International Journal of Science, Technology & Management www.ijstm.com Volume No.04, Issue No. 02, February 2015 ISSN (online): 2394-1537 ON CENOZOIC VOLCANIC LAVA OF AL WAABAH CRATER (MAKLAA TAMEYA), KISHB AREA, : GEOCHEMICAL ASSESSMENT AND TECTONIC IMPLICATION

Antar A. Abdel Wahab1,2, Mohamed F. Ghoneim3, Finlay M. Stuart4, Aziz M. Kafafy1,3 1 Professor, Earth Science Research Unit, P.O. Box 888, Taif University, Taif 21974, KSA 2 Professor, Department of Geology, Faculty of Science, Kafrelsheikh University, Egypt Professor, 3Geology Department, Faculty of Science, Tanta University, Egypt Professor, 4Isotope Geosciences Unit, Scottish Universities Environmental Research Centre, Scottish Enterprise Technology Park, East Kilbride G75 0QF, UK ABSTRACT The objective is to clarify the geochemical characteristics of Al Waabah Crater; compare the volcanic assemblage with other nearby lavas, and to get better understanding of magma types and tectonic evolution. Rock sequence includes: basaltic scoria; olivine basalt and alkali olivine basalt together with subordinate andesine and scare dacite. Geochemical study using major elements, trace elements and REE's are carried out for 30 samples. Geochemical variation diagrams exhibit generally, linear to gently curved trends of chemical data. However, plots of Al2O3, K2O, Na2O and P2O5 show erratic variations.TiO2 plots form two cluster areas. Alteration effect prove that there is precludes variation in the nature of the lava and /or changes in the source plum. Andesitic rocks have generally high Ba content indicating accumulative K-feldspar. Using HFS elements on the spider diagram, shows general enrichments of Pb, Nb, Ta and depletion of Cr, Li and Y. The acidic varieties are mostly enriched in LILE (Cs, Ba & Rb). The rocks are, generally, comparable with that of OIB normalized pattern (than the other patterns). In TAS diagram they composed mostly, of basalts, hawaiite and mugearites together with more acidic varieties including andesites and subordinate dacites. The volcanic assemblage is compared with Harrat-Al Madinah using both TAS diagram and SiO2 vs K2O diagrams. It is evident that the rock plots overlap field plots of Harrat-Al Madina lavas. The volcanic exhibits wide range of magma types including alkaline, subalkaline and low – k subalkaline indicating transition magma affinity. REE's data are normalized to both chondritic normalization and ocean crust. They show parallel and moderate patterns related to both chondrite and ocean crust patterns. However, they exhibit partial depletion for both Dy and Yb. Relative enrichment is recorded for Tb and Tm. Basic varieties shows split normalized pattern practically regarding LREE. The more acidic varieties perform more or less harmonic REE pattern. Lack of Eu depletion indicates absences of subduction signature.

Keywords: Al-Waabah, KSA; Geochemistry; REE's; Subduction; Tectonic Implication

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I. INTRODUCTION

Saudi Arabia, and forming one of the largest intraplate volcanic provinces on Earth (the actual area 2 covered by volcanic rocks =180,000 km , [1]. Magmatism in this region (30 Ma – Present,) preceded, was concurrent with, and continued after the main extension that formed the Red Sea Rift. In the last decades, these rocks have been extensively studied (e.g. [2]; [3]; [4]; [5]; [6,7]; [8]; [9]; [10]; [11]. Although volcanism in southwestern Arabia has been associated with the activity of the Afar mantle plume [12]; [13, 14]; [15], the origin of the lava fields in northern Arabia is less clear and many models have been suggested to explain their origin.

Several major volcanic fields (termed harrats) occur throughout the western part of the Kingdom of Saudi Arabia (KSA), [16];[17] (Fig. 1). A series of seminal studies of these lava fields was undertaken in the late 1980s and early 1990s by the Saudi Arabian Directorate General of Mineral Resources [18, 19, 20]; [21,22]; [23]. The largest volcanic fields form a 600 km-long north south oriented trend that may be related to an underlying rift zone within the Proterozoic basement (Fig. 1). This trend, called the Makkah- Madinah - Nafud (MMN) volcanic line [21], links in the south with and Harrat Ithnayn in the north. The MNN line is a rift zone that has been extending at approximately 0.05 mm/ year for the last 10 million years.

Harrat Kishb (41 08' 299''E, 22 54' 040''N) volcanic field covers ~5,900 km2 and lies 100 km east of the MMN zone (Roobol and Camp, 1991. It lies approximately 100 km east of the MMN line, and Harrats Kura,Raha, has similar distance to the west. Al Wahbah crater (Maklaa Tameya crater a part of Harrat Kishb. The hole (Al Wahbah crater) is very large, measuring about 3.100m from north to south, 2.460 m from east to west and the depth is between 350-400 m (Fig.2a). The oval-shaped crater north – south radius, is longer than the east - west diameter, and the edges of the hole are semi-vertical, and in the top of this segment palm trees grow. It is located about 6 kilometers north of Kishb Village, and 40 kilometers north of Umm Dom Village of Taif Governorate, (about 240 km NE. of Taif city through the Hijaz – Riyadh Highway),

The bottom of the hole has topped layer white saline color resulting from the decomposition of rocks developed by the rainwater, forming a small shallow lake, due to leakage of fluids to the bottom of the clogged pores of the bottom deposits mud over the years, so the remaining water layer evaporates, either due to the hot weather or due to heat from the earth, Fig.2b.

The objective of the present study is; to clarify the geochemical characteristics of Harrat Kishb (Al Waabah Crater or MaklaaTameya); compare the volcanic assemblage of the present area with other lavas (particular Harrat –Al Madinah), and to get better understanding of magma types and tectonic evolution of the area .

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II. GEOLOGICAL SETTING

Harrat Kishb covers about 5900 km2 and its surface is at an altitude of approximately 1000 m above sea level (Fig. 2b). It is the youngest of the harrats associated with the MMN line. The crater is elliptical and orientated 340°. An orange-brown, we a kl y lithified tuff ring composed of poorly sorted material, ranging from sand-sized particles to rock fragments and mafic nodules several tens of centimeters in size, surrounds the crater for a maximum distance of 1.5 km. The laminated and dune-bedded tuff deposits are typical of pyro- clastic base-surge deposits formed by the settling of material from the radially directed blast of gas and suspended solid debris that exploded as a density flow from the crater. The deposits are 10 –15 m thick in the rim of the crater and dip and thin away radially. Numerous small crystals of olivine and augite occur in the base-surge deposits. The olivine crystals are of interest value only, but elsewhere on Harrat Kishb other tuff rings have yielded peridots (gem variety of olivine), ([24]. Harrat Kishb is a basalt 2 plateau of 5900 km located about 270 km northeast of Jeddah. The larger Harrat Rahat lies 30 km to the west. The taif – Riyadh Highway passes immediately south of Harrat Kishb and access to the northern part is from the gold mining town of Mahd ad Dhahab; the ancient pilgrim route of Darb Zubaydah gives access to the western of the Harrat. The lavas of the harrat Kishb has an age range 2 Ma to post-Neolithic. It comprises a strongly undersaturated series extending from alkali – olivine basalt to basanite, tephrite, and phonolite. The central vent zone of the harrat is characterized by abundant ultramafic nodules. Basaltic scoria cones and associated lavas are common and are the most differentiated products (phonotephrites to phonolite) from domes and dome flows. Five basaltic tuff rings are present and one of them has a well – exposed Maar Crater (Al 59 | P a g e International Journal of Science, Technology & Management www.ijstm.com Volume No.04, Issue No. 02, February 2015 ISSN (online): 2394-1537

Wahbah), [25]. Underlying the base-surge deposits are two basanite flows that formed the pre- explosion land surface.. They have a maximum thickness of about 50 m. The olivine crystals in the base- surge deposits were derived from these lavas. The lavas flowed from a cone on the north- western edge of the crater that was cut in half by the explosion to expose the throat of the volcano. Surge deposits are plastered onto the flanks of the cone. The lavas overlie Proterozoic rocks, mainly granite, that form the lower three-quarters of the crater walls.

