H/L chondrite LaPaz Icefield 031047 – A feather of Icarus?

Wittmann, A.; Friedrich, J. M.; Troiano, Julianne M.; Macke, R. J.; Britt, D. T.; Swindle, T. D.; Weirich, J. R.; Rumble, Douglas; Lasue, J.; Kring, D. A.

doi:10.1016/j.gca.2011.07.037

Cited by 32 publications

(19 citation statements)

References 71 publications

(102 reference statements)

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“…), or such asteroids like 2008 FF5 (Wittmann et al. ). One or more subsequent disruption and re‐assembly events could then rebury the heated material into a region of the asteroid that once again experienced aqueous alteration, and possibly further metamorphism.…”

Section: Discussionmentioning

confidence: 99%

“…The evidence from our experiments does indicate that MCCs and CM2s could have evolved from a common precursor in result from cycle(s) of hydration-dehydration processes. The water for that could be formed from asteroid ice by heating, and the source(s) of heat for the protoplanets and minor bodies to melt the ice could be (1) energy from the decay of short-lived radionuclides (Grimm and McSween 1989;Miyamoto 1991); (2) impact events where MCC material was far from the impact crater and only heated up to the temperature of melting ice (Davison et al 2012); (3) MCC material could be formed at the surface of asteroids with perihelion near the Sun, such as Phaethon (Ohtsuka et al 2007(Ohtsuka et al , 2009), Icarus (Licanrdo et al 2007), or such asteroids like 2008 FF5 (Wittmann et al 2011). One or more subsequent disruption and re-assembly events could then rebury the heated material into a region of the asteroid that once again experienced aqueous alteration, and possibly further metamorphism.…”

Section: Evolution Of the Oxygen Isotopic Composition Of Metamorphosementioning

confidence: 99%

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Experimental simulation of oxygen isotopic exchange in olivine and implication for the formation of metamorphosed carbonaceous chondrites

Ivanova

Lorenz

Franchi

et al. 2013

Meteorit & Planetary Scien

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Abstract-We have conducted hydration-dehydration experiments on terrestrial olivine to investigate the behavior of oxygen isotopic fractionation to test the hypothesis that multiple cycles of aqueous and thermal processing on a parent asteroid comprise a genetic relationship between CM2s and metamorphosed carbonaceous chondrites (MCCs). Two experiments were undertaken. In the first experiment, serpentine was obtained by hydrating terrestrial olivine (Fo 90.9 ) in the laboratory. During this experiment, olivine was reacted with isotopically heavy water (d 18 O 21.5&) at T = 300°C, P H 2 O = 300 bar, for 100 days. The oxygen isotopic composition of the experimental serpentine was enriched in

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Section: Discussionmentioning

confidence: 99%

Section: Evolution Of the Oxygen Isotopic Composition Of Metamorphosementioning

confidence: 99%

Experimental simulation of oxygen isotopic exchange in olivine and implication for the formation of metamorphosed carbonaceous chondrites

Ivanova

Lorenz

Franchi

et al. 2013

Meteorit & Planetary Scien

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“…5. X‐ray microtomography also provides a 3‐D image of the sample, but the instrumentation is very expensive and requires qualified operators [e.g., Friedrich et al , 2008; McCausland et al , 2010; Wittmann et al , 2011] to produce good results.…”

Section: Introductionmentioning

confidence: 99%

A new method for the measurement of meteorite bulk volume via ideal gas pycnometry

