petrology and geochemistry of a boninite dyke from the

J. Earth Syst. Sci. (2019) 128:32 c© Indian Academy of Scienceshttps://doi.org/10.1007/s12040-018-1052-y

Petrology and geochemistry of a boninite dyke fromthe western Bastar craton of central India

Biswajit Hazarika1, D B Malpe1 and Ashish Dongre2,*1Department of Geology, RTM Nagpur University, Nagpur 440 001, India.2Department of Geology, Savitribai Phule Pune University, Pune 411 007, India.*Corresponding author. e-mail: [email protected]

MS received 10 January 2018; revised 5 April 2018; accepted 29 April 2018;published online 25 January 2019

The Dongargarh Supergroup along with the basal Amgaon Gneissic Complex constitutes thenorthwestern part of the central Indian Bastar craton. In the present study, we report a new finding ofa boninite dyke intruded in the Amgaon gneisses of this area. The dyke composed of mainly pyroxenes,amphiboles and subordinate amount of plagioclase. The higher contents of SiO2 (51–54wt.%), MgO(12–14wt.%), Ni (375–473 ppm), Cr (1416–1580 ppm) and very low TiO2 (0.2–0.4wt.%) are consistentwith the boninite nature of the dyke as well as the unevolved primary nature of the source magma. Theextraordinarily high CaO content (15.97–17.7wt.%) with higher CaO/Al2O3 (3.13–3.96) ratios classifiesit as high-Ca boninite. The trace element ratios including Zr/Ti, Ti/V, Ti/Sc and Ti/Yb further showits geochemical similarity with the Archaean boninite. The dyke also shows negative high-field strengthelement (Nb, Ta and Ti) anomalies which are the characteristics of the boninite rocks reported elsewhereand along with the enriched light rare earth element pattern, it shows more affinity particularly with thenorthern Bastar boninite dyke. The mineralogical and geochemical similarities of the boninite dykes fromthe Bastar craton indicate a widespread boninitic event during the Palaeoproterozoic having a similarorigin. These boninite dykes indicate the preservation of subduction-related signatures in the lithosphericmantle beneath the Bastar craton at the time of its evolution or may be during the convergence of theBastar and Bundelkhand cratons.

Keywords. Boninite; petrology; subduction; Bastar craton; central India.

1. Introduction

Boninites are relatively rare, high MgO (>8 wt.%)and low TiO2 (<0.5 wt.%) basaltic-to-andesiticrocks (Le Bas 2000). They are thought to formin the supra-subduction zone tectonic environ-ment, derived from the shallow melting of ahighly depleted hydrous mantle, fluxed with water

Supplementary material pertaining to this article is available on the Journal of Earth System Science website (http://www.ias.ac.in/Journals/Journal of Earth System Science).

from subducted slabs (e.g., Hickey and Frey 1982;Beccaluva and Serri 1988; Crawford et al. 1989;Stern and Bloomer 1992). However, they are alsoreported to form at the extended fore-arc with ascenario of propagation of back-arc spreading cen-tres into the fore-arc regions (e.g., Manikyambaet al. 2005; Meffre et al. 2012), as well as themantle plume interaction with the arc can also

1

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32 of 17 J. Earth Syst. Sci. (2019) 128:32

be a possible scenario for the boninite formation(Falloon et al. 2007, 2008). The atypical geo-chemical characteristics of boninite point to itsunusual genesis that includes high temperature(>1100◦C) and involvement of subduction fluid inmetasomatism of the shallow harzburgitic mantle,which was previously depleted by extensive extrac-tion of tholeiitic melt (Crawford et al. 1989). Theboninitic affinity of parental magmas for two of theworld’s largest platinum-group element deposits,the Bushveld igneous complex of South Africa andStillwater complex of Montana, USA, manifest itseconomic importance (Crawford et al. 1989).

In the context of Indian subcontinent, boninitesare reported from most of the cratons likewise theSinghbhum craton (Mir et al. 2015), Dharwar cra-ton (Manikyamba et al. 2005; Ganguly et al. 2016)and Bastar craton (Srivastava 2006, 2008; SubbaRao et al. 2008a, b; Chalapathi Rao and Srivas-tava 2009). The Bastar craton contains the reportsof the emplacement of boninitic rocks mostly inits southern and northern parts (Srivastava 2006;Subba Rao et al. 2008a, b), whereas a boniniticdyke is also reported from the Dongargarh Super-group of rocks (Chalapathi Rao and Srivastava2009). The aim of the present study is to reportthe occurrence of a boninite dyke for the firsttime from the western Bastar craton intruded inthe Amgaon gneisses. The paper further discussesthe geodynamic significance of this dyke based onthe comprehensive petrological and geochemicalstudies.

2. Geological setting

The Archaean Bastar craton is one of the cen-tral Indian cratonic domains, which was sepa-rated from the Bundelkhand craton by the centralIndian tectonic zone (CITZ) (Roy et al. 2000).The roughly rectangular-shaped Bastar craton,located south of the CITZ, is limited by NW–SE trending Mahanadi and Godavari rifts, ENE–WSW trending Narmada–Son rift and EasternGhats Mobile Belt. These rifts are considered tobe formed during Precambrian (e.g., Naqvi andRogers 1987; Srivastava et al. 2004). It lies in theENE of the Dharwar craton, separated later bythe Godavari rift. The overall tectonic trend ofthe craton is north–south, in contrast to ENE–WSW to east–west trend recorded in the Bun-delkhand craton (Yedekar et al. 1990; Roy et al.2000). The craton comprises granitoids and mafic