III. PETROGRAPHY

Petrographic composition of Harrat Kishb lava is considerably undersaturated and resembles those of Harrat Kura. It includes abundance of peridotite, pyroxenite and xenoliths of mantle nodules up to 60 cm across. Some of these xenoliths are recoded with larger sizes in the bottom of Al- Wahbah maar crater A detailed study of the mineralogy of the encountered ultramfic rocks of Harrat Kishb has been carried out [26]; [27, 28].

Petrographically, the basalts comprise undersaturated series extending from basalt (hawaite to basanite, tephrite and phonolite, together with olivine basalt. The exposed rocks at Al Waabah Crater (from top to bottom) are mainly classified into: (A) basaltic scoria; and (B) basaltic lava flows (olivine basalt, basalt, and alkali olivine basalt).

3.1. Basaltic Scoria The Scoria cones and associated lavas are common and the most differentiated products (phonotephrite to phonolite) from domes and dome flows. Basaltic tuff ring is also present and has a well exposed maar crater Al Waabah. Most of the gem olivine (peridot) and augite resulted from deposition of basaltic ash and scoria that are observed at the upper most part of the Waabah crater. Generally, the scoria rocks are fine to medium grained (0.2 mm), vesicular with dark gre y to bluish grey colour. Microscopically, they composed, mainly of vesicles (up to 60% of whole rock) which are embedded in fine grained basalt groundmass. The vesicles are filled by colloidal silica, zeolites and carbonates (Fig. 3a). The basaltic groundmass is fine- grained olivine basalt with porphyritic texture (Fig. 3b). The phenocrysts c o n s i s t of olivine and pyroxene embedded in fine grained plagioclase laths (An35-55) of (<0.1mm length), olivine, clinopyroxene and opaque minerals are the main constituent of the rocks.

3.2. Basaltic Lava Flows Basaltic lava flows are classified, according their textural and mineralogical composition, into olivine basalt, basalt and alkali olivine basalt.

3.2.1. Olivine Basalt This rock is fine to medium (mm. across) grained, massive with dark grey to black colour. Microscopically, it has porphyritic texture where olivine is the main phenocryst (Fig. 3d). Olivine phenocrysts are embedded in fine grained groundmass composed of plagioclase, clinopyroxene, olivine and opaque minerals. The olivine phenocrysts occur as subhedral to euhedral crystals up to 2 mm length (Fig 3d), mostly fresh but some

60 | P a g e International Journal of Science, Technology & Management www.ijstm.com Volume No.04, Issue No. 02, February 2015 ISSN (online): 2394-1537 crystals are rimmed by iddingsite along the margin and cracks. The plagioclase is confined to the groundmass with length < 0.2mm as small laths, fresh and exhibits albite and albite Carlsbad twinning.

3.2.2. Basalt

This rock is fine to medium grained, massive with dark grey colour and tend in some places to dolerite. Microscopically, it exhibits ophitic to sub- ophitic texture, where the early crystallized plagioclase minerals are completely or partly enclosed by clinopyroxene. It is mainly composed of plagioclase, clinopyroxene a n d olivine. Minor amounts of opaque minerals occur as accessory minerals. Plagioclase (An35-40) occurs as subhedral to euhedral crystals up to 1.6 mm length, Fresh, unzoned and twinned. Clinopyroxene (augite) occur as subhedral crystals up to 1-5 mm length, fresh with pale brown colour. Olivine f o r m s subhedral to euhedral crystals with a length up to 1 mm. Iddingesite is formed around the margins of some olivine crystals and along their cracks (Fig. 3c).

3.2.3 Alkali Olivine Basalt These rocks are fine to medium grained, massive with dark grey to black colour. Microscopically, they show porphyritic texture with olivine, plagioclase and clinopyroxene phenocrysts. The groundmass consists of plagioclase, clinopyroxene, olivine and opaque minerals. The olivine phenocrysts are mostly subhedral with a length up 2.5 mm (Fig. 3e and g). Some olivine crystals are partly altered to iddingsite around the margins or along cracks. Small olivine crystals are encountered in the as fresh groundmass. Plagioclase phenocrysts(An40-45), from euhedral to subhedral up to 2mm length. They are fresh, sometimes zoned and twinned. Plagioclase groundmass is the most abundant constitute and occurs as small crystals up to 0.2mm length, fresh, unzoned. Clinopyroxene fo r ms subhedral crystals up to 1mm length. Meanwhile they form fresh crystals of the groundmass of less than 0.2 mm in length.

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IV. GEOCHEMISTRY

4.1. Analytical Methods Analyses of thirty samples were carried out using a Philips 2400 X-ray fluorescence spectrometer (XRF) at the Geological Survey of KSA. The sample preparation technique involved grinding the sample to a fine powder and then fusing the powder with a flux, so forming disc. For trace elements, the powder is pressed into a briquette using a binding agent. Sample preparation and analysis procedure are similar to those reported [29]; [30]. The major and trace element data are shown at "Table" 1.

4.2. Major Elements Variations Maklaa Tameya Crater (MTC) have SiO2 contents in the range of 42.1-65.43 wt.% with wide Ala2O3 range

(13.88-17.41), Fe2O3 (4.83-15.16), TiO2 (0.46-3.1), CaO (2.51-13.83), MgO (2.15-10.69), Na2O (0.8-

5.56) ) and K2O (0.06-2.54) wt.%. Figures (4 and 5) show major elements variation diagram for MTC rock verities using number (mg) and MgO as an index of differentiation. The plotted data are generally exhibit linear to gently curved trend. However, plots of Al2O3, K2O and Na2O show erratic variations. TiO2 plots form two cluster areas (Figs. 4e and 5g). Deviation of the plot from descending line could suggest, either late alteration or else, independent generation.

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4.3. Trace Elements Variations Trace elements are, mostly, display systematic variations in a suite of co genetic volcanic. Zr represent good indicator of degree of fractionation and is apparently immobile under weathering conditions [31]; [32] and [33]. Variations of Zr among other trace elements show that there is no clear variation trend (Figures 6 and 7).. However, there are two main clusters of the plots above the value of 200 ppm of Zr (Figs. 6 and 7g). That precludes variation in the nature of the extrusive MTC lava and/or changes in the source plum. The compatible elements Both Ni (22.2-312.09 ppm) and Cr (11.35-340.7 ppm) contents show wide variations range "Table 1". They exhibit two distinctive clusters on Zr vs Ni –Cr (Fig. 6). Abundances of the incompatible trace elements generally increase from basalts to acidic verities. The LILE like Ba (15.46-920.29 ppm), Sr (125.48-1873.76) and Li (6.05-40.25) form two pronounced clusters (Fig. 6). The highest Ba contents characterize the highly evolved rocks of sample of andesitic composition (no. 18 & 19). High Ba content implies accumulative K- feldspar.

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HFSE Contents Zr (57.28-377.36 ppm), Nb (10.36-73.05), Hf (1-8.35) ppm), Ta (1.03-10.03), and Y (10.1-24.31 ppm) show clusters rather than regular correlation with MgO and Zr (Fig. 7). On spider diagram, the analyzed trace elements are normalized to chondrite and oceanic crust, [34] (Fig. 8). Their patterns shows general enrichments of Pb , Nb, Ta and depletion of Cr ,Li ,and Y. The acidic verities are mostly enriched in LILE (Cs, Ba & Rb). However the pattern is, generally, comparable with that of ocean crust normalized diagram than the other normalization patterns.

