites (e.g. BağcıandParlak, 2009). Data presented for theAntalya chromitites conform tothe notion that they are precipitated from boninitic melts derived fromthe interaction between old mantle lithosphere and subduction-relatedmelts in a supra-subduction zone setting (Fig. 12). This is also consistentwith the genesis of the dunite envelopes representing boninitic melt-extracted equivalents during the interaction. Therefore, the olivine–spinel compositions of the chromitite are similar to those of the duniteenvelopes, but considerably more refractory than those in thesurrounding harzburgites.

Antalya harzburgites hosting chromitite-bearing dunites have 10–20% modal orthopyroxene, high Cr# and low Al2O3 (Fig. 9C). Theorthopyroxenes in the host harzburgites have 0.32–0.94 wt.% Cr2O3

contents and show corrosion morphologies resulting from melt–rockinteraction. When the orthopyroxenes are dissolved (or completelydepleted) via melt–rock interaction, the chrome contents of boniniticmelts increase. Thus, during upward migration, the boninitic magmascrystallize high-Cr chromitites resulting in numerous small orebodiesin the AO harzburgites. ‘Moderately refractory’ (Cpx-) harzburgites,with ‘intermediate’ Cr#s of c. 50, are the more likely host for high-Crchromitites produced during melt–wall–rock interaction, becausethey have higher modal ratios of orthopyroxene with relatively low Alcontent (Arai, 1997). This feature may explain the abundant presenceof high-Cr chromitite deposits in to the Antalya ophiolite harzburgites.

6.4. Oxygen fugacities

Oxygen fugacities associated with ophiolite genesis can be readilycalculated from equilibria represented by coexisting olivine, pyroxeneand spinels in the peridotites. Because the dunites and chromitites

Fig. 10. Partial meltingmodeling: (A) on spinel Cr# and olivine Fo from the AO spinel lherzolites, harzburgites, dunites and chromitites; (B) on the bulk rock REE abundance of the AOspinel lherzolites; (C) on the bulk rock REE abundance of the AO harzburgites; (D) on Ti vs Yb for whole-rock data. Field of MOR peridotites is from Dick and Bullen (1984), fields ofSSZ dunites and forearc harzburgites from Izu, Bonin, Mariana and South Sandwich Islands are from Parkinson and Pearce (1998) and Pearce et al. (2000), the olivine–spinel mantlearray (OSMA) from Arai (1994). The chondrite-normalized REE abundance calculated for refractory peridotites after variable degrees of spinel facies fractional melting of N-MORmantle are annotated for comparison in (B) and (C), which is from Piccardo et al. (2007). N-MORmantle is fromMcCulloch and Bennett (1994). Line of boninites is from Hickey andFrey (1982) and Sobolev and Danyushevsky (1994). The Ti-Yb plot has calculated trends for fractional and batch melting, which are annotated from Parkinson and Pearce (1998).

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commonly lack Opx, we have used the calibration scheme of Ballhauset al. (1991), based on equilibria established between coexisting olivinesand spinels, as a basis for estimating oxygen fugacities (ƒO2), assuming an

Fig. 11. (A) TiO2 vs Cr# variation diagram for Cr-spinels of the harzburgites, dunites and chbetween partial melting trends and melt–mantle interaction trends. FMM refers to fertile Mtaken from van der Laan et al. (1992) and Sobolev and Danyushevsky (1994). (B) The V-YParkinson and Pearce (1998).

arbitrarypressureof 1 GPa. Suchcalculated ƒO2valuesdependon realisticestimates of the ferrous/ferric ratios of iron in the spinels, which can bederived using Mössbauer spectroscopy and on the basis of electron

romitites from the AO (modified from Pearce et al. (2000)). The diagram discriminatesOR-type mantle, island arc tholeiite (IAT) and boninite (BON). The field of boninite isb plot shows fractional melting trends for different oxygen fugacities annotated from

Fig. 12. (A) Spinel lherzolite formation from partial melting within a seafloor spreading (MOR) provenance (modified from Niu, 2004) (B) Interaction of boninitic melt and hostharzburgite within a supra-subduction zone (SSZ) setting. (C) A melt and wall rock interaction model for the formation of both high-Cr chromitite and the surrounding duniteenvelope in a mantle sequence of the oceanic lithosphere (modified from Zhou and Robinson (1994)). See text for detailed discussion.

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microprobe analyses (e.g. Wood and Virgo, 1989; Ballhaus et al., 1991).Here, we have calculated ƒO2 values based on stoichiometric ratios fromspinels (Table 1). The estimated oxygen fugacities are presented as logunits relative to the FMQ (fayalite–magnetite–quartz) buffer, whereΔlogƒO2 (FMQ) refers to the deviation from FMQ conditions.

