Mineralogy of Meteorites from the North-Eastern India: A Brief Review

Bhaskar J. Saikia^1*, Gopalakrishnarao Parthasarathy², Rashmi R. Borah³

¹Department of Physics, Anandaram Dhekial Phookan College, Nagaon, India.
²National Geophysical Research Institute (CSIR-NGRI), Hyderabad, India.
³Department of Physics, Nowgong College, Nagaon, India.

DOI: 10.4236/gm.2017.73007                

Abstract

We present a brief overview of meteorites from the north-eastern India, with a focus on falls, finds, and research developments. To date, out of a total 150 numbers of meteorites fall/find in India (in Meteoritical Bulletin Database), only six meteorites from north-eastern region have received official international recognition from the Nomenclature Committee of the Meteoritical Society. Among these six meteorites, 2 finds and 4 falls, including one ureilite, two H chondrites and three L chondrites. The first meteorite from north-eastern India (Assam L5, Find) was documented in 1846. After a lack of 153 years, the first fall (Sabrum LL6 chondrite) was documented in 1999. The most recent fall is Kamargaon (L6) chondrite in 2015. Intensively researched meteorites of this region are Goalpara and Dergaon. The reported most massive meteorite of north-eastern India is Mahadevpur (H4/5) chondrite, 70.5 kg of total known weight, and the rest are <13 kg of total known weight. The researches on these meteorites from north-east India can be applied to the newly recovered meteorites to understand the astrophysical enigma.

Keywords

Meteorite, Mineralogy, North-East India

1. Introduction

Rocks of extraterrestrial origin that penetrate the atmosphere and reach the Earth’s surface are called meteorites. Meteorites recovered following observed falls are called falls; those which cannot definitely be associated with observed falls are called finds [1] . The fall and find of a meteorite is quite rare. The meteorites are classified on the basis of their mineralogy, structure and chemical compositions [2] [3] [4] . The major classification of meteorites is: stony meteorites constituting 92.8% of all meteorites, stony iron meteorites constituting nearly 1.5% and iron meteorites with abundance of 5.7%. The standard method for identifying meteorites is to compare the chemical composition of the sample with that of the meteoritic rock previously studied [5] . The explosive growth of meteorite inventory has been accompanied by a steady growth in the science of meteoritics, and associated fields of observational small body astronomy, cosmochemistry, and astrobiology. The study of meteorites has specific contributions to materials science, e.g., discovery of new minerals, a refinement of our picture of the evolution of the solar system [6] [7] . A multidisciplinary approach to the documentation and interpretation of a meteorite provides interesting opportunities to the understanding of diverse scientific fields (e.g. [8] ). Meteorites provide the most substantial evidence of the chemical and physical makeup of asteroids. The broad objectives of the meteorite studies are to understand the chemical and isotopic composition of the “solar nebula” that evolved to form the solar system objects, formation of the solar system, various physicochemical processes involved to their time scales and the present state of the solar system, connection of solar system with stellar environment, evolution of terrestrial planets including Earth, and to explore the origin and evolution of life and the dynamical processes involved in the meteorite delivery to Earth.

The Meteoritical Bulletin database recorded fall/find of Indian meteorites since 1621 (Appendix Table A1) with two ancient impact craters at Dhala (1700 - 2100 Ma) and Lonar (52000 ± 6000 a) of Madhya Pradesh and Maharashtra respectively. Meteorite studies in India have been initiated in late 1960s. During the journey of Indian meteorite studies, some major outcomes, e.g., scrupulous studies of isotope records in early solar system solids using secondary ion and noble gas mass spectrometry techniques at Physical Research Laboratory, which led to the identification of fossil records of short-lived nuclides of stellar origin in early solar system solids; identification of the short-lived nuclide ²⁶Al as the heat source for early melting of planetesimals, etc. The fall and find of meteorite recovery rate in the north-eastern region of India is very low, yet some very special finds have been recovered (e.g. Goalpara).

2. Meteorites Fall/Find in North-East India

Here is a quick chronological survey of all meteorites from north-east India, including some of the most extensively-researched examples, with emphasis on the subjects of research in this field. Table 1 represents the meteorites fall/find in north-east India.

The meteorite documentation era of north-eastern region of India was started with the documented meteorite Assam L5 (1846) by Silberrad [9] . It is worthwhile to mention that, out of 150 documented meteorites from India (to date), only six meteorites have been officially recognized by Nomenclature Committee of the Meteoritical Society from north-eastern region of India with various sizes and chemical classes.