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4.4. Variation of Normative Composition CIPW normative compositions are calculated and listed in Table (1). D.I is currently used as differential index showing trends of variation of the normative minerals during magmatic process. D.I. (Sum of weight % of normative quartz, orthoclase, albite, nephelene, Lucite, kalsilite, [35] versus normative compositions is plotted in Figure (9). It indicates that the basic varieties are mostly undersaturated (free of Q) and they contain Ne (nephelene) up to 10.8 wt% (Fig. 9d). Olivine normative ranges between 4.6-12.0 wt % (Table 1). It is of foreseterite type (Mg olivine) (Fig. 9i and j). The normative hyperthene is only recorded in more acidic verities (Fig. 9h). Both normative magnetite (Mg) and hematite (Hm) show linear conversation with D.I (Fig. 9k and m). Ap normative classify the present rocks into two groups (Fig. 9). Generally, D.I. confirms that the study rocks are cluster into two groups, which is already recorded using both major and trace elements variations. However, the overall scatter on the diagram, within the individual cluster, may be attributed to intravolcanic variations. Defining relative coherent are shown within the same cluster (basic and acidic varieties). Further, the combinations of scattered trends on variation diagram (Fig.9) could indicate that several processes have influenced the whole composition of the studied rocks

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4.5. Alteration Effects. Major elements are tested for alteration using [36] diagrams (Fig. 10). It shows that the general trend of the plotted samples lie close to the solid lines defined unaltered rock zone. This preclude the erratic variation of some major elements of (Figs.4 and5) could not attributed to selective alteration.

2.5 3.5 Log(CaO/K2O) 3 2 log(SiO2/K2O) 2.5 2 1.5 1.5 1 1 0.5 0 0.5 0 0.5 1 1.5 2 2.5 3 log( Al2O3/K2O) 0 0 0.5 1 1.5 2 2.5 3 log( Al2O3/K2O)

Fig. 10. Logarithmic oxides ratio for MIC volcanics lie within unaltered zones, {36} (logCaO/K2O) vs (logAl2O3/K2O) at left, (logSiO2/K2O) vs (logAl2O2O3/K2O)at right.

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4.6. Classification and Magma Type MTC volcanics have wide SiO2 contents (42.10-65.43 wt%) with average 49.12 wt%. they show general increase with total alkalies (Na2O+K2O) with positive trend (Figs. 11, 12, 13 and 14). In TAS classification diagram most of the studied rocks are basalts, hawaiite and mugearites together with more acidic varieties including andesites and few dacites (Figs. 11 and 13). MTC volcanics assemblage are compared with Harrat-El Fahda, Jordon, Harrat Rahat, Saudi Arabia [18] and Harrat Al Madinah, Saudi Ara[37]. In both TAS diagram [38] and SiO2 vs K2O diagram [39]. It is evident that the studied rocks plots overlap points these Harrat (Figs. 13 and 14). MTC volcanics exhibit wide range of magma types including alkaline, subalkaline and low–k subalkaline which indicates transition magma affinity (Figs. 12 and 14).

4.7. Rare Earth Elements, REEs

REEs and their ratios are recalculated and listed in Table (1). They show that total contents of REEs of MTC have wide variation range (55.5-274.7 ppm) with LREE la ranges (8.23-64.4 ppm) and HREE Lu (1.11-2.06 ppm). La ranges from 34.42 to 271.81times the chondrite, whereas HREE (e.g. Lu) is clustering at lower values of 43.7 to 61.10 times chondrite. These values indicate moderately fractionation.

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Calculate (La/LU)n (0.6-3.8 except sample 7 have5.98), values of (La/Sm)n (1.23-3099) and range of (Gd/Yb)n (1.7-4.29) all indicate moderate fractionation. Data of MTC volcanic are normalized to both chondrite and ocean crust (Fig. 15). Generally, they show parallel and moderate pattern coincide for both chondrite and ocean crust patterns. However, they have partial depletion of Dy and Yb. Relative enrichment is recorded for Tb and Tm. The normalized patterns for basic verities of MTC are spitted, particularly for LREE (Fig. 15). Meanwhile, the normalized diagram exhibits more or less harmonic REE pattern for more acidic varieties. Lack of Eu depletion indicates absences of subduction signature. In an attempt to evaluate the suggestion of two clusters compositions of MTC volcanic we use (Sm/Nd) n Vs (La/Lu )n diagram (Fig. 16). The ratios are relatively insensitive to fractionation to different degree of melting. The plots on the diagram favor two clusters trends at (Sm/Nd)n ratio = 2 (Fig. 16). It reflects magma production from heterogeneous mantle [40] or else, contamination during evolution. That will be discussed in details in second part of the given project.

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4.8. Tectonic Setting Several major and trace elements and their ratios variations diagrams are constructed to consider the tectonic environments and discriminate between them. The high Nb/Y and relative Zr contents of MTC basic volcanics are reflected in Nb-Zr-Y tectonic setting diagram of [41] the plotted rocks favor within plate alkali basalt (fields A1 & AII) (Fig.17). The Ti-Zr-Y diagram is the most effectively discriminates between within –plate basalts (ocean island or continental flood basalt) and other basaltic types [32].

Data o MTC basic varieties are plotted in field D of within –plate basalt (Fig.18) confining with other cited diagrams. Meanwhile, the MTC acidic varieties indicate Calc- alkali magma type (field C of Pearce and Cann, Op.cit). The ratio of Zr/Y plotted against the fractionation index of Zr proved a good tool to discriminate between basalts from ocean- island arcs [42], MORB and within- plate basalts. MTC rocks plots show within plate basalts (field A) (Fig.19). For further identification of tectonic setting of volcanic rocks a discrimination diagram based on the immobile HFSE (Th-Hf-Ta and Nb) was proposed [43]. On using the diagram, MTC basic varieties plot in field C confirming similarities with within- plate volcanics (Fig. 20).

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V. SUMMARY AND CONCLUSION

A series of Cenozoic alkaline volcanics explosions are located in western part of the Kingdom of Saudi Arabia termed as Harrah. They form about 600 km-long of north south trend. It is called the Makkah- Madinah - Nafud (MMN) volcanic line [21]. Harrat Kishb of the present study lies approximately 100 km east of the MMN line. Regarding their origin, several suggestions have been proposed i.e. (1) lithospheric rifting mobilizing old fossil plume head material beneath the subcontinental lithosphere [44]; (2) progressive lithospheric thinning tapping lithospheric (fossil plume material) to asthenospheric [45]; [5]; (3)melting of hydrous mantle lithosphere by heat conduction from sub-lithospheric anomalously hot mantle [46]; [9], (4) A separate mantle plume existing underneath northern Arabia [47]; [48], (5) Northwestward channeling of hot Afar plume material [20]; [6]. Magmatism in this