rocks, tonalite–trondhjemite gneisses, supracrustalrocks including greenstone belts and intrusivegranitic plutons and unmetamorphosed Neopro-terozoic sediments (Crookshank 1963; Ramakrish-nan 1990; Chaudhuri et al. 2002; Srivastava et al.2004; Ramakrishnan and Vaidyanadhan 2008). Thecraton has experienced different mafic magmaticevents (volcanics and intrusives) during Precam-brian that are reported from the different parts ofthe craton (Srivastava and Gautam 2009). Maficvolcanics are mostly represented by the basaltsand basaltic andesites (Krishnamurthy et al. 1990;Neogi et al. 1996). However, the low-Ti and high-Ti volcanics and siliceous high magnesium basalts(SHMB) are also reported from the Palaeoprotero-zoic Dongargarh Supergroup (Asthana et al. 1996;Sensarma et al. 2002). Mafic intrusives of differ-ent ages and compositions are extensively reportedfrom the southern, central and northern parts ofthe craton (e.g., Ramachandra et al. 1995; Sri-vastava and Singh 2004; Subba Rao et al. 2004,2008a; Srivastava 2006; Mondal et al. 2007; Frenchet al. 2008; Hussain et al. 2008; Srivastava andGautam 2008, 2009, 2012; Ratre et al. 2010; Daset al. 2011; Srivastava et al. 2011; Gautam and Sri-vastava 2011; Sinha et al. 2011; Pisarevsky et al.2013). The intrusives include sub-alkaline maficdykes i.e., Bastar Dykes 1 (BD1 of ∼2.7 Ga) andBastar Dykes 2 (BD2 of 1.88–1.89 Ga), boninite–norite dykes (∼2.1 Ga) from the southern part(French et al. 2008; Srivastava 2008; Srivastavaet al. 2011), Bhanupratappur–Keshkal dykes fromthe central part (Ramachandra et al. 1995; Gautamand Srivastava 2011; Srivastava and Gautam 2012)and Dongargarh, Chhura, Lakhna (∼1.44 Ga) andBandimal (∼1.42 Ga) dykes from the northernpart of the craton (Ratre et al. 2010; Das et al.2011; Sinha et al. 2011; Pisarevsky et al. 2013;Srivastava and Gautam 2015).

The boninite of the present study (21◦28′40.3′′Nand 80◦29′56′′E) found as intrusive within theAmgaon gneisses of western Bastar craton(figure 1). This part of the craton mostly comprisesthe Amgaon Group and Dongargarh Supergroupof rocks. The Amgaon Group is composed ofpsammitic–psamopelitic metamorphite alternatingwith metabasic lavas. Granite gneisses along withTTG gneissic phase forms basement for the Don-gargarh Supergroup (Sarkar et al. 1981; Rao 1981;Krishnamurthy et al. 1988; Sarkar 1994; Wan-jari et al. 2005; Ramakrishnan and Vaidyanadhan2008). The Neoarchean–Palaeoproterozoic Dongar-garh Supergroup comprises older bimodal volcanics

J. Earth Syst. Sci. (2019) 128:32 of 17 32

Figure 1. Geological map of the western Bastar craton,central India (after Asthana et al. 2017). Black asterisk rep-resents the location of the present boninite dyke and theother one represents the location of Dongargarh boninite(Chalapathi Rao and Srivastava 2009).

of the Nandgaon Group and younger volcano-sedimentary sequence of the Khairagarh Groupdivided by an unconformity after the Dongar-garh granitoid emplacement (Krishnamurthy et al.1990).

3. Analytical technique

The mineral chemistry was determined using aCameca SX 100 electron probe micro-analyser(EPMA) at the University of Johannesburg, SouthAfrica. Quantitative mineral analyses were oper-ated at 20 kV accelerating voltage, 20 nA beamcurrent and 1µm beam diameter with variable (12–40 s) counting time on the peak, based on theelement. The standards used for the calibrationof EPMA were natural jadeite (Na), olivine (Mg),almandine (Al), diopside (Si), orthoclase (K), wol-lastonite (Ca), rhodonite (Mn) and haematite (Fe),and synthetic pure oxides for TiO2, Cr2O3 andNiO. Elements were measured on their Kα lines.The ‘X-PHI’ method was used for the matrixcorrection (Merlet 1994). Backscattered electron(BSE) imaging was performed on the same instru-ment using the same conditions of accelerationvoltage and beam current.

For the whole-rock chemical analyses, powderedrock samples were milled in HERZOG swing grind-ing mill (Model HSM-100) and were analysed usingthe fused disc and the borate fusion method. Major

element oxides for five samples were determined byinductively coupled plasma-emission spectrometrytechnique (SpectroCiros-CCD) at Acme Labora-tories Canada and wavelength dispersive X-rayfluorescence spectrometry at Wadia Institute ofHimalayan Geology, Dehradun. Trace elements(including rare earth elements (REEs)) were anal-ysed by inductively coupled plasma-mass spec-trometry (Perkin Elmer SCIEX, Model ELAN�

9000). Instruments were calibrated using the stan-dard reference materials and internal standards,and accuracy was monitored using the certifiedreference materials using the fundamental parame-ters model. The analyses of the standard referencematerials are given in table S1 (online supplemen-tary material) to show the accuracy and precisionof the present data.

4. Petrography

Petrographic studies reveal fine-to-medium-grainednature of the rock. Mineralogically, it mainly con-sists of pyroxenes with minor amounts of amphi-boles and plagioclase (figure 2). Pyroxenes arerepresented by subhedral-to-anhedral grains ofboth clinopyroxenes (cpx) and orthopyroxenes(opx). Clinopyroxenes are dominant than orthopy-roxenes. Patches of orthopyroxenes occurring asrelict granulations in clinopyroxenes suggest theirearlier formation. At some places, orthopyrox-enes are replaced by amphiboles. Chloritisationeffects are not predominant. Plagioclase grainsoccur as intercumulus by occupying the spacesbetween pyroxene grains. It shows albite twinningand some twin lamellae are deformed or disap-peared, indicating the deformation of the grains(figure 2). Saussaritisation and sericitisation at thegrain boundaries suggest an alteration.

5. Mineral chemistry

The mineral chemical compositions of clinopyrox-enes and amphiboles are given in table 1.