Table 1. List of meteorites fall/find in north-east India during last two centuries.

3. Studies on these Meteorites

Assam (26˚00'N; 92˚00'E) is the first documented meteorite “find” in North- eastern India. Total known weight of this meteorite was 2.7 kg in the form of three fragments, was recovered from Meghalaya in 1846 [9] . Assam is a fine representative of one of the most abundant meteorite classes L5 chondrite.

Goalpara (26˚10'N, 90˚36'E) meteorite is “find” in 1868, a stony meteorite belong to ureilite achondrite. In last few decades it has become arguably the most- researched meteorite from north-east India. Ureilite-achondrite is a rare type of stony meteorite that has a unique mineralogical composition, which is very different from that of other stony meteorites. It has seen a level of research being described in various articles. The total known mass of this meteorite is 2.7 kg and it is the massive of all Indian ureilites. Goalpara was the most massive ureilites known before the recovery of the Kenna ureilite in 1972. Only three of this rare class has been documented from India, among them, except Goalpara, both Dyalpur (1872) and Lahrauli (1955) are fall. Ureilites contain slightly high amounts of trace elements like Cr, Mn and Zn, but the distribution of trace elements like zinc between different silicate mineral phases is not well known. Bulk zinc contents of the more heavily shocked ureilites are lower compared to the weakly shocked ureilites. The reason for the low levels of zinc in Goalpara olivines is not yet understood [10] . The Goalpara is one of the heavily shocked ureilites which contains lonsdaleite together with diamond (see [11] ). Goalpura meteorite has been identified as a stony meteorite that lacks chondrules and originated on a differentiated parent body. The petrographic studies of Goodrich also indicate Goalpara experienced higher shock pressures and temperatures [12] . Presence of lonsdaleite and diamond in carbon grains of Goalpara ureilite was reported by many authors (e.g. [11] [13] [14] ). Generally, lonsdaleite is not found weakly shocked ureilites. Nakamuta and Toh (2013) observed coarse-grained olivine and pigeonite with minor amounts of blade-like shaped carbon grains and mosaic texture of olivine and pyroxene crystals in Goalpara ureilite. The well crystallized graphite coexisted with olivine and pyroxene during igneous processes is converted to high-pressure diamond by impact (see [15] [16] ), which suggests that the meteorite has been heavily shocked [17] . Other polymorphous of carbon (e.g. chaoite and graphite) are also found in Goalpara ureilite. The black, fine grained agglomerates, a few tenths of 1 mm in sized diamond in Goalpara and Dyalpur are formed under shock above 160 kb. In Goalpara ureilite, diamonds are mainly cubic, with less than 10 percent hexagonal (see [11] ). According to Hanneman et al, there is no evidence of hexagonal diamonds of terrestrial origin and also cubic diamond cannot be transformed into hexagonal under static or shocked pressure combined with temperature. Therefore, they conclude that the diamonds found in Goalpara ureilite were formed by impact shock in space from well crystallized graphite existing with the meteorite before impact [11] .

Sabrum (23˚05'N; 91˚40'E) is one of the six Indian LL6 chondrites, among Segowlie (1853), Dhurmsala (1860), Manbhoom (1863), Bhawad (2002) and Sulagiri (2008) of this class. It is the first documented “fall” of this region. The total known weight of Sabrum is 478 g. The major mineral composition of Sabrum is olivine (Fa_31.4), orthopyroxene (Fs_25.1, Wo_2.0), clinopyroxene (Wo₄₅En_45.6Fs_9.4) and plagioclase (An_10.6Ab_83.6Or_5.8) [18] . This meteorite is belongs to S4 category with moderate shock features and the exposure age 24.8 Ma. The activities of most of the short-lived isotopes indicate the low galactic cosmic-ray fluxes over the orbital space of the meteoroid during the last few years prior to its fall. The observed cosmic-ray f1uxes of Sabrum corresponding to the solar quiet period between cycles 22 and 23 appear to be anomalously low and require further investigation (see [18] ).