70 | P a g e International Journal of Science, Technology & Management www.ijstm.com Volume No.04, Issue No. 02, February 2015 ISSN (online): 2394-1537 region (30 Ma-Present,) preceded, was concurrent with, and continued after the main extension that formed the Red Sea Rift. Away from studying the pathogenesis of these outcrops, it is vital to assign their geochemical characteristics, which formulate the objective of the present study. The following could represent the main geochemical characteristics of Harrat Kishb. Petrochemical composition of Harrat Kishb volcanics includes basalts, hawaiite and mugearites together with more acidic varieties including andesites and few dacites. The basaltic varieties are mostly undersaturated and they contain Ne (nephelene) up to 10.8 wt %. Despite of the plotted data, on chemical variation diagrams, exhibit generally linear to gently curved trend, TiO2 plots constitute two cluster areas. Deviation of the plot from descending line could suggest, either late alteration or else, independent generation. Trace elements show that there is no clear variation trend among most of plotted elements. Rather than, they display two main clusters of the plots above the value of 200ppm of Zr. That precludes variation in the nature of the extrusive MTC lava and/or changes in the source plum. This variation, is, in turn, cannot attributed to selective alteration. Harrat Kishb volcanics show wide range of magma types including alkaline, subalkaline and low–k subalkaline which indicates transition magma affinity. They are similar to Harrat- El Fahda, Jordon, Harrat Rahat, Saudi Arabia. The REE's normalized patterns for basic verities are spitted, particularly for LREE Meanwhile, the normalized diagram exhibits more or less harmonic REE pattern for more acidic varieties. Lack of Eu depletion indicates absences of subduction signature. On (Sm/Nd)n Vs (La/Lu)n diagram implies two clusters trends at (Sm/Nd)n ratio = 2 which in turn, reflects magma production from heterogeneous mantle . Trace elements and their ratios variations diagrams favor within plate alkali basalt for the studied volcanics.Identification of tectonic setting of the present volcanic rocks on discrimination diagram based on the immobile HFSE (Th-Hf-Ta and Nb) it indicates that basic varieties plot in Field of within- plate volcanic Finally, it worth mention that studding of mineral chemistry is must to improve compositional and physical-chemical variations involved during magma generation. This will be the subject of further work.

VI. ACKNOWLEDGEMENTS

This paper is a part of the research project 3606-435-1 funded by Taif University. The authors express their sincere thanks to His Excellency the Taif University Chancellor, Professor Abdel Elah Banaja, for continuous support and encouragement during all steps of research since its inception. Thanks must go to Dr. Fareed Felemban, the Vice President for Higher Studies and Scientific Research, and Dr Abdallah Al Harthy, the Dean of Scientific Research for financial support. We thank the support services people at Taif

REFRENCES

[1] Coleman, R.G., Gregory, R.T., Brown, G.F., 1983. Cenozoic volcanic rocks in Saudi Arabia. Saudi Arabian Deputy Minister of Mineral Resources, Open File Report, USGS-OF93.

[2] Almond, D.C., 1986. The relation of Mesozoic–Cenozoic volcanism to tectonics in the Afro- Arabian dome. Journal of Volcanology and Geothermal Research 28, 225–245.

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[18] Camp, V.E., Roobol, M.J., 1989. The Arabian continental alkali basalt province: Part I, Evolution of HarratRahat, Kingdom of Saudi Arabia: Geological Society of America Bulletin, 101, 71-95. [19] Camp, V.E., Roobol, M.J., 1991. Geological map of Cenozoic lava field of HarratRahat, Kingdom of Saudi Arabia: Saudi Arabian Deputy Ministry for mineral Resources Geosciences Map GM-123, scale 1:250,000 with text. (Previously released as Saudi Arabian Deputy Ministry for mineral Resources Open File Report DGMR-OF- 07-9-91p. 1987). [20] Camp, V.E., Roobol, M.J., 1992. Upwelling asthenosphere beneath western Arabia and its regional implications. Journal of Geophysical Research 97, 15255–15271. [21] Camp, V.E., Roobol, M.J., Hooper, P.R., 1991. The Arabian continental alkali basalt province: Part II, Evolution of HarratKhaybar, Ithnayn, and Kura, Kingdom of Saudi Arabia. Geological Society of America Bulletin 103, 363-391. [22] Camp, V.E., Roobol, M.J., Hooper, P.R., 1992. The Arabian continental alkali basalt province: Part III, Evolution of HarratKishb, Kingdom of Saudi Arabia. Geological Society of America Bulletin 103, [23] Roobol, M.J., Camp, V.E. 1991. Geological map of the Cenozoic lava fields of HarrasKhayba. Ithnayen and Kurs, Kingdom of Saudi Arabia: Saudi Arabian Directorate General of Mineral Resources Geosciences Map Gm-131, scale 1:250 000 with text. (Previously released as Saudi Arabian Directorate General of Mineral Resources Open – File report DGMR – OF – 10 – 1. 88p., 1989).379-396.

[24] Abdel Wahab, Antar, Abul Maaty, M. A. Stuart, F.M., Awad, Hesham and Kafafy, Aziz M. 2014) : The geology and geochronology of Al Wahbah maar crater, Harrat Kishb, Saudi Arabia. Quaternary Geochronology, v.21, p.70- 76. [25] Roobol, M., J., Simsim, M., Abdul-Hafez, K., and Tayeb, O., 1999, Basalt as an industrial rock-3.Harrat Kishb: Quarry sites at Taif, Riyadh and Ad dammam, Technical report, Brgm0 Tr-98-13, Ministry of Petroleum and Mineral resources Deputy Ministry for Mineral resources, Jeddah, Kingdom of Saudi Arabia, AH1419, AD, 1999. [26] Vaughan, A.W., 1985, Mantle xenoliths from Harrat al Kishb, Western Saudi Arabia: EOS (Transactions of the American Geophysical Union) v. 66, p.1114. [27] McGuire, A.V., 1988a, Petrology of mantle xenoliths from Harrat al Kishb: the mantle beneath western Saudi Arabia : Journal of petrology , v. 29, p. 73-92. [28] McGuire, A.V., 1988b, the mantle beneath the Red Sea margin: xenoliths from western Saudi Arabia : Tectonophysics, v. 150, p. 101-119. [29]. Rollinson, H., 1993, Using Geochemical Data: Evaluation, Presentation, Interpretation: John Wiley, NY.

[30] Fitton, G., 1997, X-Ray fluorescence spectrometry, in Gill, R. (ed.), Modern Analytical Geochemistry: An Introduction to Quantitative Chemical Analysis for Earth, Environmental and Material Scientists: Addison Wesley Longman, UK. [31] Floyd, P.A., Winchester, J.A., 1975. Magma type and tectonic setting discrimination using immobile elements. Earth and Planetary Science Letters, 27, 211-218. [32] Pearce, J.A., Cann, J.Y, 1973, Tectonic setting of basic volcanic rocks determined using trace elements analyses. Earth and Planetary Science Letters, 19, 290-300.