5.1 Clinopyroxene

Clinopyroxene is a major mineral constituent ofthe dyke. It shows a narrow range of Mg num-ber [Mg# = Mg/(Mg + Fe) atomic] between 0.76and 0.78 and is mostly diopside in composi-tion (Wo48.5−50.1−En38.2−39.2−Fs11.5−12.3). Theseclinopyroxenes are more enriched in Ca compared


Figure 2. (a) Photomicrograph showing the presence of Cpx, Pl and Amp; (b) patches of Opx are visible in Cpx, at someplaces Opx breaks down to amphibole; (c and d) BSE images of present dykes showing Cpx and Amp grains. Abbreviations:Pl, plagioclase; Cpx, clinopyroxene; Amp, amphibole.

to the clinopyroxenes of the mafic Deccan basalticrocks (Melluso and Sethna 2011) and are showingmore similarity with the composition of the Don-gargarh boninitic dyke (figure 3). The extremelylow TiO2 (0.02–0.09wt.%) content of clinopy-roxene is also similar to the boninitic dyke ofthe Dongargarh Supergroup (Chalapathi Rao andSrivastava 2009).

5.2 Amphibole

The amphiboles of the present study are mainlyCa-bearing and consist of high (>5 wt.%) and lowalumina (<5 wt.%) variety. They are classified asactinolite and hornblende on the basis of Mg/(Mg+Fe) and Si (a.p.f.u.) contents (Leake et al. 1997)(figure 4). Chalapathi Rao and Srivastava (2009)reported the amphiboles of actinolite and horn-blende composition from the boninitic dyke ofDongargarh Supergroup rocks, which are mostlyshowing similar composition with little enrichmentin Mg content.

6. Bulk rock geochemistry

The major and trace element compositions of thestudied dyke along with the average composi-tions of earlier reported boninite dykes from the

Bastar craton of the central India (Srivastava 2006;Subba Rao et al. 2008a, b; Chalapathi Rao andSrivastava 2009), from Gadwal greenstone belt ofsouth India (Manikyamba et al. 2005) and theArchaean boninites (Smithies et al. 2004) are givenin table 2. The characteristic higher SiO2 (>51.8−53.6 wt.%) and MgO (>12.2−14.3 wt.%) contentsand higher Mg number (Mg# = Mg + Fe/Mg)of 73–76 shown by the present dykes are similarto the earlier reported worldwide boninitic rocks.The high Mg-rock classification schemes recom-mended by IUGS (Le Bas 2000), based on the totalalkali vs. SiO2 content, classify the present samplesas boninites and are showing very similar com-position to the earlier reported Bastar boninites(Srivastava 2006; Subba Rao et al. 2008a, b; Cha-lapathi Rao and Srivastava 2009) (figure 5). Thedyke shows extremely elevated CaO content (15.9–17.7wt.%) as compared to the earlier reportedboninites from the Bastar craton. The SiO2, Al2O3

and Na2O contents show a negative correlationwith MgO, while the TiO2 increases with theincreasing MgO (figure 6a–d), which is consis-tent with the fractionation trends in the maficmagma and with the other boninites. The nor-mal trends of major oxides with MgO also suggesttheir immobility during alteration or metamorphicprocesses.


Table

1.Chem

icalcompositions(E

PMA

results),andcalculatedmineralform

ulaeoftheamphibole

andclinopyroxenein

theboninitedykeofthepresentstudy.

Min

eral

Am

phib

ole

Analy

sis

no.

AM

G-

11/3

AM

G-

11/5

AM

G-

11/8

AM

G-

11/10

AM

G-

11/1

AM

G-

11/2

AM

G-

11/4

AM

G-

11/6

AM

G-

11/7

AM

G-

11/9

AM

G-

11/11

Majo

rox

ides

(wt.

%)