Dergaon (26˚42'N, 93˚51'E) is the fourth meteorite “fall” in north-east India (Figure 1). It is also an exhaustively studied meteorite of this region. A multiple fell of meteorite was observed on 2nd March, 2001, with a fireball accompanied by two land detonations. The largest fragment, weighing 10.3 kg, was recovered in the village of Balidua, ten km west of Dergaon town. Additional fragments were recovered in the village of Koilaghat of weighing about 1.5 kg and two fragments, each of weighing about 1 kg, were recovered in Majuli. The possibilities of other fragments fell in the Brahmaputra River channels cannot be ignored. The total known weight of this meteorite is 12.5 kg. This fall is classified and documented as Dergaon H5 chondrite [19] . The detail focussed on integrated petrology, bulk chemistry, oxygen isotopes, noble gas and cosmic ray track density of Dergaon reported by Shukla et al. (see [20] ). A cosmic ray exposure of 9.7 Ma for Dergaon is inferred from the cosmogenic noble gas records (see [20] ). Dergaon is a classic example of H chondrite with high chondrule- matrix ratio. The chondrules of Dergaon contains porphyritic olivine, porphyritic

Figure 1. Photographs of some meteorites fell in North-eastern India. (a) Dergaon H5; (b) Mahadevpur H4/5; (c) Kamargaon L6.

pyroxene, porphyritic olivine pyroxene, barred olivine, and barred pyroxene nearly 75% and about 25% non-porphyritic chondrules mainly radial pyroxene, cryptocrystalline, granular pyroxene and glassy ( [21] , see [22] ). The lower value of K makes Dergaon notable among the H chondrites. The volatile elements such as Zn and Se are also absent in this meteorite. Besides olivine, orthopyroxene and clinopyroxene, kamacite and rare occurrences of taenite are also observed as exsolved lamellae in the metallic phases. Ray et al., has presented a reasonable explanation for bulk K depletion, interpretation of chondrule formation and shock-thermal history of the Dergaon. The vesicular texture in shock- melted feldspar and concomitant loss of K were attained during the post-shock decompression stage under low pressure (see [22] ). The infrared stretching features of aliphatic hydrocarbon in Dergaon were reported by Saikia et al [23] [24] . The weathering of the meteorite sample cannot be overlooked for presence of these features. To date, Dergaon is one of the fifteen documented Indian H5 chondrites.

Mahadevpur (27˚40'N, 95˚47'E) of total known weight 70.5 kg, is the largest documented multiple fall of north-eastern India [25] [26] . The largest fragment, weighing 60 kg (Figure 1), was recovered in Pangari, about 40 km away from Mahadevpur. To date, only two Indian meteorites has classified of type H4/5. (i.e. Mahadevpur (2007) and Kendrapara (2003) chondrite). The mineralogical phases of olivine in Mahadevpur are: olivine (Fo_80.8Fa_19.3), orthopyroxene (En₈₁ Fs₁₇Wo₁), and clinopyroxene (En₅₈Fs₈Wo₃₅) [27] , albitic plagioclase (Ab₈₇ Or₃An₁₀), kamacite, taenite, apatite and rare chromite [25] . The matrix is a heterogeneous mixture of chondrule fragments, olivine, ortho-pyroxene and plagioclase. Chondrule sizes range from 250 to 1300 mm. The Raman and infrared spectroscopic analysis of Mahadevpur reflects a partially polymerized silicate framework [27] [28] . Red luminescence characteristic features of olivine in Mahadevpur by Laser-induced fluorescence (LIF) are also reported by Dehingia and Baruah [29] . Olivine in chondrules and matrix do not show compositional variation, suggesting that Mahadevpur is an equilibrated H-chondrite. The noble gas analyses suggest the exposure age of Mahadevpur is 6 Ma (see [30] ).

Kamargaon (26˚39'01''N; 93˚46'02''E) is the most recent fall of north-eastern India (Figure 1). A single stone fell from clear sky at the mustard oil cultivation field of the Bali-chapari village, near Kamargaon town in Golaghat District of Assam, India, on 13th November 2015 at 12:00 hrs (Local time) with fireball and a tremendous sound [31] [32] . The stone was fully covered with fusion crust and had well rounded edges and well developed regmaglypts (thumbprint like impressions) on its surface, that are formed by ablation of material from the surface as a meteor passes through the Earth’s atmosphere. The strike of the meteorite makes a crater of 1.5 ft diameter and penetrated the ground 3ft in depth. A single piece of meteorite of weight 12.095 kg is recovered and preserved under the custodian of the local police station. The fusion crust (about 1 mm of thickness) and the regmaglypths are clearly visible on the surface of Kamargaon meteorite. The olivine composition is estimated to Fo: 78.98 mol %; Fa: 20.80 mol % and Tp: 0.88 mol %. The bulk chemical composition and mineralogical data indicates that the Kamargaon meteorite is an L6 chondrite. In Kamargaon, ²²Na/²⁶Al activities ratio is lower than expected values for an L chondrite fall during the declining stage of solar cycle 24 [33] .