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[33] Weaver, B.L., Tarney, J. 1981. Geochemistry of Archaean crustal components. (abs) Geophysical. Journal of the Royal Astronomical Society 65, 246. [34] Thompson, R.N., 1982, British Tertiary volcanic province. Scottish Journal of Geology, v. 18,p. 49–107. [35] Thornton and Tuttle, 1960, Chemistry of igneous rocks I: Differentiation Index, American Journal of Science, v. 258, p. 664-684 [36] Geringer,G.J.; Botha,B.,V..;Petorius,J.J. and Ludick,D.J. 1986. Calc- alkaline volcanicsm along the eastern margin of the volcanic arc. Precambrian Res. 33:139-170. [37] Moufti, M.R., Moghazi, A.M., Ali, K.A., 2012. Geochemistry and Sr–Nd–Pb isotopic composition of the Harrat Al-Madinah Volcanic Field, Saudi Arabia. Gondwana Research 21, 670-689. [38] Le Bas, M.J. , Le Maitre, R. W., Streckeisen, A., and Zanettin, B., 1986, A chemical classification of volcanic rocks based on the total alkali-silica diagram: Journal of Petrology, v. 27, pt. 3, p.745- 750. [39] Middlemost, E.A.K., 1975. The basalt clan. Earth Science Reviews 11, 337–364. [40] Nicholis, I.A., Whitford, D.J., Hariris, K.L., and Taylor, S.R., 1980. Variation in the geochemistry of mantle sources for tholeiitic and calc alkaline mafic magmas, western Sunda volcanic arc, Indonesia. Chemical Geology, 30, 177-199. [41] Meschede, M., 1986. A method of discriminating between different types of mid-oceanic ridge basalts and continental tholeiites with the Nb--Y diagram. Chemical Geology, 56, 207-218. [42] Pearce, J.A., Norry, M.J, 1979, Petrogenesis implications of Ti, zr, and Nb variations in volcanic rocks. Contributions to Mineralogy and Petrology, 69, 33-47. [43] Wood, D.A., 1980, The application of a Th-Hf-Ta diagram to problems of tectono magmatic classification and to establishing the nature of crustal contamination of basaltic lavas of the British Tertiary volcanic povince. Earth and Planetary Science Letters, 50, 11-30. [44] Stein, M., Hofmann, A.W., 1992. Fossil plume head beneath the Arabian lithosphere? Earth and Planetary Science Letters 114, 193–209. [45] Bertrand, H., Chazot, G., Blichert-Toft, J., Thoral, S., 2003. Implications of widespread high-m volcanism on the Arabian Plate for Afar mantle plume and lithosphere composition. Chemical Geology 198, 47–61 [46] Stein, M., Navon, O., Kessel, R., 1997. Chromatographic metasomatism of the Arabian– Nubian lithosphere. Earth and Planetary Science Letters 152, 75–91. [47] Moufti, M.R., Hashad, M.H., 2005. Volcanic hazards assessment of Saudi Arabian Harrats: geochemical and isotopic studies of selected areas of active Makkah– Madinah–Nafud (MMN) volcanic rocks. Final project Report (LGP-5-27) submitted to King Abdulaziz City for Science and Technology, Riyadh, Saudi Arabia. 401 pp. [48] Chang, S.-J., Lee, S., 2011. Mantle plumes and associated flow beneath Arabia and East Africa. Earth and Planetary Science Letters 302, 448–454.

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TABLE (1) MAJOR AND TRACE ELEMENTS AT ALWAABAH, MAKLAATAMEYA, KISHB AREA

SP.NO. 1 2 3 4 5 6 7 8 9 10

MAJOR OXIDES (WT %)

SIO2 46.74 46.4 43.3 43.5 43.8 43.1 44.12 50.86 44.39 44

AL2O3 15.38 15.19 14.77 14.62 14.63 14.02 14.89 16.26 14.58 14.55

FE2O3 12.19 12.45 14.44 14.73 14.53 14.17 13.01 11.01 13.88 15

TIO2 2.33 2.45 3.03 3.1 3.06 2.96 2.45 0.89 2.85 2.74

CAO 7.43 7.53 8.25 8.6 8.51 8.69 8.68 13.83 8.41 8.02

MGO 6.47 6.67 7.51 7.61 7.67 8.76 6.85 2.82 7.57 7.3

NA2O 5.09 5.22 4.42 4.64 4.54 3.81 4.13 0.8 4.69 4.62 K2O 1.8 1.71 1.59 1.62 1.36 1.6 1.42 0.06 1.63 1.66

MNO 0.19 0.19 0.19 0.21 0.21 0.2 0.19 0.18 0.21 0.21

SO3 < 0.05 < 0.05 < 0.05 < 0.05 < 0.05 < 0.05 0.72 < 0.05 < 0.05 < 0.05 P2O5 0.71 0.73 0.83 0.84 0.86 0.76 0.78 0.22 0.82 0.86 L.O.I 1.55 0.85 1.37 0.37 0.55 1.59 2.63 2.66 0.33 0.84

NORMATIVE COMPOSITION Q 0 0 0 5.25 6.66 0 0 1.05 15.24 12.91 C 0 0 0 0 0 0 0 0 0 0

OR 10.83 9.92 10.3 10.26 4.06 9.53 10.93 9.14 9.46 15.9

AB 29.01 23.07 17.49 30.75 24.15 37.48 28.43 28.83 29.84 29.51

AN 14.01 14.18 14.16 26.82 30.64 25.33 12.97 27.8 24.84 20.23

NE 7.99 8.88 10.02 0 0 0 9.62 0 0 0

LC 0 0 0 0 0 0 0 0 0 0

AC 0 0 0 0 0 0 0 0 0 0

NS 0 0 0 0 0 0 0 0 0 0

DI 14.97 16.28 18.94 4.18 5.65 5.05 15.31 10.55 1.72 4

DIWO 8.04 8.74 10.17 2.25 3.03 2.71 8.22 5.67 0.92 2.15

DIEN 6.93 7.54 8.77 1.94 2.61 2.34 7.09 4.89 0.8 1.85

DIFS 0 0 0 0 0 0 0 0 0 0

HY 0 0 0 10.63 15.65 8.73 0 10.98 9.98 8.04

HYEN 0 0 0 10.63 15.65 8.73 0 10.98 9.98 8.04

HYFS 0 0 0 0 0 0 0 0 0 0

OL 6.66 7.63 9.66 0 0 1.39 6.26 0 0 0

OLFO 6.66 7.63 9.66 0 0 1.39 6.26 0 0 0

OLFA 0 0 0 0 0 0 0 0 0 0

MT 0.63 0.69 0.66 0.58 0.65 0.59 0.63 0.64 0.51 0.45

HM 11.96 14.68 14.06 9.91 10.84 10.22 11.92 9.73 7.31 7.65

IL 0 0 0 0 0 0 0 0 0 0

AP 1.58 1.9 1.74 0.64 0.64 0.67 1.59 0.48 0.41 0.49

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C_I 22.26 24.6 29.26 15.4 21.94 15.76 22.2 22.17 12.21 12.49 D_I 47.83 41.87 37.8 46.27 34.87 47.01 48.98 39.02 54.53 58.32

TRACE ELEMENTS (PPM)

SC 17.9 18.52 17.82 17.09 18.33 19.59 19.34 27.15 15.95 17.21 Y 21.31 21.14 22.05 22.8 22.4 18.95 17.83 16.54 18.2 20.32

AG 1.05 1.15 1.15 1.33 <1 <1 1.17 <1 <1 1.44

LI 12.88 13.1 7.8 6.21 10.25 6.58 11.83 24.55 7.9 11.74

BE 4.33 4.26 3.3 3.59 3.53 3.26 3.49 1.32 3.04 3.11 V 186.69 204.06 211.31 213.04 213.03 207.39 168.97 245.03 165.19 172.67

CR 127.5 132.87 146.67 167.96 141.3 175.46 165.86 11.93 142.86 170.32

CO 52.07 52.83 58.69 53.18 59.43 57.98 51.27 27.57 46.92 55.16

NI 104.68 110.2 118.66 122.15 114.92 139.36 105 22.42 101.55 126.25

CU 48.45 51.5 46.89 47.97 49.51 65.77 52.36 7.48 43.03 59.87

ZN 118 130.41 102.68 101.17 97.69 82.51 81.99 81.84 95.1 106.39

GA 24.96 23.17 22.93 16.2 23.14 20.69 22.53 26.19 18.08 24.16

GE <1 <1 <1 <1 <1 1.52 12.15 3.25 1.36 <1

AS <5.5 <5.5 <5.5 <5.5 <5.5 <5.5 <5.5 <5.5 <5.5 <5.5

SR 934.5 934.5 950.34 975.82 845.25 919.86 1157.81 1873.76 838.39 944.62

ZR 318.31 318.31 377.36 310.66 259.79 265.36 350.67 92.91 301.96 345.24

NB 61.06 61.06 62.13 56.62 38.84 63.56 56.65 11.02 47.95 56.02

MO 2.38 2.38 <2 <2 <2 <2 <2 <2 <2 <2

CD <0.5 <0.5 0.59 <0.5 0.64 <0.5 <0.5 <0.5 <0.5 <0.5

SN <10 <10 <10 <10 <10 <10 <10 <10 <10 <10

SB <10 <10 <10 <10 <10 <10 <10 <10 <10 <10

BA 313.44 313.44 308.6 305.72 255.68 308.98 332.08 15.46 256.61 273.81

HF 7.44 7.44 7.44 7.36 6.04 4.75 4.33 1.28 6.02 6.8

TA 6.3 6.3 8.62 7.52 6.34 4.89 6.84 2.88 6.81 5.16 W <5 <5 <5 <5 <5 <5 <5 <5 <5 <5

PB 16.35 1864.19 16.15 15.58 16.84 14.41 20.8 27.65 1894.51 16.31

BI <10 <10 <10 <10 <10 <10 <10 <10 <10 <10

TH 6.22 2.76 3.66 2.95 4.02 3.54 2.61 1.56 1.1 3.85 U <5 <5 <5 <5 <5 <5 <5 <5 <5 <5

RARE EARTH ELEMENTS (PPM)

