Piplia Kalan eucrite: Fall, petrography and chemical characteristics

Shukla, A. D.; Shukla, P. N.; Suthar, K. M.; Bhandari, N.; Vaya, V. K.; Sisodia, M. S.; Roy, Subimal Sinha; Rao, K. N.; Rajawat, R. S.

doi:10.1111/j.1945-5100.1997.tb01546.x

Cited by 21 publications

(12 citation statements)

References 8 publications

(5 reference statements)

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“…PRA 04401 is plotted as measured (low Al, Ca) and after correction for approximately 55% CM clast content (see text). Howardite and polymict eucrite data are from this study; literature data are from Allen and Mason (), Cleverly et al (), Duke and Silver (), Fitzgerald (), Ghosh et al (), Jarosewich (), Jérome (), Kharitonova & Barsukova (), Kolesov & Hernandez (), Lovering (), Marvin and Mason (), Mason (), Mason and Jarosewich (), Mason et al (), McCarthy et al (, , ), von Michaelis et al (), Mittlefehldt et al (), Shima (), Shukla et al (), Simpson (), Symes and Hutchison (), Takeda (), Takeda et al (, , ), Yanai et al ().…”

Section: Bulk Composition Resultsmentioning

confidence: 96%

Composition and petrology of HED polymict breccias: The regolith of (4) Vesta

Mittlefehldt

Herrin²,

Quinn³

et al. 2013

Meteorit & Planetary Scien

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† This study is dedicated to the memory of friend and colleague David S. McKay, who taught us much about the regoliths of airless bodies.Abstract-We have done petrologic and compositional studies on a suite of polymict eucrites and howardites to better understand regolith processes on their parent asteroid, which we accept is (4) Vesta. Taking into account noble gas results from companion studies, we interpret five howardites to represent breccias assembled from the true regolith: Elephant Moraine (EET) 87513, Grosvenor Mountains (GRO) 95535, GRO 95602, Lewis Cliff (LEW) 85313, and Meteorite Hills (MET) 00423. We suggest that EET 87503 is paired with EET 87513, and thus is also regolithic. Pecora Escarpment (PCA) 02066 is dominated by melt-matrix clasts, which may have been formed from true regolith by impact melting. These meteorites display a range in eucrite:diogenite mixing ratio from 55:45 to 76:24. There is no correlation between degree of regolith character and Ni content. The Ni contents of howardite, eucrite, and diogenites (HEDs) are mostly controlled by the distribution of coarse chondritic clasts and metal grains, which in some cases resulted from individual, lowvelocity accretion events, rather than extensive regolith gardening. Trace element compositions indicate that the mafic component of HED polymict breccias is mostly basalt similar to main-group eucrites; Stannern-trend basaltic debris is less common. Pyroxene compositions show that some trace element-rich howardites contain abundant debris from evolved basalts, and that cumulate gabbro debris is present in some breccias. The scale of heterogeneity varies considerably; regolithic howardite EET 87513 is more homogeneous than fragmental howardite Queen Alexandra Range (QUE) 97001. Individual samples of a given howardite can have different compositions even at roughly 5 g masses, indicating that obtaining representative meteorite compositions requires multiple or large samples.

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Section: Bulk Composition Resultsmentioning

confidence: 96%

Composition and petrology of HED polymict breccias: The regolith of (4) Vesta

Mittlefehldt

Herrin²,

Quinn³

et al. 2013

Meteorit & Planetary Scien

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“…These samples together with standards(Allende(CV3), Dhajala (H3.8), BCR-l and AGV-l) were irradiated in Dhruva reactor of Bhabha Atomic Research Center, Mumbai. The irradiated samples were counted at different intervals of time on a high-purity Ge detector (148 em") located in 10 em thick lead shield following standard procedures (Laul, 1979;Shukla et al, 1997). In this way concentrations of AI, Mg, Ca, Ti, Mn, Fe, Ni, Na and K were determined using ICP-AES/AAS and elements such as Fe, Ni, Co, Cr, Na, K, Zn, Sc, La, Ce, Sm, Eu, Yb, Ir, Os and Au were determined using INAA procedures.…”