4. Conclusion

All meteorites from north-eastern India were belongs to ordinary chondrites except Goalpara, which is stony achondrite. The studies of meteoritic olivine of these meteorites have been reported by many authors (e.g. [18] [34] [35] [36] [37] ). The carbon polymorphous hexagonal diamond is usually formed in static and shock high pressure. The presence of diamond in Goalpara reflects this phase of temperature and pressure condition under which these diamonds are formed. The crystalline graphite is the main source of the meteoritic diamonds in Goalpara. Presence of nanodiamonds in Dergaon and Mahadevpur is also reported by Saikia et al. (see [38] ). This finding has important implications concerning the origin of meteoritic diamonds. As the meteorites from north-east India are most common type chondrites, they originate from debris of the solar nebula (e.g. [7] [39] ). Due to their unique origin, these chondrites are also regarded as the sole witness for the formation of the early solar system. For example, Dergaon chondrite reports several significant observations that help to understand both nebular and asteroidal processes (e.g. [22] ). Meteorites still hold many secrets about our earth and other solar system bodies that are yet to be deciphered. The researches on the meteorites from north-east India will undeniably contribute to the understanding and demystify these secrets.

Acknowledgements

This paper is dedicated to 72^nd Birthday of Professor N.C. Sarmah, Department of Physics, Dibrugarh University, Dibrugarh. We are grateful to Professor N. Bhandari of Physical Research Laboratory, Ahmedabad for motivation and mentoring. G.P. thanks PLANEX, Physical Research Laboratory for funding.

Appendix

Table A1. List of meteorites from India (https://www.lpi.usra.edu/meteor/index.php accessed on 24.04.2017).

**Meteorites fall/find in north-eastern India.

Conflicts of Interest

The authors declare no conflicts of interest.