LA 60.15 60.88 56.42 38.6 60.6 56.03 63.88 10.45 52.15 56.57

CE 87.9 87.62 84.53 92.72 89.99 80.84 89.06 15.68 76.29 82.6

PR 6.11 6.58 6.01 <5.5 6.63 5.51 <5.5 <5.5 5.91 <5.5

ND 48.26 47.26 51.54 46.53 52.6 51.21 52.25 18.77 42.07 47.74

SM 11.59 12.61 13 10.87 12.94 11.88 10.08 3.92 11.14 12.98

EU <1 <1 <1 <1 <1 <1 <1 <1 <1 <1

GD 11.57 12.68 12.98 17.67 13.21 13.65 13.47 6.84 9.02 14.12

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TB 4.93 5.63 6.65 5.13 6.31 6.16 4.94 3.71 4.97 6.08

DY 7.29 7.63 8 6.18 8.01 7.59 7.33 4.72 6.66 7.7

HO <1 <1 <1 <1 <1 <1 <1 <1 <1 <1

ER 12.31 13.23 14.83 8.89 15.04 15.25 12.77 5.47 10.21 12.81

TM 3.37 3.61 4.13 2.87 4.43 3.81 2.6 1.26 3.22 3.73

YB 2.94 3.12 2.9 2.57 2.92 2.58 2.6 2.91 2.45 2.68

LU 1.61 2 2.02 1.17 2.02 2.06 1.11 1.55 1.48 1.96

TOTAL REE 258.03 262.85 263.01 233.2 274.7 256.57 260.09 75.28 225.57 248.97

LREE TOTAL 214.01 46.77 30.65 29.79 28.83 27.82 43.5 17.33 42.54 36.21 HREE 44.02 47.9 51.51 44.48 51.94 51.1 44.82 26.46 38.01 49.08

BA/LA 5.21 5.15 5.47 7.92 4.22 5.51 5.2 1.48 4.92 4.84

NB/LA 1.02 1 1.1 1.47 0.64 1.13 0.89 1.05 0.92 0.99

LA/YB 20.46 19.51 19.46 15.02 20.75 21.72 24.57 3.59 21.29 21.11

ZR/NB 5.21 5.21 6.07 5.49 6.69 4.17 6.19 8.43 6.3 6.16

(LAN/LU)N 3.88 3.16 2.9 3.42 3.11 2.82 5.98 0.7 3.66 3

(LA/SM)N 3.27 3.04 2.73 2.24 2.95 2.97 3.99 1.68 2.95 2.74

(GD/YB)N 3.19 3.29 3.63 5.57 3.67 4.29 4.2 1.91 2.98 4.27

(LA/LU)N 3.88 3.16 2.9 3.42 3.11 2.82 5.97 0.7 3.66 3 LRRE/HRRR 4.861654 0.976409 0.59503 0.669739 0.555064 0.544423 0.970549 0.654951 1.119179 0.737775

TABLE (1) CONTINUE

SP.NO. 11 12 13 14 15 16 17 18 19 20

MAJOR OXIDES (WT %)

SIO2 43.42 50.69 49.69 48.89 47 49.41 57.32 56 56.3 61.95

AL2O3 14 16.84 16.06 17.41 15.6 16.87 16.04 15.2 15.5 16.04

FE2O3 14.42 9.81 10.86 10.09 12.23 9.81 7.38 7.52 7.29 5.33

TIO2 2.97 0.92 1.03 0.96 2.32 0.78 0.68 0.78 0.83 0.46

CAO 8.65 6.5 7.68 6.43 7.37 8.29 5.46 5.08 4.6 2.96

MGO 8.97 4.78 7.03 4.96 6.35 6.12 4.15 3.74 3.81 2.49

NA2O 4.23 3.46 2.75 4.21 5.41 3.29 3.4 3.3 3 5.56 K2O 1.73 1.65 0.66 1.53 1.83 1.49 1.54 2.54 2.43 1.57

MNO 0.2 0.17 0.19 0.17 0.19 0.19 0.15 0.13 0.13 0.11

SO3 < 0.05 < 0.05 < 0.05 < 0.05 < 0.05 < 0.05 < 0.05 < 0.05 < 0.05 < 0.05 P2O5 0.79 0.28 0.28 0.29 0.72 0.21 0.18 0.21 0.27 0.15 L.O.I 0.47 4.58 3.59 4.8 0.44 3.22 3.18 4.7 5.24 2.78

NORMATIVE COMPOSITION Q 15.6 0 14.44 0 0 0 4.51 15.53 17.19 0 C 0.14 0 0.13 0 0 0 0 0 0 0

OR 15.26 10.26 9.61 10.03 9.76 4.06 12.16 13.12 12.63 9.52

AB 26.93 28 48.63 28.97 23.58 12.51 25.57 36.03 34.71 25.23

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AN 22.57 13.13 14.3 14.56 13.35 26.05 30.11 20.24 20.38 14.22

NE 0 9.09 0 5.61 7.72 6.1 0 0 0 7.52

LC 0 0 0 0 0 0 0 0 0 0

AC 0 0 0 0 0 0 0 0 0 0

NS 0 0 0 0 0 0 0 0 0 0

DI 0 15.89 0 14.24 13.76 25.05 3.49 1.99 2.23 15.71

DIWO 0 8.54 0 7.65 7.39 13.45 1.88 1.07 1.2 8.43

DIEN 0 7.36 0 6.59 6.37 11.6 1.62 0.92 1.03 7.27

DIFS 0 0 0 0 0 0 0 0 0 0

HY 10.12 0 6.44 0 0 0 11.61 5.21 4.95 0

HYEN 10.12 0 6.44 0 0 0 11.61 5.21 4.95 0

HYFS 0 0 0 0 0 0 0 0 0 0

OL 0 6.69 0 7.61 12.01 11.36 0 0 0 7.83

OLFO 0 6.69 0 7.61 12.01 11.36 0 0 0 7.83

OLFA 0 0 0 0 0 0 0 0 0 0

MT 0.45 0.63 0.37 0.66 0.66 0.58 0.62 0.47 0.47 0.72

HM 7.43 12.2 5.26 14.01 14.4 12.38 10.08 6.17 6.31 14.75

IL 0 0 0 0 0 0 0 0 0 0

AP 0.63 1.62 0.34 1.76 1.9 0.52 0.83 0.56 0.47 1.73 C_I 10.57 23.22 6.81 22.5 26.44 36.98 15.72 7.67 7.65 24.26 D_I 57.79 47.35 72.69 44.61 41.05 22.67 42.23 64.68 64.53 42.27

TRACE ELEMENTS (PPM)