SiO

251.8

453.6

554.8

352.5

650.1

150.2

350.8

949.7

347.9

849.8

149.9

4

TiO

20.3

30.1

0.0

60.1

20.6

10.4

30.2

90.3

60.7

70.5

60.4

2

Al 2

O3

4.1

33.0

12.2

13.5

35.3

85.4

4.9

66.1

17.5

5.6

25.5

3

FeO

11.7

910.9

310.2

111.2

612.5

412.4

812.0

312.7

813.9

212.5

212.6

5

MnO

0.1

80.1

60.1

60.1

80.1

90.1

50.1

50.1

90.1

90.1

60.1

7

MgO

15.3

316.3

617.2

516.0

614.4

314.4

14.7

914.0

713.1

314.5

14.6

9

CaO

12.8

212.7

313.1

12.9

12.6

712.7

912.7

812.6

512.8

212.6

12.7

9

Na2O

0.6

40.4

30.2

60.4

80.8

60.7

90.7

10.9

1.1

10.8

20.7

8

K2O

0.3

20.1

80.1

20.2

20.4

10.4

50.3

50.4

40.5

60.4

0.4

2

F0.1

30.0

80.0

90.0

90.1

0.1

10.1

10.1

20.1

0.1

0.1

Cl

0.0

20.0

10

0.0

20.0

70.0

40.0

20.0

70.0

70.0

40.0

5

Tota

l97.5

397.6

498.2

997.4

297.3

797.2

797.0

897.4

298.1

597.1

397.5

4

Calc

ula

ted

min

eralfo

rmula

e(a

.p.f.u

.)∗

Coef

.8.7

08.6

08.5

18.6

68.7

78.7

88.7

68.7

88.8

18.7

98.7

7

Si

7.5

07.6

87.7

67.5

87.3

27.3

47.4

27.2

77.0

37.2

97.2

9

Ti

0.0

40.0

10.0

10.0

10.0

70.0

50.0

30.0

40.0

80.0

60.0

5

Al

0.7

00.5

10.3

70.6

00.9

30.9

30.8

51.0

51.3

00.9

70.9

5

Fe2

+1.4

31.3

11.2

11.3

61.5

31.5

21.4

71.5

61.7

11.5

31.5

4

Mn

0.0

20.0

20.0

20.0

20.0

20.0

20.0

20.0

20.0

20.0

20.0

2

Mg

3.3

13.4

93.6

43.4

53.1

43.1

43.2

13.0

72.8

73.1

63.2

0

Ca

1.9

91.9

51.9

91.9

91.9

82.0

02.0

01.9

82.0

11.9

82.0

0

Na

0.1

80.1

20.0

70.1

30.2

40.2

20.2

00.2

60.3

20.2

30.2

2

K0.0

60.0

30.0

20.0

40.0

80.0

80.0

70.0

80.1

00.0

70.0

8

F0.0

60.0

40.0

40.0

40.0

50.0

50.0

50.0

60.0

50.0

50.0

5

Cl

0.0

00.0

00.0

00.0

00.0

20.0

10.0

00.0

20.0

20.0

10.0

1

Tota

l15.2

915.1

715.1

315.2

415.3

715.3

615.3

115.4

115.5

115.3

715.4

0

XM

g0.7

00.7

30.7

50.7

20.6

70.6

70.6

90.6

60.6

30.6

70.6

7

32 of 17 J. Earth Syst. Sci. (2019) 128:32Table

1.(C

ontinued.)

Min

eral

Clinopyro

xen

e

Analy

sis

No.

AM

G-

11/1

AM

G-

11/2

AM

G-

11/3

AM

G-

11/4

AM

G-

11/5

AM

G-

11/6

AM

G-

11/7

AM

G-

11/8

AM

G-

11/9

AM

G-

11/10

AM

G-

11/11

Majo

rox

ides

(wt.

%)

SiO

253.7

853.6

153.8

253.6

53.8

53.7

553.6

553.4

853.2

553.5

53.9

7

TiO

20.0

60.0

30.0

20.0

90.0

20.0

70.0

6n.a

.0.0

40.0

40.0

3

Al 2

O3

0.5

30.5

50.2

60.5

30.4

50.5

80.5

0.3

60.4

70.6

10.4

8

FeO

7.4

77.1

77.1

77.6

27.3

27.2

67.2

77.1

97.3

57.6

37.3

5

MnO

0.2

30.2

20.2

50.2

0.2

0.2

30.2

0.2

20.2

40.2

10.2

MgO

13.6

813.6

913.9

613.9

113.6

713.7

713.8

913.8

213.7

813.7

813.7

2

CaO

24.4

724.3

925.0

323.9

724.8

524.4

224.5

625.1

224.6

24.3

424.6

8

Na2O

0.3

50.3

50.2

20.4

30.2

80.3

30.3

10.2

80.3

30.3

30.3

2

K2O

n.a

.0.0

10.0

10.0

1n.a

.n.a

.0.0

10.0

1n.a

.0.0

1n.a

.

F0.0

60.0

50.0

20.0

20.0

30.0

30.0

4n.a

.0.0

50.0

10.0

2

Cl

0.0

10.0

10.0

1n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.0.0

1n.a

.

Tota

l100.6

4100.0

8100.7

7100.3

8100.6

2100.4

4100.4

9100.4

8100.1

1100.4

7100.7

7

Calc

ula

ted

min

eralfo

rmula

e(a

.p.f.u

.)∗

Coeff

.2.2

32.2

32.2

22.2

32.2

32.2

32.2

32.2

32.2

42.2

32.2

2

Si

1.9

91.9

91.9

91.9

91.9

91.9

91.9

91.9

91.9

81.9

91.9

9

Ti

n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.

Al

0.0

20.0

20.0

10.0

20.0

20.0

30.0

20.0

20.0

20.0

30.0

2

Fe2

+0.2

30.2

20.2

20.2

40.2

30.2

20.2

30.2

20.2

30.2

40.2

3

Mn

0.0

10.0

10.0

10.0

10.0

10.0

10.0

10.0

10.0

10.0

10.0

1

Mg

0.7

60.7

60.7

70.7

70.7

50.7

60.7

70.7

70.7

70.7

60.7

6

Ca

0.9

70.9

70.9

90.9

50.9

90.9

70.9

81.0

00.9

80.9

70.9

8

Na

0.0

30.0

30.0

20.0

30.0

20.0

20.0

20.0

20.0

20.0

20.0

2

F0.0

10.0

1n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.

Cl

n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.n.a

.

Tota

l4.0

14.0

14.0

14.0

14.0

14.0

14.0

14.0

24.0

24.0

14.0

1

XM

g0.7

70.7

70.7

80.7

60.7

70.7

70.7

70.7

70.7

70.7

60.7

7

Calc

ula

ted

min

eralfr

act

ions(m

ol%

)†

Wo

49.4

349.5

749.8

348.5

149.9

749.4

149.4

150.1

349.5

249.0

549.7

0

En

38.4

538.7

238.6

739.1

738.2

538.7

738.8

938.3

838.6

038.6

538.4

5

Fs

12.1

211.7

111.5

012.3

211.7

911.8

211.7

111.5

011.8

812.3

011.8

5

n.a

.:not

analy

sed

or

mea

ns

bel

owth

eE

PM

Adet

ecti

on

lim

it;X

Mg

=M

g/(M

g+

Fe)

ato

mic

.∗ C

alc

ula

ted

on

the

basi

sof23

(am

phib

ole

s)and

6(c

linopyro

xen

es)

oxygen

ions

per

form

ula

unit

,re

spec

tivel

y.† A

bbre

via

tions

use

dfo

rnorm

ati

ve

min

erals

.W

o:w

ollast

onit

e;E

n:en

stati

te;Fs:

ferr

osi

lite

.


Figure 3. Composition of pyroxenes in Ca–Mg–Fe diagram.Deccan basalts pyroxenes field is taken from Melluso andSethna (2011) and data for Dongargarh boninites from Cha-lapathi Rao and Srivastava (2009).

Figure 4. Compositional variation and classification ofamphiboles (after Leake et al. 1997). Data for Dongargarhboninites from Chalapathi Rao and Srivastava (2009).

