Variability of Chelyabinsk meteoroid stones studied by Mössbauer spectroscopy and X-ray diffraction

Оштрах, М. И.; Maksimova, A. A.; Чукин, А. В.; Petrova, E. V.; Jenniskens, Peter; Кузманн, Э.; Grokhovsky, V. I.; Homonnay, Z.; Semionkin, V. A.

doi:10.1016/j.saa.2019.03.036

Cited by 26 publications

(53 citation statements)

References 56 publications

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“…The relative areas of components in the M€ ossbauer spectra of ordinary chondrites can be used for meteorites classification as has already been shown by Paliwal et al (2000), Verma et al (2002Verma et al ( , 2003, Verma and Tripathi (2004), Oshtrakh et al (2008), Galazka-Friedman et al 2017, and Elewa and Cadogan (2017). We used this approach also and found that the plot of the total relative area of components related to Fe-Ni-Co alloy plus those assigned to Fe 3+ compounds versus the total relative area of components associated with the M1 and M2 sites in olivine can be considered as the most useful for classification (Oshtrakh et al 2008(Oshtrakh et al , 2019Maksimova et al 2017Maksimova et al , 2018bMaksimova and Oshtrakh 2019). This way is possible for nonweathered meteorites and in situations with small weathering grade when iron in silicate crystals is not oxidized.…”

Section: M1mentioning

confidence: 67%

“…The obtained M€ ossbauer parameters for spectral components are given in Table 3. The assigning of spectral hyperfine parameters to the indicated compounds (phases) was done in the same way as it was recently done in the studies of other ordinary chondrites (see Maksimova et al 2018b;Oshtrakh et al 2019; and references therein). It should be noted that we were unable to calculate correctly the…”

Section: The Interiormentioning

confidence: 99%

“…Calculated values of T eq are 553 and 1213 K for olivine and orthopyroxene, respectively. Using relative areas of corresponding spectral components in the M€ ossbauer spectrum of Ozerki L6, we can calculate K D and T eq for olivine and orthopyroxene also using the values of fayalite (Fa) and ferrosilite (Fs) for this meteorite by means of approach described in detail by Oshtrakh et al (2008Oshtrakh et al ( , 2019. The values of Fa and Fs are 0.26 and 0.21 (Meteoritical Bulletin 2018).…”

Section: M1mentioning

confidence: 99%

“…Vertical and horizontal error bars are roughly estimated averaged relative errors. Adopted from Oshtrakh et al (2019). (Color figure can be viewed at wileyonline library.com.…”

Section: M1mentioning

confidence: 99%

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Characterization of the matrix and fusion crust of the recent meteorite fall Ozerki L6

Maksimova

Petrova

Чукин

et al. 2019

Meteorit & Planetary Scien

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We studied the interior and the fusion crust of the recently recovered Ozerki L6 meteorite using optical microscopy, scanning electron microscopy (SEM) with energy dispersive spectroscopy, X-ray diffraction (XRD), magnetization measurements, and M€ ossbauer spectroscopy. The phase composition of the interior and of the fusion crust was determined by means of SEM, XRD, and M€ ossbauer spectroscopy. The unit cell parameters for silicate crystals were evaluated from the X-ray diffractograms and were found the same for the interior and the fusion crust. Magnetization measurements revealed a decrease of the saturation magnetic moment in the fusion crust due to a decrease of Fe-Ni-Co alloy content. Both XRD and M€ ossbauer spectroscopy show the presence of magnesioferrite in the fusion crust. The temperatures of cation equilibrium distribution between the M1 and M2 sites in silicates calculated using the data obtained from XRD and M€ ossbauer spectroscopy appeared to be in a good consistency: 553 and 479 K for olivine and 1213 and 1202 K for orthopyroxene.

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Section: M1mentioning

confidence: 67%

Section: The Interiormentioning

confidence: 99%

Section: M1mentioning

confidence: 99%

“…Vertical and horizontal error bars are roughly estimated averaged relative errors. Adopted from Oshtrakh et al (2019). (Color figure can be viewed at wileyonline library.com.…”

Section: M1mentioning

confidence: 99%

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Characterization of the matrix and fusion crust of the recent meteorite fall Ozerki L6

Maksimova

Petrova

Чукин

et al. 2019

Meteorit & Planetary Scien

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“…X-ray diffraction (XRD) and Raman spectroscopy analyses indicate that the overall mineralogy of the three Chelyabinsk lithologies is similar (Moroz et al 2014;Reddy et al 2014;Oshtrakh et al 2019). Newly crystallized long-prismatic olivine crystals, which are more magnesium-rich as described in Kaeter et al (2018), are an exception to this.…”

Section: Introductionmentioning

confidence: 99%

Experimental constraints on the ordinary chondrite shock darkening caused by asteroid collisions

