After sonic booms were heard, two stones were recovered in Tamilnadu, Salem, Kakangari, India. One stone was broken into pieces while the other, weighing 347 g, was preserved. Most of this meteorite is accounted for in only four institutions, with the above specimen being obtained through the Natural History Museum in London by an American meteorite dealer.
Kakangari was initially termed an anomalous chondrite. It is a petrologic type 3.6 chondrite that belongs to none of the known chondrite groups, but has some characteristics in common with both ordinary and carbonaceous chondrite groups. Along with the similar petrologic type 3 LEW 87232 (23 g) and the most recently classified type 4 NWA 10085 (52.2 g; Utas et al., 2017, #2906), these three meteorites form a unique grouplet. A fourth meteorite, Lea County 002, was previously considered to share a genetic relationship with the other three K chondrites. However, this has been called into question by some investigators in light of several significant differences: (1) matrix abundance of 33 vol% vs. 6077 vol%, respectively; (2) chondrule size of 1.01.25 mm vs. 0.250.5 mm, respectively; and (3) CAIs in Lea County 002 differ in mineralogy from Kakangari and LEW 87232 (Weisberg et al., 1996; Prinz et al., 1991); CAI data is not yet reported for NWA 10085. Although Lea County 002 is a very small and weathered meteorite, which makes its characterization difficult, it is considered to be mineralogically and isotopically more similar to the CR chondrite group (Krot et al., 2005 and references therein). It should be noted that NWA 10085 most closely resembles Lea County 002, and future recoveries of new K chondrites should help resolve the full range of data which defines this grouplet.
The Kakangari grouplet has unique petrologic and O-isotopic characteristics that distinguish it from other chondrite groups, including the following:
an oxidation state between H and E chondrites
a matrix unlike other chondrite groups (enstatite-rich and compositionally similar to the chondrules)
a high matrix abundance (~70 vol%)
a high metal abundance similar to H group ordinary chondrites
a high troilite abundance (10.5 vol%) with depleted chalcophile element abundances, indicative of large-scale sulfurization
refractory lithophile and siderophile abundances similar to ordinary chondrites
chalcophile elements that plot close to R chondrites
whole-rock O isotopic compositions that plot near the CR chondrites
chondrule O isotopic compositions that plot with the E chondrites
Kakangari consists of about half chondrules and half chondrule fragments, mostly type-I, FeO-poor just as are EH3 chondrules, and they are FeNiFeS-rich. In addition, AOAs and refractory material in the form of irregularly shaped CAIs are present. The relative proportion of chondrule textural-types, predominantly porphyritic and non-porphyritic, is unlike that in other chondrite groups; however, the abundance of POP chondrules is most similar to that of ordinary chondrites. Some porphyritic chondrules contain large metalsulfide intergrowths having ragged outlines, while others contain small metalsulfide beads within olivines and groundmass. Most chondrules and fragments also have metalsulfide rims, but some have fine-grained, igneous-textured silicate rims. The abundance of silicate rims in Kakangari is intermediate to that found in the CV and ordinary chondrites. Layered rims are found on some chondrules, implying that they have experienced at least three melting events with two accretionary episodes. Spongy troilite usually forms the final layer on chondrules and fragments.
The matrix mineralogy preserves the thermal history of Kakangari, revealing peak metamorphic temperatures of <500°C, with an estimated cooling rate of at least 10 K/m.y. (Nagashima et al., 2015 and references therein). Kakangari matrix is composed of both relatively large clastic grains (enstatite, olivine, and clinopyroxene) and aggregates of ultrafine-grained, magnesium-rich, crystalline enstatite and olivine, along with lesser amounts of albite, anorthite, Cr-spinel, troilite, and FeNi-metal (Floss and Stadermann, 2012; Nagashima et al., 2015). The precursor material was likely a mixture of nebular and presolar amorphous or partially crystalline dust. Following thermal metamorphism, which probably caused the destruction of primary presolar grains, a period of rapid cooling ensued resulting in the production of orthoenstatite and clinoenstatite in the matrix. Chondrules and matrix have similar compositions and both experienced reduction processes, likely nebular and parent body, with the chondrules being less reduced than matrix silicates. Kakangari chondrules probably formed from material similar to that from which the matrix formed, but reached higher temperatures necessary for complete melting. Solar-wind-implanted He and Ne suggest a residence in a regolith, with the probability that the meteorite is a breccia. Limited aqueous alteration on the parent body produced ferrihydrite and chlorapatite as replacements for kamacite.
Mineralogical anaysis of Kakangari by Nagashima et al. (2015) revealed a majority of FeO-poor type-I chondrules, with only rare FeO-enriched chondrules (not typical type-II). Although silicates in Kakangari show evidence for reduction processes, silicates in E chondrites were reduced to a greater degree than Kakangari as demonstrated by the more Mg-rich chondrules and the higher content of Cr and Ti in the troilite of E chondrites (Berlin et al., 2007). It was suggested that the FeO-rich silicates observed in both of these groups had a common precursor, despite their differences in degree of reduction. In a broader sense, the K chondrites have a combination of properties that do not fit the existing systematics of either the E, O, R, or C chondrites for which isotopic, chemical, and petrologic characteristics vary smoothly relative to their heliocentric distance of formation. For example, the chondrule/matrix ratio is negatively correlated to the oxidation state through the series E>H>L>LL>C3>CM2>CI1, but the K chondrites do not fit into this sequence. Redox analysis suggests that Kakangari contains a unique suite of chondrules (Berlin et al., 2007).
Generally, the O-isotope composition of the bulk chondrules in Kakangari are 16O-poor and plot along the terrestrial fractionation line on an oxygen three-isotope diagram (ave. olivine: Δ17O +0.0 [±0.8]; ave. low-Ca pyroxene: +0.2 [±0.9]), while that of the matrix olivine and enstatite grains are slightly 16O-enriched by 2.6 (Nagashima et al., 2011, 2015). Analyses show that the matrix grains actually exhibit a bimodal distribution with a majority that are 16O-rich (Δ17O ~ 23.5 [±2.9]) and others that are 16O-poor (Δ17O 0.1 [±1.7]). In accordance with these values, the O-isotope composition of olivines composing a coarse-grained igneous rim on a porphyritic chondrule is 16O-rich (Δ17O ~ 24). As indicated by the O-isotopic data, Nagashima et al. (2015) deduced that Kakangari chondrule and matrix components likely formed from the same nebular reservoir, and that the observed 16O-enrichment in the bulk matrix compared to the 16O-poor bulk chondrules is due to the presence of 16O-rich grains in the matrix.
A NanoSIMS study of Kakangari conducted by Floss and Stadermann (2009, 2012) revealed a single C-anomalous grain (13C-rich), probably SiC from AGB stars, corresponding to an abundance of ~4 ppm. Kakangari also contains relatively low abundances of presolar silicate/oxide grains (< ~5 ppm). Furthermore, there is a complete lack of both O-anomalous presolar grains and amorphous silicates in the matrix. These findings attest to the fact that Kakangari experienced secondary processing, probably on the parent body, and thus cannot be considered a primitive meteorite.
The fusion crust of Kakangari is described as dull and dark brown, exhibiting a close textured, locally ribbed and netted texture (S. Ghosh and A. Dube, 1999). The photos above show a 1.15 g surface fragment of Kakangari dispalying both the fusion-crusted side and the interior.