The present dyke shows high amounts ofcompatible trace elements such as Sc (49–50 ppm),V (228–230 ppm), Cr (1416–1580 ppm) and Ni(375–473 ppm). Nickel shows a positive correla-tion with MgO (figure 7a) like other boninite rocksand is consistent with the fractionation of themafic magma. The Zr, Ti, Nb and V concentra-tions (figure 7b–d) are much more similar to theother reported boninites from Bastar and Dharwarcratons and particularly to the Archaean boninites(Smithies 2002). Nb concentration is between 2.2and 2.7 ppm. The very low Nb values are reportedfrom the Dongargarh boninites (0.18–0.23 ppm)(Chalapathi Rao and Srivastava 2009), whereashigher values (5–6 ppm) are known from the Bastar(Srivastava 2006; Subba Rao et al. 2008a, b) andGadwal boninites (Manikyamba et al. 2005). Prim-itive mantle normalised multi-element diagrams

(normalising values after Sun and McDonough1989) show enrichment of large ion lithophile ele-ments (LILEs) as compared to high-field strengthelements (HFSEs) with prominent negative anoma-lies at Nb, Ta, Zr, Hf and Ti (figure 8b). Chondritenormalised REE patterns (Sun and McDonough1989) (figure 8a) show an enriched trend of lightREEs (LREE) and a relatively depleted trendof heavy REEs (HREE) with distinct negativeEu anomaly indicating plagioclase fractionationduring the evolution of the melt.

7. Discussion

The studied dyke shows higher MgO content (i.e.,>12 wt.%) and compatible trace elements (Sc, V,Cr and Ni) which indicates the primary nature ofits source magma. The higher amount of MgO andlower Al2O3, K2O, Na2O, Rb and Sr demonstratethat the dyke is not affected by the significantcrustal contamination. The intrusion of dyke in thegneisses would have been elevated these elementconcentrations on the event of crustal contamina-tion. The Al and Ti contents of boninites alongwith the trace elements such as Th, Nb, Ta, Zr,Hf, Y, Sc and V are considered to be least sus-ceptible to alteration and conventionally used todifferentiate various high-Mg mafic rocks such asboninite, high-Mg norite, SHMB and komatiite(Poidevin 1994; Piercey et al. 2001; Polat et al.2002; Smithies 2002; Srivastava 2006; ChalapathiRao and Srivastava 2009). The very low valuesof Nb/La (0.15–0.22), Nb/Ce (0.07–0.08) Rb/Sr(0.01–0.05) and Rb/Ba (0.04–0.07) showed by thepresent dyke also rule out the effects of post-magmatic deuteric alteration processes as well ascrustal contamination (Lafleche et al. 1992; Miret al. 2011). The negative Nb, Ta and Ti anoma-lies on multi-element diagram are common featuresin the Archaean as well as Phanerozoic boninites(Smithies et al. 2004) and also characteristic of themagmatism related to subduction (Wilson 1989;Condie 1997). The relative depletion in the HFSEs(Nb, Ta and Ti) may have been affected by crustalcontamination; however, these anomalies are con-sistent in the global boninitic rocks and it lookslike much of these and the overall trace element sig-natures may have been largely inherited from theenriched sources (Cameron et al. 1983; Hall andHughes 1990; Nielsen et al. 2002; Smithies 2002;Srivastava 2006).

32 of 17 J. Earth Syst. Sci. (2019) 128:32Table

2.Bulk

rock

chem

icalcompositionsofthedykeunder

studyandcompilationofearlierreported

boninitecompositions.

12

34

56

78

910

11

Sam

ple

no.

AM

G-1

0A

MG

-11

DM

K

2541

DM

K

2543

DM

K

2544

DB

(n=

2)

NB

B

(n=

6)

SB

B(H

igh-C

a;

n=

3)

SB

B(L

ow-C

a;

n=

24)

GB

(n=

22)

AB

(n=

15)

Majo

rox

ides

(wt.

%)

SiO

253.5

752.3

252.1

151.8

453.6

251.7

956.0

353.4

153.5

748.7

351.2

5

TiO

20.3

10.3

70.3

50.2

40.1

90.0

40.3

30.3

20.4

60.2

80.3

4

Al 2

O3

5.2

74.4

75.1

44.2

74.5

16.1

49.3

812.8

010.9

210.3

316.3

6

Fe 2

O3

7.8

99.0

48.0

79.3

27.8

18.4

19.6

29.1

710.8

111.6

410.1

9

MnO

0.1

40.1

70.1

30.1

90.2

20.1

40.1

70.1

50.1

70.1

57.8

1

MgO

12.2

012.9

013.5

314.3

413.1

718.5

611.7

510.0

213.0

318.7

49.9

6

CaO

16.5

117.7

016.8

515.9

716.3

412.1

78.5

612.2

96.5

09.3

20.1

8

Na2O

1.6

21.0

51.2

71.1

41.5

70.5

12.1

71.2

41.2

30.6

41.7

0

K2O

0.4

10.2

00.3

10.4

50.2

70.3

00.8

40.1

20.9

30.4

20.4

3

P2O

50.0

30.0

40.0

60.0

40.0

70.0

50.0

90.0

50.0

70.0

30.0

4

LO

I1.5

01.2

01.6

51.3

51.4

31.6

30.6

32.2

14.1

13.5

1

Tota

l99.4

599.4

699.4

799.1

599.2

099.7

399.0

499.5

697.7

0104.0

9101.7

4

CaO/A

l 2O

33.1

33.9

63.2

83.3

33.6

21.9

90.9

31.0

20.5

90.9

00.4

9

Mg#

76.4

374.9

674.9

373.2

875.0

481.4

568.2

571.3

770.7

177.4

564.5

3

Tra

ceel

emen

ts(p

pm

)