SC 20 34.47 38.77 37.36 17.94 35.4 26.07 26.04 22.77 13.99 Y 21.49 11.01 16.38 12.15 20.32 12.95 16.86 17.54 20.33 10.1

AG 1.31 <1 <1 <1 1.06 <1 <1 <1 <1 <1

LI 7.44 39.03 34.07 37.32 17.78 22.21 17.87 26.8 40.25 18.32

BE 3.06 1.55 1.55 1.35 4.11 1.19 1.06 1.09 1.45 <1 V 217.02 292.06 282.34 311.62 162.01 233.63 156.36 166.72 142.23 101.31

CR 205.13 11.35 88.37 11.46 107.48 45.6 35.67 32.92 38.9 18.4

CO 62.15 39.47 49.59 39.3 47.64 44.72 33.72 32.74 29.4 24.28

NI 153.82 23.57 55.57 24.56 100.8 46.39 29.83 30.87 28.76 24.52

CU 77.9 107.53 129.92 98.93 65.06 113.99 50.45 67.86 39.38 44.46

ZN 111.27 68.55 89.47 79.49 94.2 90.54 132.89 64.79 59.24 56.47

GA 21.41 23.43 21.07 22.87 26.05 21.04 18.64 21 19.4 15.83

GE <1 <1 <1 <1 <1 <1 1.2 <1 <1 2.87

AS <5.5 <5.5 <5.5 <5.5 10.49 8.54 10.52 15.82 <5.5 6.6

SR 945.95 569.92 478.15 611.68 911.21 432.25 431.71 479.08 342.89 200.57

ZR 281.7 64.27 81.77 57.28 306.3 75.95 114.87 125.15 121.37 73.22

NB 73.05 12.58 10.66 11.91 60.16 10.41 27.92 10.36 <10 <10

MO <2 <2 <2 <2 4.08 <2 <2 <2 <2 <2

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CD <0.5 <0.5 <0.5 0.52 <0.5 <0.5 <0.5 <0.5 <0.5 <0.5

SN <10 <10 <10 <10 <10 <10 <10 <10 <10 <10

SB <10 <10 <10 <10 <10 <10 <10 <10 <10 <10

BA 305.5 562.62 230.28 557.75 323.64 313.09 721.18 920.29 499.76 390.73

HF 5.9 <1 2 <1 6.98 <1 2.78 2.17 3.13 1.86

TA 9.76 1.5 1.22 1.97 6.28 4.97 10.3 4.45 4.91 4.62 W <5 <5 <5 <5 <5 <5 <5 <5 <5 <5

PB 17.41 17.69 1335.69 16.07 16.56 1038.39 16.74 16.56 12.02 15.98

BI <10 <10 <10 <10 <10 <10 <10 <10 <10 <10

TH 4.79 1.55 <1 <1 5.61 <1 2.6 2.17 2.29 1.92 U <5 <5 <5 <5 <5 <5 <5 <5 <5 <5

RARE EARTH ELEMENTS (PPM)

LA 55.59 8.99 11.09 10.36 64.42 10.75 14.56 14.74 16.58 10.84

CE 80.57 13.78 16.92 15.87 84.58 15.22 20.91 22.03 22.76 15.52

PR 5.75 <5.5 <5.5 <5.5 6.36 <5.5 <5.5 <5.5 <5.5 <5.5

ND 52.08 14.26 16.83 17.02 50.38 17.4 18.53 19.18 21.63 12.11

SM 12.59 3.51 4.62 4.13 10.86 3.87 4.42 4.62 5.58 3.07

EU <1 <1 <1 <1 <1 <1 <1 <1 <1 <1

GD 12.37 8.15 9.31 8.47 13.19 8.36 6.01 8.54 7.08 3.57

TB 6.24 3.1 3.81 3.77 4.8 3.03 2.51 2.42 2.9 1.3

DY 7.95 3.76 5.1 4.23 7.15 4.39 4.88 5.39 6.09 2.97

HO <1 <1 <1 <1 <1 <1 <1 <1 <1 <1

ER 14.32 5.25 6.41 6.81 12.22 6.39 5.28 6.26 7.08 2.91

TM 3.75 1.18 1.75 1.31 2.94 1.22 1.18 1.18 1.52 <1

YB 2.87 2.3 3 2.44 2.77 2.37 2.85 2.88 3.25 1.7

LU 2.02 1.51 1.55 1.79 1.92 1.75 1.5 1.46 1.67 1.16

TOTAL 256.1 65.79 80.39 76.2 261.59 74.75 82.63 88.7 96.14 55.15

REE

LREE 206.58 40.54 49.46 47.38 216.6 47.24 58.42 60.57 66.55 41.54

TOTAL HREE 49.52 25.25 30.93 28.82 44.99 27.51 24.21 28.13 29.59 13.61

BA/LA 5.5 62.58 20.76 53.84 5.02 29.12 49.53 62.43 30.14 36.05

NB/LA 1.31 1.4 0.96 1.15 0.93 0.97 1.92 0.7 0.54 0.83

LA/YB 19.37 3.91 3.7 4.25 23.26 4.54 5.11 5.12 5.1 6.38

ZR/NB 3.86 5.11 7.67 4.81 5.09 7.3 4.11 12.08 13.49 8.14

(LAN/LU 2.86 0.62 0.74 0.6 3.48 0.64 1.01 1.05 1.03 0.97

)N

(LA/SM) 2.78 1.61 1.51 1.58 3.73 1.75 2.07 2.01 1.87 2.22

N

(GD/YB) 3.49 2.87 2.51 2.81 3.86 2.86 1.71 2.4 1.77 1.7

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N

(LA/LU) 2.86 0.62 0.74 0.6 3.48 0.64 1.01 1.05 1.03 0.97

N LRRE/H 4.1716 1.6055 1.5990 1.6439 4.8144 1.7171 2.4130 2.1532 2.2490 3.052 REE

TABLE (1) CONTINUE

SP.NO. 21 22 23 24 25 26 27 28 29 30

MAJOR OXIDES (WT %)

SIO2 45.8 43.8 42.1 49.19 60.4 60.6 44.63 65.43 45.36 45.4

AL2O3 14.7 13.88 14.34 17.32 16.48 16.12 14.49 14.74 15.15 16

FE2O3 14.33 14.68 12.27 9.97 6.35 6.46 15.16 4.83 13.44 13.15

TIO2 2.54 2.82 1.34 0.98 0.66 0.65 2.76 0.49 2.65 2.28

CAO 7.51 7.2 11.55 7.04 4.79 4.81 7.83 2.51 7.81 7.47

MGO 6.92 9.3 10.69 5.02 2.4 2.33 7.34 2.15 7.13 6.23

NA2O 4.61 4.42 2.7 2.87 4.17 4 4.6 4.79 5.22 4.93 K2O 1.68 1.63 0.66 1.95 2.17 2.08 1.6 1.8 1.63 2.06

MNO 0.2 0.2 0.17 0.18 0.14 0.14 0.22 0.15 0.2 0.23

SO3 < 0.05 < 0.05 < 0.05 < 0.05 < 0.05 < 0.05 < 0.05 < 0.05 < 0.05 < 0.05 P2O5 0.8 0.86 0.23 0.36 0.25 0.21 0.79 0.11 0.8 0.78 L.O.I 0.69 1.03 3.67 4.42 1.91 1.92 0.13 2.59 0.13 1.27