Plots of ΔlogƒO2 vs spinel Cr# for the Antalya peridotites andchromitites are shown in Fig. 13, in which peridotite- and lava-hostedspinels may be clearly distinguished (Parkinson and Pearce, 1998;Parkinson and Arculus, 1999; Pearce et al., 2000; cf. Ballhaus et al.,1991; Elburg and Kamenetsky, 2007; Dare et al., 2009). This feature inturn allows distinction between mid-ocean ridge and subduction-related provenance for the spinels in the Antalya lherzolites,harzburgites, dunites, and chromitites. The spinel lherzolites withFMQ-1.01 and FMQ-0.57 are clearly of mid-ocean ridge affinity(Fig. 13). In contrast, the dunites and the chromitites, with higherestimated oxygen fugacities (FMQ+0.72 and FMQ+1.72, FMQ+0.78and FMQ+1.47, respectively) and higher spinel Cr#, fall within thesubduction-related range. On the other hand, harzburgites, with FMQ-

Fig. 13. Plot of ΔlogƒO2 (FMQ) vs spinel Cr# for spinel lherzolites, harzburgites, dunitesand chromitites from the AO. MOR-SSZ discrimination boundaries for dunites (du)(solid line) and harzburgites (hz) (dashed line) are from Dare et al. (2009). Field offorearc harzburgites from Mariana and South Sandwich Islands is from Parkinson andPearce (1998) and Pearce et al. (2000).

1.01 and FMQ+0.89, appear not to conform to either affinity, possiblyrepresenting a transition setting. Such an implied polygeneticassociation in harzburgites has been observed in both the Mariana-and South Sandwich forearcs (Parkinson and Pearce, 1998; Pearceet al., 2000) which (on the basis of FMQ-1.01 and FMQ+0.89) clearlydoes not preclude an association with subduction.

In summary, our results strongly suggest that the fO2 affinities ofthe Antalya harzburgites range from those characterizing mid-oceanridges (lower oxygen fugacities and spinel Cr#) to subduction-relatedassociations (higher oxygen fugacities and spinel Cr#), characteristicof several intra-oceanic forearcs (Fig. 13). On this basis, we infer atemporal transition from ‘oceanic’ to ‘subduction-related’ (‘proto-arc’) tectonic conditions (and their respectivemagmas) as interpretedfrom eruptedmelt products (where exposed), their associatedmantleperidotites and respective phase compositions, and interpolated fO2

conditions of the evolving upper mantle.

7. Conclusions

1. The mantle sequences of the Antalya ophiolite (AO) comprise amildly refractory mantle section dominated by spinel lherzolite, arefractorymantle section represented by harzburgites and locally astrongly refractory mantle section characterized by dunite envel-opes and podiform chromitites.

2. Whole-rock and mineral compositions, their respective modalproportions, and interpolated genetic oxygen fugacity conditionsindicate that the AO mantle sequence reflects a range of processesgiving rise to subduction-related magmatic activity – perhapsbuilding a ‘proto-arc’ in response to ‘new’ subduction initiation –

following the demise of a seafloor spreading system.3. Model calculations suggest that the AO spinel lherzolites represent

mantle residues following extraction of MORB from a spinel faciessource, whereas harzburgites are residues following ‘second-stage’extraction of primitive calc-alkaline and/or boninitic magma fromold MOR mantle lithosphere due to melt–rock interaction. Thespinel lherzolites perhaps provided a source for the harzburgites.

4. It is evident from semi-quantitative calculations of spinel lherzolitesand harzburgites that decreases in modal Cpx (c. 9.6% to 1.2%), in-creases in modal olivine (c. 68 to 85%), their matching compositional

324 Ş. Caran et al. / Lithos 114 (2010) 307–326

changes, and increase in spinel Cr# correspond to variations (between8 and 25%) inmelting degree ofmantle lithosphere due to both partialmelting and melt–rock interaction.

5. Although the spinel lherzolites and the harzburgites from the AOmay indicate mid-ocean ridge affinity, V-shaped, chondrite-normalized REE profiles of the harzburgites appear to reflectmetasomatic contamination of the mantle wedge magmaticsources by subduction-derived hydrous fluids and/or sediments.Such REE patterns resemble those of refractory (serpentinized)peridotites from modern forearcs (e.g. the South Sandwich andMariana Islands). In contrast, the fertile peridotites of ‘mid-oceanridge system appear to lack such subduction-related ‘signatures’.

6. TheAOdunite envelopes are residuesof boniniticmelt—harzburgiticwall–rock interaction. The chemistry of the spinel–olivine assem-blage in the dunites was modified by equilibration with a boniniticmelt. The wall-harzburgites around the reaction zone were changedto dunites due to melting caused by this interaction.

7. The spinel–olivine compositions of the AO ‘podiform’ chromititessuggest they crystallized from boninitic melts, oversaturated withchrome spinel, derived in part from the interaction of primitive,subduction-related, basaltic melts with refractory (lithospheric)harzburgites. Upward-migrating boninitic magmas appear to haveprecipitated numerous economically significant chromitite depos-its in the harzburgitic mantle sequences.

8. The Antalya mantle sequence, related to a southern branch ofNeotethys subject to newly-initiated subduction following thetermination of seafloor spreading, thus comprises both residues(lherzolite, harzburgite, and dunite) from variable mafic melt extrac-tions and Cr-rich chromitites precipitating from the extracted melt(boninitic).

Acknowledgements

Financial support from Suleyman Demirel University (SDUBAP,Project no: 06-M-1406) is gratefully acknowledged. We thank VolkerHoeck and an anonymous reviewer for their helpful reviews andNelson Eby for the editorial handling.

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