Sc

49

50

––

–56.6

641.5

036.6

730.4

642.9

144.0

8

V228

230

––

–218.5

0194.0

0168.3

3173.3

894.0

5167.3

8

Cr

1580.5

01416.2

9–

––

2677.5

01181.1

71169.5

01229.9

32008.4

1595.5

4

Co

45.2

50.3

––

–70.9

468.5

0–

–76.5

970.4

3

Ni

375

473

––

–362.0

0157.1

7274.5

0303.8

7838.7

3248.7

7

Ga

10.2

8.7

––

–11.7

821.8

36.5

06.2

5–

–

Rb

7.6

1.5

––

–7.3

556.6

73.0

047.3

358.7

320.9

2

Sr

154.2

131.2

––

–203.0

0241.6

7100.3

378.5

433.8

2100.3

1

Y8.4

12.7

––

–10.9

317.1

79.3

312.7

113.4

111.0

7

Zr

49.8

46

––

–26.1

658.0

040.6

763.2

516.6

429.0

7

Nb

2.2

2.7

––

–0.2

13.0

01.0

03.6

30.7

91.1

4

Cs

0.0

80.0

7–

––

0.1

01.6

7–

–7.0

6–

Ba

115

37

––

–158.5

0267.0

066.3

3180.2

139.2

782.4

2

Hf

1.4

1.4

––

–0.6

91.2

30.9

01.8

80.4

5–

Ta

0.2

0.1

––

–0.0

50.6

90.1

40.5

90.0

6–

Th

2.3

2.4

––

–0.6

63.5

01.4

55.2

00.2

70.4

5

U0.5

0.5

––

–0.2

31.5

0–

–0.1

40.1

7

Ti

1858.4

52218.1

5–

––

239.0

01988.2

41938.3

82727.7

31651.3

52022.3

1

RE

E(p

pm

)

La

14.8

12.5

––

–5.3

314.9

05.9

510.7

32.0

02.8

7

J. Earth Syst. Sci. (2019) 128:32 of 17 32C

e31.6

33

––

–12.1

327.9

910.5

022.1

34.1

16.4

4

Pr

3.9

34.4

7–

––

1.9

62.8

41.0

72.3

20.5

60.8

3

Nd

16.1

19.6

––

–9.2

413.2

14.4

59.0

62.4

43.4

8

Sm

3.5

94.2

9–

––

2.2

22.7

31.0

51.9

70.6

90.9

1

Eu

0.8

30.9

6–

––

0.7

30.8

50.3

50.5

30.2

90.3

1

Gd

3.0

83.6

8–

––

2.4

92.8

41.2

52.0

81.0

91.1

3

Tb

0.4

0.5

3–

––

0.3

80.4

20.2

50.3

80.2

60.2

2

Dy

1.9

42.7

7–

––

1.8

52.5

71.5

02.1

71.8

71.5

9

Ho

0.3

10.4

8–

––

0.4

20.5

40.3

50.4

50.4

90.3

9

Er

0.8

81.3

9–

––

1.1

91.6

11.0

01.3

61.4

41.2

6

Tm

0.1

20.1

8–

––

0.1

80.2

20.1

60.2

30.4

80.2

5

Yb

0.7

41.1

––

–1.0

21.3

30.9

51.3

71.4

91.4

5

Lu

0.1

0.1

5–

––

0.1

60.2

60.1

50.2

20.2

40.2

3

Tota

lR

EE

78.4

285.1

––

–39.2

672.3

128.9

848.0

517.4

421.2

4

Ti/

V8.1

59.6

4–

––

1.1

010.3

711.5

115.7

419.2

511.9

7

Ti/

Sc

37.9

344.3

6–

––

4.2

348.9

454.6

389.6

847.6

344.6

1

Ti/

Yb

2511.4

22016.5

0–

––

236.7

61516.8

11846.1

91957.9

31126.1

91552.6

8

1–5:P

rese

nt

study;6:D

ongarg

arh

bonin

ite

(DB

)(C

hala

path

iR

ao

and

Sri

vast

ava

2009);

7:nort

her

nB

ast

ar

bonin

ite

(NB

B)

(Subba

Raoet

al.

2008a,b

);8–9:so

uth

ern

Bast

ar

bonin

ite

(SB

B)

(Sri

vast

ava

2006);

10:G

adw

albonin

ite

(GB

)(M

anik

yam

baet

al.

2005);

11:A

rchaea

nbonin

ite

(AB

)(S

mit

hie

set

al.

2004).

–:not

analy

sed;M

g#

=ato

mic

Mg/(M

g+

Fe2

+)×

100.LO

I:lo

sson

ignit

ion.

Global boninites have a marked U-shape(depleted middle REE (MREE) than the LREEand HREE) multi-element pattern (Bedard 1999;Polat et al. 2002; Manikyamba et al. 2005). Sucha depleted MREE pattern is not observed in thepresent dyke and remains absent in the Bastar cra-ton boninites. Whereas the depleted HREEs com-pared to LREE and MREE patterns are observedto be a characteristic feature of all the Bastarboninites (Subba Rao et al. 2008a; Chalapathi Raoand Srivastava 2009).

The CaO content of the present dyke is veryhigh that it ranges from 15.9 to 17.7 wt.%, whichis higher compared to the Proterozoic boninitesof the Bastar craton and Gadwal greenstone belt.The Al2O3 content of the dyke is very low; how-ever, the lower Al2O3 and higher CaO are thecharacteristics of the nearby Dongargarh boni-nite from the same Bastar craton and consideredhere to be distinct features of these dykes. Verylow CaO values (i.e., 0.10–0.12wt.%) are char-acteristics of the Archaean boninites (Smithies2002). Based on the lower amounts of Al2O3

and higher CaO/Al2O3 ratios, the present dykeis classified, more precisely, as a high-Ca boninitevariety (figure 9). The phanerozoic boninites gen-erally show a very high Al2O3/TiO2 ratio and inArchaean boninites such ratio varies from 26 to 88.The value of Al2O3/TiO2 in the present dyke varies

Figure 5. Total alkali silica (TAS) classification diagram(after Le Bas 2000) for high-Mg mafic dykes and com-positional variation of present dyke is compared with theArchaean boninite field (Smithies et al. 2004), Bastarboninites (Srivastava 2006; Subba Rao et al. 2008a, b; Cha-lapathi Rao and Srivastava 2009) and Gadwal boninites(Manikyamba et al. 2005).


from 12 to 24. The lower Al2O3/TiO2 values canbe attributed to the lower content of Al2O3 in thepresent dyke, which is also a feature of Dongargarhboninite as mentioned earlier. On the other hand,TiO2 contents of the dyke are very low (0.19–0.37 wt.%) and following the boninite classificationwhere TiO2 is mostly <0.5 wt.%. The bivariateplots, using Zr/Ti, Ti/V, Ti/Sc and Ti/Yb ratios(figure 10a–d) discriminating between Archaeanboninites with contaminated komatiites andSHMB, show a distinct affinity of the studiedsamples towards the Archaean boninites.