Li¹,

Wang²,

Li³

et al. 2012

J. Geophys. Res.

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[1] To date, of the many techniques used to measure the bulk volume of meteorites, only three methods (Archimedean bead method, 3-D laser imaging and X-ray microtomography) can be considered as nondestructive or noncontaminating. The bead method can show large, random errors for sample sizes of smaller than 5 cm 3 . In contrast, 3-D laser imaging is a high-accuracy method even when measuring the bulk volumes of small meteorites. This method is both costly and time consuming, however, and meteorites of a certain shape may lead to some uncertainties in the analysis. The method of X-ray microtomography suffers from the same problems as 3-D laser imaging. This study outlines a new method of high-accuracy, nondestructive and noncontaminating measurement of the bulk volume of meteorite samples. In order to measure the bulk volume of a meteorite, one must measure the total volume of the balloon vacuum packaged meteorite and the volume of balloon that had been used to enclose the meteorite using ideal gas pycnometry. The difference between the two determined volumes is the bulk volume of the meteorite. Through the measurement of zero porosity metal spheres and tempered glass fragments, our results indicate that for a sample which has a volume of between 0.5 and 2 cm 3 , the relative error of the measurement is less than AE0.6%. Furthermore, this error will be even smaller (less than AE0.1%) if the determined sample size is larger than 2 cm 3 . The precision of this method shows some volume dependence. For samples smaller than 1 cm 3 , the standard deviations are less than AE0.328%, and these values will fall to less than AE0.052% for samples larger than 2 cm 3 . The porosities of nine fragments of Jilin, GaoGuenie, Zaoyang and Zhaodong meteorites have been measured using our vacuum packaging-pycnometry method, with determined average porosities of Jilin, GaoGuenie, Zaoyang and Zhaodong of 9.0307%, 2.9277%, 17.5437% and 5.9748%, respectively. These values agree well with the porosities of fragments of which have been measured using the Archimedean bead method and 3-D laser imaging. This method also may be applied to the study of rare samples in other fields (e.g., archeology and geology).Citation: Li, S., S. Wang, X. Li, Y. Li, S. Liu, and I. M. Coulson (2012), A new method for the measurement of meteorite bulk volume via ideal gas pycnometry,

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“…However, some ordinary chondrites (OC) cannot be easily placed within any one of the H, L or LL categories. These may have petrochemical characteristics that fall between the H and L or the L and LL groups, especially in terms of redox indicators such as kamacite Co content and olivine composition and have been called L/LL or H/L (Kallemeyn et al, 1989;Rubin, 1990;Wittmann et al, 2011). Alike in concept, but different in classification, are the chondrule-bearing inclusions within the anomalous IIE iron meteorite Netschaëvo, which displayed compositional trends that extrapolate well beyond those known for the H chondrite group (Bild and Wasson, 1977), to what may be called an "HH" chondrite (high amounts of Fe, and high amounts of reduced Fe).…”

Section: Introductionmentioning

confidence: 99%

Compositions of three low-FeO ordinary chondrites: Indications of a common origin with the H chondrites

Troiano

Rumble

Rivers

et al. 2011

Geochimica et Cosmochimica Acta

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Burnwell, EET 96031, and LAP 04575 are ordinary chondrites (OC) that possess lower than typical olivine Fa content than has been established for the H chondrites (<17 mol%). Mean low-Ca pyroxene Fs contents are typically lower than mean Fa content, with generally 616 mol% Fs. We have investigated these three low-FeO chondrites by measuring their trace element abundances, oxygen isotopic compositions, and examining their three-dimensional (3D) petrography with synchrotron X-ray microtomography. We compare our results with those established for more common OC. The low FeO chondrites studied here have bulk trace element abundances that are identical to the H chondrites. From bulk oxygen isotopic analysis, we show that Burnwell, EET 96010, and LAP 04757 sampled oxygen reservoirs identical to the H chondrites. Burnwell, EET 96031, and LAP 04575 possess common 3D opaque mineral structures that could be distinct from the H chondrites, as evidenced by X-ray microtomographic analysis, but our comparison suite of H chondrites is small and unrepresentative. Overall, our data suggest a common origin for the low-FeO chondrites Burnwell, EET 96010, and LAP 04757 and the H chondrites. These three samples are simply extreme members of a redox process where a limiting nebular oxidizing agent, probably ice, reacted with material containing slightly higher amounts of metal than typically seen in the H chondrites.

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H/L chondrite LaPaz Icefield 031047 – A feather of Icarus?

Cited by 32 publications

References 71 publications

Experimental simulation of oxygen isotopic exchange in olivine and implication for the formation of metamorphosed carbonaceous chondrites

Experimental simulation of oxygen isotopic exchange in olivine and implication for the formation of metamorphosed carbonaceous chondrites

A new method for the measurement of meteorite bulk volume via ideal gas pycnometry

Compositions of three low-FeO ordinary chondrites: Indications of a common origin with the H chondrites

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