NORMATIVE COMPOSITION Q 23.09 0 0 0 0 0 0 0 20.65 0 C 0.59 0 0 0 0 0 0 0 0 0

OR 10.98 9.7 9.56 12.37 9.63 8.11 9.65 8.7 0.37 9.74

AB 41.74 24.66 21.41 24.62 19.42 22.76 19.45 25.24 6.98 21.91

AN 12.18 13.14 16 15.64 14.33 15.62 16.72 18.51 41.84 14.02

NE 0 10.69 8.98 9.58 10.84 8.63 7.25 5.92 0 9.82

LC 0 0 0 0 0 0 0 0 0 0

AC 0 0 0 0 0 0 0 0 0 0

NS 0 0 0 0 0 0 0 0 0 0

DI 0 16.42 16.08 13.48 18.36 17 17.65 16.62 15.71 18.08

DIWO 0 8.82 8.63 7.24 9.86 9.13 9.48 8.92 8.44 9.71

DIEN 0 7.6 7.44 6.24 8.5 7.87 8.17 7.69 7.27 8.37

DIFS 0 0 0 0 0 0 0 0 0 0

HY 5.54 0 0 0 0 0 0 0 0 0

HYEN 5.54 0 0 0 0 0 0 0 0 0

HYFS 0 0 0 0 0 0 0 0 0 0

OL 0 7.23 8.16 6.7 7.44 8.03 9.91 7.03 0 7.52

OLFO 0 7.23 8.16 6.7 7.44 8.03 9.91 7.03 0 7.52

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OLFA 0 0 0 0 0 0 0 0 0 0

MT 0.51 0.66 0.63 0.76 0.69 0.69 0.67 0.64 0.61 0.69

HM 4.63 13.07 14.25 12.82 14.33 14.17 13.99 13.04 10.94 13.54

IL 0 0 0 0 0 0 0 0 0 0

AP 0.25 1.76 1.84 1.73 1.84 1.89 1.69 1.76 0.5 1.81 C_I 6.05 24.31 24.86 20.94 26.49 25.72 28.23 24.3 16.32 26.29 D_I 75.8 45.05 39.96 46.56 39.89 39.51 36.36 39.86 28 41.46

TRACE ELEMENTS (PPM)

SC 17.31 14.36 31.01 37.86 18.98 18.71 18.31 15.66 18.95 15.2 Y 20.01 20.28 14.77 14.31 20.63 19.61 23.62 19.29 22.47 24.31

AG 1.25 1.4 <1 <1 <1 <1 <1 <1 <1 <1

LI 9.38 8.6 7.23 25.95 13.03 11.89 9.64 <5 9.28 6.05

BE 2.93 2.9 1.09 1.35 <1 <1 3.6 1.16 4.08 3.05 V 171.43 158.66 203.48 295.81 111.53 121.62 197.73 70.6 202.57 143.84

CR 166.36 251.97 340.7 26.3 26.45 12.57 178.26 20.73 170.94 104.65

CO 50.51 54.31 69.72 37.6 25.38 24.98 55.03 17.89 51.92 36.94

NI 111.69 221.35 312.09 26.39 26.86 22.12 137.01 29.37 120.8 92.22

CU 35.47 39.63 78.88 104.17 36.49 27.43 44.24 3.02 40.14 28.74

ZN 105.65 103.2 79.7 76.58 53.97 52.51 109.81 79.76 95.08 70.28

GA 18.68 19.12 15.31 21.17 21.43 21.33 15.63 14.05 17.31 13.44

GE <1 2 <1 <1 <1 4.57 <1 7.36 2.46 <1

AS <5.5 10.87 11.1 9.05 21.64 <5.5 <5.5 12.49 <5.5 8.67

SR 836.7 914.89 570.95 621.78 457.92 412.82 777.45 125.48 812.07 824.44

ZR 235.25 291.7 130.22 82.21 159.69 127.79 280.59 102.92 322.8 243.37

NB 43.11 47.7 20.38 12.44 11.28 <10 36.22 <10 48.07 64.5

MO <2 <2 <2 <2 <2 <2 <2 <2 <2 3.09

CD <0.5 <0.5 <0.5 <0.5 <0.5 <0.5 0.94 0.71 <0.5 0.76

SN <10 <10 <10 <10 <10 <10 <10 <10 <10 <10

SB <10 <10 <10 <10 <10 <10 <10 <10 <10 <10

BA 268.6 262.8 164 662.88 567.5 727.7 246.1 427.8 255.98 314.4

HF 5.68 6.56 3.03 1 3.44 3.04 7.12 2.76 8.35 5.68

TA 4.39 6.93 3.99 1.03 4 3.36 5.67 4.53 8.75 7.69 W <5 <5 <5 <5 <5 <5 <5 <5 <5 <5

PB 917.61 16.44 14.46 4076.7 16.98 14.27 974.1 23.33 18.6 14.97

BI <10 <10 <10 <10 <10 <10 <10 <10 <10 <10

TH 3.28 4.29 2.3 <1 1.98 1.25 2.14 1.83 3.36 5.99 U <5 <5 <5 <5 <5 <5 <5 <5 <5 <5

RARE EARTH ELEMENTS (PPM)

LA 53.4 55.48 16.37 17.05 17.99 13.75 34.97 8.23 41.04 36.47

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CE 74.65 80.71 21.58 25 25.06 19.06 83.89 20.61 90.78 79.55

PR 7.12 6.8 <5.5 <5.5 <5.5 <5.5 <5.5 <5.5 5.77 <5.5

ND 43.32 47.16 19.31 21.61 20.95 18.73 47.71 15.05 46.37 41.37

SM 12.55 13.11 5.07 5.7 5.63 5.27 10.94 4.23 10.03 8.94

EU <1 <1 <1 <1 <1 <1 <1 <1 <1 <1

GD 10.56 12.27 7.55 8.86 8.29 6.88 16.33 5.6 17.32 12.64

TB 5.42 5.65 4.03 3.57 2.05 2.51 4.87 1.42 4.89 3.73

DY 7.54 7.8 5.1 4.96 5.94 5.8 6.31 4.13 6.15 6.08

HO <1 <1 <1 <1 <1 <1 <1 <1 <1 <1

ER 10.11 12.72 7.61 6.38 6.36 6.37 9.24 3.38 7.5 7.39

TM 3.62 3.93 2.03 1.67 1.17 1.22 2.76 <1 2.72 2.15

YB 2.7 2.57 2.57 2.62 3.23 3.19 2.64 2.8 2.75 3.03

LU 1.6 1.83 1.76 1.73 1.79 1.85 1.35 <1 1.21 1.19

TOTAL 232.5 250 92.98 99.15 98.46 84.63 221.0 65.45 236.5 202.5 REE

LREE 191.04 203.2 62.33 69.36 69.63 56.81 177.5 48.12 193.99 166.3

TOTAL HREE 41.55 46.77 30.65 29.79 28.83 27.82 43.5 17.33 42.54 36.21

BA/LA 5.03 4.74 10.02 38.88 31.55 52.93 7.04 51.99 6.24 8.62

NB/LA 0.81 0.86 1.24 0.73 0.63 0.65 1.04 1.09 1.17 1.77

LA/YB 19.78 21.59 6.37 6.51 5.57 4.31 13.25 2.94 14.92 12.04

ZR/NB 5.46 6.12 6.39 6.61 14.16 14.2 7.75 11.44 6.72 3.77

(AN/LU)N 3.47 3.15 0.97 1.02 1.04 0.77 2.69 0.95 3.52 3.18

LA/SM)N 2.68 2.66 2.03 1.88 2.01 1.64 2.01 1.23 2.58 2.57

(GD/YB)N 3.17 3.87 2.38 2.74 2.08 1.75 5.01 1.62 5.1 3.38

(LA/LU)N 3.47 3.15 0.97 1.02 1.04 0.77 2.69 0.95 3.52 3.18 LRRE/HR 4.59 4.34 2.03 2.32 2.41 2.04 4.08 2.77 4.56 4.59 EE

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