Smithies et al. (2004) recognised two groupsof Archaean high-Mg mafic rocks having strongrefractory mantle source, e.g., Whundo type andWhitney type. Whundo type (known in age from3.12 and 2.8 Ga) rocks are considered to be trueArchaean analogues of modern boninites, havingsimilarities in the composition and also their asso-ciation with tholeiitic to calc-alkaline mafic tointermediate magmatism. They are similar to mod-ern boninites in terms of their derivation fromthe metasomatised refractory mantle. On the otherhand, Whitney type (of 3.8Ga) rocks are closelyassociated with ultramafic komatiites and are con-sidered to be derived by plume magmatism. Pearceet al. (1992) suggested the genesis of boninites bymelting of depleted residual metasomatic MORB

mantle where metasomatism is due to fluids andmelts are derived from the dehydrated subductedslab. Earlier studies (e.g., Arndt et al. 1987; Sunet al. 1989) reported the role of assimilation-fractional crystallisation (AFC) of komatiites forthe formation of boninites. The present dyke rep-resents a Whundo type of magmatism and is notconsistent with a komatiite AFC model in itsgenesis because of no record of komatiite in thevicinity.

The formation of boninites by higher degreesof partial melting of a refractory mantle sourcerelated to the subduction is now well established(Tatsumi and Eggins 1995; Turner et al. 1997;Green and Falloon 1998; Falloon and Danyu-shevsky 2000; Kushiro 2007). Very low contents oftitanium are considered to be due to residual Ti-bearing phase after melting (Green and Pearson1986) in the refractory mantle source formed by thetholeiitic melt extraction (Sun and Nesbitt 1978).Subsequent enrichment of refractory mantle sourceregions and higher concentrations of LILEs, Th andLa compared to HFSEs are considered to be theresult of interaction with subduction-derived fluidprior to the second-stage melting (Sun and Nesbitt1978; Hickey and Frey 1982; Crawford et al. 1989;Falloon and Danyushevsky 2000; Polat et al. 2002;Smithies et al. 2004).

Figure 6. (a–d) Variations of major oxides (SiO2, TiO2, Al2O3 and Na2O) with MgO (wt.%) and are compared with earlierreported Archaean boninites (Smithies et al. 2004), Bastar boninites (Srivastava 2006; Subba Rao et al. 2008a, b; ChalapathiRao and Srivastava 2009) and Gadwal boninites (Manikyamba et al. 2005).


Figure 7. (a) MgO (wt.%) vs. Ni (ppm); (b) Zr (ppm) vs. Nb (ppm); (c) Zr (ppm) vs. Y (ppm); and (d) Ti/1000 vs.V (ppm) variation diagrams for the present boninite dyke and their comparison with earlier reported Archaean boninites(Smithies et al. 2004), Bastar boninites (Srivastava 2006; Subba Rao et al. 2008a, b; Chalapathi Rao and Srivastava 2009)and Gadwal boninites (Manikyamba et al. 2005).

The formation of boninitic dykes from arefractory mantle source and subduction-inducedmetasomatism have been known from the Bastarcraton (Srivastava 2008; Chalapathi Rao and Sri-vastava 2009) and the neighbouring Singhbhumcraton (Mir et al. 2015). It was suggested thatthe extensive extraction of tholeiitic melt dur-ing Archaean to Palaeoproterozoic (Srivastava andGautam 2009) may have resulted in the formationof refractory mantle sources beneath the Bastarcraton and the subduction-related tectonic settings(Yedekar et al. 1990; Asthana et al. 2016) could bethe reason for geochemical characteristics typicalof boninite shown by these rocks.

The samples under the study show very low TiO2

contents (i.e., <0.40 wt.%) with correspondinglyhigher CaO/TiO2 ratios (47.84–86.00) indicatetheir highly refractory mantle source which hadexperienced earlier the tholeiitic melt extractionevent. The enriched Ce/Ta ratios (158–330) alongwith negative HFSE anomalies reflect the con-tribution of subduction-related component in themelt (Smellie et al. 1995) and thus support therole of subduction in influencing the geochemical

characters of the present boninite dyke in thewestern part of the Bastar craton.

7.1 Geodynamics involved

Boninite dyke emplaced in the Archaean basementwas reported from the margin of the Chhattis-garh basin in the northern Bastar craton (SubbaRao et al. 2008a, b). This dyke inferred to form inintra-cratonic settings, similar to other Archaeanboninite rocks reported from other parts of theworld (e.g., Smithies 2002). Boninite dyke reportedfrom the Neoarchean–Palaeoproterozoic Dongar-garh Supergroup is intrusive into the Bijli rhyolitesin northwestern Bastar craton (Chalapathi Raoand Srivastava 2009) and is considered to repre-sent a fossil subduction zone where a lithosphericmantle in this domain appears to have retainedmemories of ancient subduction. Palaeoproterozoicboninites are reported from the southern Bastarcraton which are intrusives into basement gneisses(Srivastava and Singh 2003; Srivastava et al. 2004,2011) and also from the areas of Bastanar, Dan-tewada and Katekalyan of southern Bastar craton


Figure 8. (a) Chondrite-normalised (after Sun and McDonough 1989) and (b) primitive-mantle normalised (after Sun andMcDonough 1989) patterns for the present study dyke and boninite dykes from the north Bastar craton (Subba Rao et al.2008a, b) and Dongargarh boninite dyke (Chalapathi Rao and Srivastava 2009).