References

[1]	Krot, A.N., Keil, K., Goodrich, C.A., Scott, E.R.D. and Weisberg, M.K., (2005) Classification of Meteorites. In: Davis, A.M., Ed., Meteorites, Comets, and Planets: Treatise on Geochemistry, Elsevier-Pergamon, Oxford, 84-128.
[2]	Larimer, J.W. (1971) Composition of the Earth: Chondritic or Achondritic? Geochimica et Cosmochimica Acta, 35,769-786. https://doi.org/10.1016/0016-7037(71)90125-6
[3]	Oura, Y., Ebihara, M., Yoneda, S. and Nakamura, N. (2002) Chemical Composition of the Kobe Meteorite; Neutron-Induced Prompt Gamma Ray Analysis Study. Geochemical Journal, 36, 298-307. https://doi.org/10.2343/geochemj.36.295
[4]	Randa, Z., Kucera, J. and Soukal, L. (2003) Elemental Characterization of the New Czech Meteorite “Moravka” by Neutron and Photon Activation Analysis. Journal of Radioanalytical and Nuclear Chemistry, 257, 275-283. https://doi.org/10.1023/A:1024767309558
[5]	Nair, A.G.C., Acharya, R., Sudarshan, K., Gangotra, S., Reddy, A.V.R., Manohar, S.B. and Goswami, A. (2003) Development of an Internal Mono Standard INAA Method Based on in situ Detection Efficiency for Analysis of Large and Non-Standard Geometry Samples. Analytical Chemistry, 75, 4868-4874. https://doi.org/10.1021/ac034457d
[6]	McSween, H.Y. (1999) Meteorites and Their Parent Bodies. Cambridge University Press, Cambridge.
[7]	Hutchison, R. (2004) Meteorites: A Petrologic, Chemical and Isotopic Synthesis. Cambridge University Press, Cambridge.
[8]	Brown, P.G., Hildebrand, A.R., Zolensky, M.E., Grady, M., Clayton, R.N., Mayeda, T.K., Tagliaferri, E., Spalding, R., MacRae, N.D., Hoffman, E.L., Mittlefehldt, D.W., Wacker, J.F., Bird, J.A., Campbell, M.D., Carpenter, R., Gingerich, H., Glatiotis, M., Greiner, E., Mazur, M.J., McCausland, P.J., Plotkin, H. and Mazur, T.R. (2000) The Fall, Recovery, Orbit, and Composition of the Tagish Lake Meteorite: A New Type of Carbonaceous Chondrite. Science, 290, 320-325. https://doi.org/10.1126/science.290.5490.320
[9]	Silberrad, C.A. (1932) List of Indian Meteorites. 290-304. https://doi.org/10.1180/minmag.1932.023.139.05
[10]	Wasson, J.T., Chou, C.L., Bild, R.W. and Baedecker, P.A. (1976) Classification of an Elemental Fractionation among Ureilites. Geochimica et Cosmochimica Acta, 40, 1449-1450. https://doi.org/10.1016/0016-7037(76)90081-8
[11]	Hanneman, R.E., Strong, H.M. and Bundy, F.P. (1967) Hexagonal Diamonds in Meteorites: Implications. Science, 155, 995-997. https://doi.org/10.1126/science.155.3765.995
[12]	Goodrich, C.A. (1992) Ureilites: A Critical Review. Meteoritics & Planetary Science, 27, 327-352. https://doi.org/10.1111/j.1945-5100.1992.tb00215.x
[13]	Bundy, F.P. and Kasper, J.S. (1967) Hexagonal Diamond—A New Form of Carbon. The Journal of Chemical Physics, 46, 3437-3446. https://doi.org/10.1063/1.1841236
[14]	Frondel, C. and Marvin, U.B. (1967) Lonsdaleite, a Hexagonal Polymorph of Diamond. Nature, 214, 587-589. https://doi.org/10.1038/214587a0
[15]	Goodrich, C.A., Scott, E.R.D. and Fioretti, A.M. (2004) Ureilitic Breccias: Clues to the Petrologic Structure and Impact Disruption of the Ureilite Parent Asteroid. Chemie der Erde-Geochemistry, 64, 283-327.
[16]	Nakamuta, Y. and Aoki, Y. (2000) Mineralogical Evidence for the Origin of Diamond in Ureilites. Meteoritics & Planetary Science, 35, 487-493. https://doi.org/10.1111/j.1945-5100.2000.tb01430.x
[17]	Nakamuta, Y. and Toh, S. (2013) Transformation of Graphite to Lonsdaleite and Diamond in Goalpara Ureilite Directly Observed by TEM. American Mineralogist, 98, 574-581. https://doi.org/10.2138/am.2013.4341
[18]	Ghosh, S., Murty, S.V.S., Shukla, P.N., Shukla, A.D., Mahajan, R.R., Bhandari, N., Pant, N.C., Ghosh, J.B. and Shome, S. (2002) Fall, Classification and Cosmogenic Records of the Sabrum (LL6) Chondrite. Meteoritics & Planetary Science, 37, 439-448. https://doi.org/10.1111/j.1945-5100.2002.tb00826.x
[19]	Grossman, J.N. and Zipfel, J. (2001) The Meteoritical Bulletin, No. 85, 2001 September. Meteritics & Planetary Science, 36, A293-A322. https://doi.org/10.1111/j.1945-5100.2001.tb01542.x
