High‐pressure polymorphs in Yamato‐790729 L6 chondrite and their significance for collisional conditions

Kato, Yukako; Sekine, Toshimori; Kayama, Mitsu; Miyahara, Masaaki; Yamaguchi, A.

doi:10.1111/maps.12957

Cited by 8 publications

(14 citation statements)

References 58 publications

(156 reference statements)

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“…Ringwoodite, majorite, akimotoite, and Na‐lingunite are present in the shock vein, indicating impact events (Kato et al. ; Tomioka and Miyahara ).…”

Section: Experimental Methods and Materialsmentioning

confidence: 99%

“…Yamato‐790729 contains large amounts of olivine, low‐Ca pyroxene, plagioclase, metallic Fe‐Ni, and iron‐sulfide with minor phosphate and chromite (Kato et al. ), and shows a shock vein and remnants of chondritic textures. Ringwoodite, majorite, akimotoite, and Na‐lingunite are present in the shock vein, indicating impact events (Kato et al.…”

Section: Experimental Methods and Materialsmentioning

confidence: 99%

“…; Kato et al. ). Lingunite with a hollandite structure has been found in several L chondrites, H chondrites, and Martian meteorites (El Goresy et al.…”

Section: Introductionmentioning

confidence: 96%

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Cathodoluminescence of high‐pressure feldspar minerals as a shock barometer

Kayama

Sekine

Tomioka

et al. 2018

Meteorit & Planetary Scien

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Cathodoluminescence (CL) analyses were carried out on maskelynite and lingunite in L6 chondrites of Tenham and Yamato‐790729. Under CL microscopy, bright blue emission was observed in Na‐lingunite in the shock veins. Dull blue‐emitting maskelynite is adjacent to the shock veins, and aqua blue luminescent plagioclase lies farther away. CL spectroscopy of the Na‐lingunite showed emission bands centered at ~330, 360–380, and ~590 nm. CL spectra of maskelynite consisted of emission bands at ~330 and ~380 nm. Only an emission band at 420 nm was recognized in crystalline plagioclase. Deconvolution of CL spectra from maskelynite successfully separated the UV–blue emission bands into Gaussian components at 3.88, 3.26, and 2.95 eV. For comparison, we prepared K‐lingunite and experimentally shock‐recovered feldspars at the known shock pressures of 11.1–41.2 GPa to measure CL spectra. Synthetic K‐lingunite has similar UV–blue and characteristic yellow bands at ~550, ~660, ~720, ~750, and ~770 nm. The UV–blue emissions of shock‐recovered feldspars and the diaplectic feldspar glasses show a good correlation between intensity and shock pressure after deconvolution. They may be assigned to pressure‐induced defects in Si and Al octahedra and tetrahedra. The components at 3.88 and 3.26 eV were detectable in the lingunite, both of which may be caused by the defects in Si and Al octahedra, the same as maskelynite. CL of maskelynite and lingunite may be applicable to estimate shock pressure for feldspar‐bearing meteorites, impactites, and samples returned by spacecraft mission, although we need to develop more as a reliable shock barometer.

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“…Ringwoodite, majorite, akimotoite, and Na‐lingunite are present in the shock vein, indicating impact events (Kato et al. ; Tomioka and Miyahara ).…”

Section: Experimental Methods and Materialsmentioning

confidence: 99%

Section: Experimental Methods and Materialsmentioning

confidence: 99%

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Cathodoluminescence of high‐pressure feldspar minerals as a shock barometer

Kayama

Sekine

Tomioka

et al. 2018

Meteorit & Planetary Scien

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“…DOI: https://doi.org/10.2138/am-2021-7632. http://www.minsocam.org/ close to the Mg-Fe join (Coleman 1977;Walton 2013;Kato et al 2017) and in solid solution with other garnet components, including pyrope (Mg Al Si O 12 ; Chen et al 1996), almandine (Fe 3 Al 2 Si 3 O ; Ma and Tschauner 2016), and calcic garnet (Xie and Sharp 2007).…”

Section: Silica Glass (Sio )mentioning

confidence: 99%

An evolutionary system of mineralogy, Part IV: Planetesimal differentiation and impact mineralization (4566 to 4560 Ma)

Morrison

Hazen

2021

American Mineralogist

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The fourth installment of the evolutionary system of mineralogy considers two stages of planetesimal mineralogy that occurred early in the history of the solar nebula, commencing by 4.566 Ga and lasting for at least 5 million years: (1) primary igneous minerals derived from planetesimal melting and differentiation into core, mantle, and basaltic components; and (2) impact mineralization resulting in shock-induced deformation, brecciation, melting, and highpressure phase transformations. We tabulate 90 igneous differentiated asteroidal minerals, including the earliest known occurrences of minerals with Ba, Cl, Cu, F, and V as essential elements, as well as the first appearances of numerous phosphates, quartz, zircon, and amphibole group minerals. We also record 40 minerals formed through high-pressure impact alteration, commencing with the period of asteroid accretion and differentiation. These stages of mineral evolution thus mark the first time that high pressures, both static and dynamic, played a significant role in mineral paragenesis.

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“…2016; Kato et al. 2017). The kinetics controlling the phase transitions and growth rates of the high‐pressure polymorphs should also be considered, because both the pressure and temperature change rapidly during the shock metamorphism.…”

Section: Introductionmentioning

confidence: 99%

Back‐transformation mechanisms of ringwoodite and majorite in an ordinary chondrite

Fukimoto

Miyahara

Sakai

et al. 2020

Meteorit & Planetary Scien

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We investigated the back-transformation mechanisms of ringwoodite and majorite occurring in a shock-melt vein (SMV) of the Yamato 75267 H6 ordinary chondrite during atmospheric entry heating. Ringwoodite and majorite in the shock melt near the fusion crust have back-transformed into olivine and enstatite, respectively. Ringwoodite (Fa~1 8) occurs in the SMV as a fine-grained polycrystalline assemblage. Approaching the fusion crust, fine-grained polycrystalline olivine becomes dominant instead of ringwoodite. The back-transformation from ringwoodite to olivine proceeds by incoherent nucleation and by an interface-controlled growth mechanism: nucleation occurs on the grain boundaries of ringwoodite, and subsequently olivine grains grow. Majorite (Fs 16-17 En 82-83 Wo 1) occurs in the SMV as a fine-grained polycrystalline assemblage. Approaching the fusion crust, the majorite grains become vitrified. Approaching the fusion crust even more, clino/ orthoenstatite grains occur in the vitrified majorite. The back-transformation from majorite to enstatite is initiated by the vitrification, and growth continues by the subsequent nucleation in the vitrified majorite.

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High‐pressure polymorphs in Yamato‐790729 L6 chondrite and their significance for collisional conditions

Cited by 8 publications

References 58 publications

Cathodoluminescence of high‐pressure feldspar minerals as a shock barometer

Cathodoluminescence of high‐pressure feldspar minerals as a shock barometer

An evolutionary system of mineralogy, Part IV: Planetesimal differentiation and impact mineralization (4566 to 4560 Ma)

Back‐transformation mechanisms of ringwoodite and majorite in an ordinary chondrite

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