Formation of metal and silicate globules in Gujba: a new Bencubbin-like meteorite fall

Rubin, Alan E.; Kallemeyn, G. W.; Wasson, J. T.; Clayton, Robert N.; Mayeda, T. K.; Grady, M. M.; Verchovsky, A. B.; Eugster, O.; Lorenzetti, Silvio

doi:10.1016/s0016-7037(03)00098-x

Cited by 125 publications

(140 citation statements)

References 49 publications

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“…These properties include (1) a broad compositional range of FeNi-metal, which is characterized by an approximately solar CofNi ratio; (2) large depletions in moderately volatile elements, such as Mn, Na, K, Ga, Ge, and S; (3) bulk oxygen isotopic compositions plotting on or near the CR-mixing line on a three-isotope diagram; and (4) large positive anomalies in ol5N (Herzog et al, 2000;Weisberg et al, 1993Weisberg et al, , 1995Weisberg et al, ,2001Rubin et al, 2001;Krot et al, unpubl. data).…”

Section: Introductionmentioning

confidence: 99%

Heavily‐hydrated lithic clasts in CH chondrites and the related, metal‐rich chondrites Queen Alexandra Range 94411 and Hammadah al Hamra 237

Greshake

Krot

Meibom

et al. 2002

Meteorit & Planetary Scien

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Abstract-Fine-grained, heavily-hydrated lithic clasts in the metal-rich (CB) chondrites Queen Alexandra Range (QUE) 94411 and Hammadah al Hamra 237 and CH chondrites, such as Patuxent Range (PAT) 91546 and Allan Hills (ALH) 85085, are mineralogically similar suggesting genetic relationship between these meteorites. These clasts contain no anhydrous silicates and consist of framboidal and platelet magnetite, prismatic sulfides (pentlandite and pyrrhotite), and Fe-Mn-Mg-bearing Ca-carbonates set in a phyllosilicate-rich matrix. Two types of phyllosilicates were identified: serpentine, with basal spacing of~O.73 nm, and saponite, with basal spacings of about 1.1-1.2 nm. Chondrules and FeNi-metal grains in CB and CH chondrites are believed to have formed at high temperature (> 1300 K) by condensation in a solar nebula region that experienced complete vaporization. The absence of aqueous alteration of chondrules and metal grains in CB and CH chondrites indicates that the clasts experienced hydration in an asteroidal setting prior to incorporation into the CH and CB parent bodies. The hydrated clasts were either incorporated during regolith gardening or accreted together with chondrules and FeNi-metal grains after these high-temperature components had been transported from their hot formation region to a much colder region of the solar nebula.

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Section: Introductionmentioning

confidence: 99%

Heavily‐hydrated lithic clasts in CH chondrites and the related, metal‐rich chondrites Queen Alexandra Range 94411 and Hammadah al Hamra 237

Greshake

Krot

Meibom

et al. 2002

Meteorit & Planetary Scien

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“…The origin of the chondrules and metal grains in CB chondrites is less certain as they have very distinctive properties and clearly formed under unusual circumstances, possibly in a planetary impact Rubin et al, 2003). Nevertheless, the presence in CB chondrites of CAIs and highly altered matrix-rich inclusions, as in most other chondrites, suggests that the CB chondrules and metal grains accreted from the nebula when it was still turbulent and capable of mixing materials that formed at diverse nebular locations and times (Cuzzi et al, 2003).…”

mentioning

confidence: 99%

Meteoritical and dynamical constraints on the growth mechanisms and formation times of asteroids and Jupiter

Scott

2006

Icarus

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“…Amelin et al (2004) and Amelin and Krot (2005) further reported absolute ages of chondrules from Allende, Gujba (CB), and Hammadah al Hamra 237 (CB) of 4.5667 (± 0.0010) Ga, 4.5627 (± 0.0005) Ga, and 4.5628 (± 0.0009) Ga, respectively. Considering that chondrules from CB chondrites may have been produced by impact related processes on the parent body and may not be products in the protoplanetary disk (Rubin et al, 2003), the difference between the Pb Pb ages of CAIs and chondrules suggest that chondrule formation started contemporaneously with or shortly after CAI formation and lasted for ~ 2 Myr. Petrographical evidence from CAI bearing chondrules and chondrule bearing CAIs (Itoh and Yurimoto, 2003;Krot et al, 2005) supports these dating results.…”

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confidence: 99%

Chondrule formation and evolution of the early solar system

Tachibana¹

2006

Journal of Mineralogical and Petrological Sciences

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Chondrules are millimeter to sub millimeter size silicate spherules that formed during localized and transient high temperature events in the early solar system. Although it is not yet understood how chondrules formed, recent studies have provided important clues in understanding the physical conditions of chondrule formation. In this paper I review recent developments in studies of chondrules to provide constraints on high temperature processes during the evolution of protoplanetary disks, including: (1) the timing and duration of the chondrule forming high temperature period, based on long lived and short lived chronometers; (2) the thermal history of chondrule melts during each chondrule forming event, as constrained from laboratory experiments and petrological and isotopic studies of chondrules, including shock wave heating as a plausible heat source for chondrule formation; and (3) sources for shock waves and chondrule forming regions in the protoplanetary disk. Given our current knowledge, I provide the following possible answers to the above four points: (1) the period of chondrule formation began shortly after the formation of calcium aluminum rich inclusions and lasted for a few million years; (2) chondrule precursors were heated at a rate of > 10 4 K/h in the temperature range of ~ 1400 1600 K, and melt droplets were cooled from a peak temperature of ~ 1800 2200 K at a rate of ~ 5 1000 K/h; (3) high velocity shock waves (> 20 km/s) in a low density gas region (< 10 19 particles/m 3 ) may be appropriate for localized transient heating events associated with chondrule formation; and (4) X ray flares from the young Sun in its T Tauri stage might be the source of the shock waves.

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Formation of metal and silicate globules in Gujba: a new Bencubbin-like meteorite fall

Cited by 125 publications

References 49 publications

Heavily‐hydrated lithic clasts in CH chondrites and the related, metal‐rich chondrites Queen Alexandra Range 94411 and Hammadah al Hamra 237

Heavily‐hydrated lithic clasts in CH chondrites and the related, metal‐rich chondrites Queen Alexandra Range 94411 and Hammadah al Hamra 237

Meteoritical and dynamical constraints on the growth mechanisms and formation times of asteroids and Jupiter

Chondrule formation and evolution of the early solar system

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