[20]	Shukla, P.N., Shukla, A.D., Rai, V.K., Murthy, S.V.S., Bhandari, N., Goswami, J.N., Mazumder, A.C., Phukon, K., Duorah, K., Greenwood, R.E. and Franchi, I.A. (2005) The Dergaon (H5) Chondrite: Fall, Classification, Petrological and Chemical Characteristics, Cosmogenic Effects, and Noble Gas Records. Meteoritics & Planetary Science, 40, 627-637. https://doi.org/10.1111/j.1945-5100.2005.tb00967.x
[21]	Wasson, J.T., Krot, A.N., Lee, M.S. and Rubin, A.E. (1995) Compound Chondrules. Geochimica et Cosmochimica Acta, 59, 1847-1869.
[22]	Ray, D., et al. (2016) Insights into Chondrule Formation Process and Shock-Thermal History of the Dergaon Chondrite (H4-5). Geoscience Frontiers, 8, 413-423.
[23]	Saikia, B.J., Parthasarathy, G. and Sarmah, N.C. (2009) Fourier Transform Infrared Spectroscopic Characterization of Dergaon H5 Chondrite: Evidence of Aliphatic Organic Compound. Nature and Science, 7, 45-51.
[24]	Saikia, B.J., Parthasarathy, G., Sarmah, N.C. and Baruah, G.D. (2009) Organic Compounds in H5 Meteorite: Spectroscopic Investigation of Dergaon H5 Chondrite. Geochimica et Cosmochimica Acta, 71, 867.
[25]	Weisberg, M.K., Smith, C., Benedix, G., Foloco, L., Righter, K., Zipfel, J., Yamaguchi, A. and Chennaouiaoudjehane, H. (2008) The Meteoritical Bulletin, No. 94. September 2008. Meteoritics & Planetary Science, 43, 1551-1588. https://doi.org/10.1111/j.1945-5100.2008.tb01027.x
[26]	Saikia, B.J. and Parthasarathy, G. (2009) Spectroscopic Investigation of Mahadevpur H4/5 Ordinary Chondrite. Geochimica et Cosmochimica Acta, 73, 1144.
[27]	Saikia, B.J., Parthasarathy, G. and Sarmah, N.C. (2009) Spectroscopic Characterization of Olivine[(Fe, Mg)2SiO4] in Mahadevpur H4/5 Ordinary Chondrite. Journal of American Science, 5, 71-78.
[28]	Saikia, B.J., Parthasarathy, G., Borah, R.R. and Borthakur, R. (2016) Raman spectroscopic Study of Dergaon H5 and Mahadevpur H4/5 Chondrite. 47th Lunar and Planetary Science Conference, No. 1799.
[29]	Dehingia, N. and Baruah, G.D. (2010) Extended Red Emission in Mahadevpur (Namsai) Meteorite. Spectroscopy Letters, 43, 144-147. https://doi.org/10.1080/00387010903261198
[30]	Murty, S.V.S., Mahajan, R.R., Shukla, A.D., Mazumdar, A.C., Shukla, P.N., Durga Peasad, K., Rai, V.K., Panda, D., Ghevaria, Z.G. and Goswami, J.N. (2009) Jodia (L5) and Mahadevpur (H4/5): Twp Recent Ordinary Chondrites Falls in India. 72nd Annual Meteoritical Society Meeting, No. 5058.
[31]	Goswami, T.K., Ray, D., Sarmah, R.K., Goswami, U., Bhattacharyya, P., Majumdar, D., Bezbaruah, D. and Borgohain, P. (2016) Meteorite Fall at Komargaon, Assam, India. Current Science, 110, 1894-1895.
[32]	Saikia, B.J., Parthasarathy, G. and Borah, R.R. (2017) Raman Spectroscopy of Kamargaon L6 Ordinary Chondrite. 48th Lunar and Planetary Science Conference, No. 1979.
[33]	Rosén, A.V., Sivers, M.V., Hofmann, B.A., Schumann, M. and Pathak, D. (2016) Cosmogenic Radionuclides in the Komar Gaon Meteorite Measured in a New Low-Background Gamma-Ray Spectrometry Facility, GeMSE. 79th Annual Meeting of the Meteoritical Society, No. 6398.
[34]	Bhattacharyya, S., Gohainbarua, A., Knowar, R., Changmai, R. and Baruah, G.D. (2004) Nature of the Emission Band of Dergaon Meteorite in the Region 5700-6700 A. Pramana, 62, 1299-1301. https://doi.org/10.1007/BF02704442
[35]	Gohainbarua, A., Barua, B.P., Bhattachyya, S. and Baruah, G.D. (2003) Spectroscopic Investigation of Dergaon Meteorite with Reference to 10 μm and 20 μm Bands. Pramana, 60, 47-52. https://doi.org/10.1007/BF02705067
[36]	Saikia, B.J. and Parthasarathy, G. (2008) Spectroscopy of Dergaon Meteorite. Geochimica et Cosmochimica Acta, 72, 818.
[37]	Saikia, B.J., Parthasarathy, G. and Borah, R.R. (2011) Spectroscopic Characterization of Olivine Due to Fe/Mg in Dergaon Chondrite. Mineralogical Magazine, 75, 1780.
[38]	Saikia, B.J., Parthasarathy, G. and Borah, R.R. (2017) Nanodiamonds and Silicate Minerals in Ordinary Chondrites as Determined by Micro-Raman Spectroscopy. Meteoritics & Planetary Science, 52, 1146-1154. https://doi.org/10.1111/maps.12850
[39]	Zanda, B. (2004) Chondrules. Earth and Planetary Science Letters, 224, 1-17