Section: Chemical Analysismentioning

confidence: 99%

Itawa Bhopji (L3–5) chondrite regolith breccia: Fall, classification, and cosmogenic records

Bhandari

Murty

Shukla

et al. 2002

Meteorit & Planetary Scien

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Abstract-A stony meteorite fell at Itawa Bhopji, Rajasthan, India on 2000 May 30. This is the fifth recorded fall in a small area of Rajasthan during the past decade. The meteorite is an ordinary chondrite with light clasts in a dark matrix, consisting of a mixture of equilibrated (mainly type 5) and unequilibrated components. Olivine is Fa24-26 and pyroxene FS 20-22 but, within the unequilibrated components, olivine (Fa5-29) and low calcium pyroxene (FS 5-37) are highly variable. Based on petrographic studies and chemical analyses, it is classified as L(3-5) regolith breccia. Studies of various cosmogenic records, including several gamma-emitting radionuclides varying in half-life from 5.6 day 52Mn to 0.73 Ma 26AI, tracks and rare gases have been carried out. The exposure age of the meteorite is estimated from cosmogenic components ofrare gases to be 19.6 Ma. The track density varies by a factor of -3 (from 4 to 12 x 10 6/cm2) within the meteorite, indicating a preatmospheric body of -9 ern radius (corresponding to a meteoroid mass of -11 kg) and small ablation (1.5 to 3.6 ern). Trapped components in various rare gases are high and the solar component is present in the dark portion of the meteorite. Large excess of neutron-produced 82Kr and 128Xe in both the light and the dark lithology but very low 60Co, indicating low neutron fluxes received by the meteoroid in the interplanetary space, are clear signatures of an additional irradiation on the parent body.

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“…The irradiated samples were counted using a high-purity Ge detector (148 cm 3 ) housed within 10 cm thick lead shield. The procedures are described by Laul (1979) and Shukla et al (1997). Concentrations of Al, Mg, Ca, Mn, Fe, Ni, Na and K were determined using ICP-AES/AAS, while concentrations of other elements, such as, Co, Cr, Zn, Se, As, Sc, La, Sm, Eu, Yb, Ir, Os, and Au as well as Fe, Ni, and Na were determined using INAA procedures.…”

Section: Samples and Experimental Approachmentioning

confidence: 99%

The Dergaon (H5) chondrite: Fall, classification, petrological and chemical characteristics, cosmogenic effects, and noble gas records

Shukla

Vinai

et al. 2005

Meteoritics &Amp; Planetary Science

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. Several fragments weighing <2 kg and a single large fragment weighing ∼10 kg were recovered from the strewn field, which extended over several tens of square kilometers. Chemical, petrographic, and oxygen isotopic studies indicate it to be, in most aspects, a typical H5 chondrite, except the unusually low K content of ∼340 ppm. A cosmic ray exposure of 9.7 Ma is inferred from the cosmogenic noble gas records. Activities of eleven cosmogenic radionuclides were measured. 26 Al and 22 Na activities as well as the 22 Na/ 26 Al activity ratio are close to the values expected on the basis of solar modulation of galactic cosmic rays. The low 60 Co activity (<1 dpm/kg) is indicative of a small preatmospheric size of the meteorite. Cosmic ray heavy nuclei track densities in olivine grains range from ∼10 6 cm −2 in samples from the largest fragment to approximately (4-9) × 10 5 cm −2 in one of the smaller fragments. The combined track, radionuclide, and noble gas data suggest a preatmospheric radius of ∼20 cm for the Dergaon meteorite.

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Piplia Kalan eucrite: Fall, petrography and chemical characteristics

Cited by 21 publications

References 8 publications

Composition and petrology of HED polymict breccias: The regolith of (4) Vesta

Composition and petrology of HED polymict breccias: The regolith of (4) Vesta

Itawa Bhopji (L3–5) chondrite regolith breccia: Fall, classification, and cosmogenic records

The Dergaon (H5) chondrite: Fall, classification, petrological and chemical characteristics, cosmogenic effects, and noble gas records

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