(Srivastava 2006) where they are very well exposed.These dykes are also reported to form in an intra-cratonic setting. This clearly indicates the presenceof widespread intra-cratonic boninite magmatismin the whole Bastar craton during Neoarchean toPalaeoproterozoic.

A number of geodynamic models have beenproposed for the evolution of central Indian Neoar-chean–Palaeoproterozoic Dongargarh Supergrouprocks (e.g., Yedekar et al. 1990; Raza et al. 1993;Neogi et al. 1996; Asthana et al. 1996, 1997,2016, 2017; Manikyamba et al. 2016). Yedekaret al. (1990) envisaged the Dongargarh volcanicrocks as remnant island arc lavas and proposed asouthward subduction model of the Bundelkhandproto-continent under the Deccan proto-continentduring the Proterozoic. Raza et al. (1993) alsosupported the subduction-related origin of theDongargarh volcanics that exist along a Palaeopro-terozoic ocean closure in central India and mark the

suture of two proto-continental masses. Asthanaet al. (1996, 1997) suggested an arc-related set-ting for Khairagarh volcanics of the DongargarhSupergroup, which are inter-layered with terrige-nous sediments formed in back-arc basin. In recentworks, Asthana et al. (2016, 2017) proposed a ridgesubduction model followed by slab window alongPalaeoproterozoic central Indian suture to accountfor the distribution of fore arc–arc–back arc asso-ciation of the Bastar craton. Geochemical studieson gneisses and granitoids also provide significantevidence for the multiphase subduction-relatedevents and for crustal growth during Protero-zoic and Archaean in the Bastar craton (Hussainet al. 2004; Mondal et al. 2006). Therefore, theconvergence-related evolution of the Bastar cra-ton and especially the Dongargarh Supergroup isclearly established from the previous studies.

The present boninite dyke is intrusive intothe Amgaon gneisses and not in the Dongargarh


Figure 9. CaO/Al2O3 classification for boninites (Crawfordet al. 1989). Boninite compositions from earlier reports suchas Archaean boninite field (Smithies et al. 2004), Bastarboninites (Srivastava 2006; Subba Rao et al. 2008a, b; Cha-lapathi Rao and Srivastava 2009) and Gadwal boninites(Manikyamba et al. 2005) are also given for comparison.

Supergroup rocks unlike the Dongargarh boninitereported by Chalapathi Rao and Srivastava (2009).The Amgaon gneisses of the western Bastar cratonshows widespread ages of 2.5–2.6Ga (Ramakrish-nan and Vaidyanadhan 2008) and forms the base-ment for the Dongargarh Supergroup rocks (Sarkaret al. 1994). The rocks belonging to Dongargarhvolcano-sedimentary successions are exposed to 40–50 km south of the present boninite dyke. Althoughboth the dykes are intruded in different litho-logical units but their proximity may indicatethat both the dykes are younger than the 2.14–2.18Ga Bijli rhyolites (Sarkar et al. 1994; DivakaraRao et al. 2000) but older than the 1.86 Gadyke swarm of the Bastar (Srivastava 2006). Thesouthern Bastar boninites are also reported tobe emplaced at 2118 ± 2 Ma (Srivastava et al.2011). The analogous mineralogical and geochem-ical characteristics of the present dyke with therest of the Bastar boninites may indicate similarmantle source regions for their genesis and thus

Figure 10. (a) Zr (ppm) vs. TiO2 (wt.%), (b) Ti (ppm) vs. Yb (ppm), (c) Ti/Sc vs. Ti/V, and (d) Ti (ppm) vs. Zr (ppm)variation diagram for the present boninite dyke and their comparison with Archaean boninites, Gadwal boninites, Bastarboninites, SHMB, Archaean basalts and komatiites, Phanerozoic arc and oceanic basalts and MORB. Data from Poidevin(1994), Smithies (2002), Polat et al. (2002), Smithies et al. (2004), Manikyamba et al. (2005), Subba Rao et al. (2008a, b)and Chalapathi Rao and Srivastava (2009).


represent a widespread boninite intrusion event inthe Bastar craton during the Palaeoproterozoic.The significant geochemical characteristics corre-sponding with subduction setting also suggest thatlike the Dongargarh boninite, the present dyke(along with north Bastar boninite) represents thepreservation of ancient subduction-related signa-tures retained by the lithospheric mantle of thisdomain during the evolution of the Bastar cratonand Dongargarh Supergroup.

8. Conclusions

The boninite dyke under study shows the pres-ence of mafic minerals such as pyroxenes andamphiboles along with subordinate amounts ofplagioclase. The pyroxenes are mostly diopside incomposition (Wo48−50), whereas amphiboles showthe composition of actinolite and hornblende. Itshows enrichment of LILEs along with depletionof HFSEs (Nb, Ti), and based on low TiO2 (0.19–0.37 wt.%), higher CaO/Al2O3 (3.13–3.96) it isclassified as high Ca boninite. These specific geo-chemical characteristics are consistent with therefractory mantle source formed by the extrac-tion of basaltic magma during Archaean/EarlyProterozoic times in the Bastar craton. The sim-ilarity of the present dyke with the earlier reportedBastar boninites and particularly with north Bas-tar boninite indicates the similar composition ofthe mantle source and a widespread Palaeopro-terozoic boninitic event in the craton. This boni-nite magmatism indicates the presence of remnantsubduction-related signatures in the lithosphericmantle formed during the evolution of the Bastarcraton.

Acknowledgements

We thank the two anonymous reviewers andAssociate Editor R Bhutani for their construc-tive comments and suggestions. BH and DM aregratefull to the Council of Scientific & IndustrialResearch (CSIR), New Delhi and UGC-SAP-DRSfor the financial assistance. AD is thankful to theHead of the Geology Department, SPPU, for thesupport.

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Corresponding editor: Rajneesh Bhutani

petrology and geochemistry of a boninite dyke from the

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