Kohout¹,

Petrova²,

Yakovlev³

et al. 2024

Preprint

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IntroductionShock-induced changes in planetary materials related to impacts or planetary collisions are known to be capable of altering their optical properties. One such example is observed in ordinary chondrite meteorites. The highly shocked silicate-rich ordinary chondrite material is optically darkened and its typical S-complex-like asteroid spectrum is altered toward a darker, featureless spectrum resembling the C/X complex asteroids. Thus, one can hypothesize that a significant portion of the ordinary chondrite material may be hidden within the observed C/X asteroid population.The exact pressure-temperature conditions of the shock-induced darkening are, however, not well constrained and due to this gap in knowledge, it is not possible to correctly assess the significance of the shock darkening within the asteroid population. In order to address this shortcoming, we experimentally investigate the gradual changes in the chondrite material optical properties together with the associated mineral and textural features as a function of the shock pressure. For this purpose, we use a Chelyabinsk meteorite (LL5 chondrite), which is subjected to a spherical shock experiment. The spherical shock experiment geometry allows for a gradual increase in the shock pressure within a single spherically shaped sample from 15 GPa at its rim toward hundreds of gigapascals in the center.ResultsFour distinct zones were observed with an increasing shock load (Fig. 1). We number the zones in the direction of increasing shock from the outside toward the center as zones I&#8211;IV The optical changes in zone I are minimal up to ~50 GPa. In the region of ~50&#8211;60 GPa corresponding to zone II, shock darkening occurs due to the troilite melt infusion into silicates. This process abruptly ceases at pressures of ~60 GPa in zone III due to an onset of silicate melting and immiscibility of troilite and silicate melts. Silicate melt coats residual silicate grains and prevents troilite from further penetration into cracks. At pressures higher than ~150 GPa (zone IV), complete recrystallization occurs and is associated with a second-stage shock darkening due to fine troilite-metal eutectic grains.<img src="https://contentmanager.copernicus.org/fileStorageProxy.php?f=gnp.369960f7c0fe58218382951/sdaolpUECMynit/0202CSPE&app=m&a=0&c=65ce9691abaaf54f5e7768045027f7ea&ct=x&pn=gnp.elif" alt="" width="777" height="639">The order of the spectral curves in the UV-VIS-NIR (ultraviolet &#8211; visible &#8211; near-infrared) region follows the visual brightness in which zone I is the brightest, followed by zones III and II, and zone IV is the darkest one (Fig. 2). The MIR reflectance (Fig. 3) follows the same albedo order as UV-VIS-NIR up to the primary Christiansen feature at 8.7 &#181;m. At higher wavelengths in the Si-O reststrahlen bands region, the reflectance order changes with zones II and III, which are brighter than zones I and IV. The comparison of the powdered sample spectra to the one obtained from the rough saw-cut surface reveals the following trends. The overall reflectance of the powdered sample is an order of magnitude lower compared to the rough surface one. The reststrahlen bands in both samples show similar positions at approximately 9.1, 9.5&#8211;9.6, 10.3, 10.8, 11.3, and 11.8&#8211;12 &#181;m. They are dominated by olivine with possible presence of orthopyroxene. The amplitudes of the reststrahlen bands are higher in the rough surface sample. The transparency feature at 12.7 &#181;m is only observed in the powdered sample. The primary Christiansen feature at 8.7 &#181;m is more pronounced in the powdered sample, while the secondary one at 15.6 &#181;m is of a low amplitude in both samples.<img src="https://contentmanager.copernicus.org/fileStorageProxy.php?f=gnp.ad38963ac0fe50178382951/sdaolpUECMynit/0202CSPE&app=m&a=0&c=1cbf38a911d6e0bef4cff605b284362f&ct=x&pn=gnp.elif" alt=""><img src="https://contentmanager.copernicus.org/fileStorageProxy.php?f=gnp.4ff3f9a9c0fe59658382951/sdaolpUECMynit/0202CSPE&app=m&a=0&c=9e7ff0973b952ce0eed7a0fbfc5b24cc&ct=x&pn=gnp.elif" alt="">ConclusionsThe important finding is the presence of the two distinct shock darkening mechanisms in ordinary chondrite material with characteristic material fabric and distinct pressure regions. These two regions are separated by a pressure interval where no darkening occurs. Thus, the volume of the darkened material produced during asteroid collisions may be somewhat lower than assumed from a continuous darkening process. While the darkening mainly affects the UV-VIS-NIR region and 1 and 2-&#181;m silicate absorption bands, it does not significantly affect the silicate spectral features in the MIR region. These are more affected by material roughness. MIR observations have the potential to identify darkened ordinary chondrite material with an otherwise featureless UV-VIS-NIR spectrum.

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Mineral Inclusions in Irghizites and Microirghizites (Zhamanshin Astroblem, Kazakhstan)

Sergienko

Janson

Esau

et al. 2023

Springer Proceedings in Earth and Environmental Sciences

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Variability of Chelyabinsk meteoroid stones studied by Mössbauer spectroscopy and X-ray diffraction

Cited by 26 publications

References 56 publications

Characterization of the matrix and fusion crust of the recent meteorite fall Ozerki L6

Characterization of the matrix and fusion crust of the recent meteorite fall Ozerki L6

Experimental constraints on the ordinary chondrite shock darkening caused by asteroid collisions

Mineral Inclusions in Irghizites and Microirghizites (Zhamanshin Astroblem, Kazakhstan)

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