International Journal of Spectroscopy
Volume 2016 (2016), Article ID 1751730, 8 pages
http://dx.doi.org/10.1155/2016/1751730

Research Article

Cathodoluminescence and Raman Spectromicroscopy of Forsterite in Tagish Lake Meteorite: Implications for Astromineralogy

Arnold Gucsik,1,2 Ildikó Gyollai,2,3 Hirotsugu Nishido,⁴ Kiyotaka Ninagawa,⁵ Matthew M. R. Izawa,⁶ Cornelia Jäger,⁷ Ulrich Ott,⁸ Irakli Simonia,⁹ Szaniszló Bérczi,³ and Masahiro Kayama¹⁰

¹Department of Geology, University of Johannesburg, Auckland Park, Johannesburg 2600, South Africa
²Konkoly Thege Miklós Astronomical Institute, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, Konkoly Thege Miklós út 15-17, Budapest 1121, Hungary
³Cosmic Material Space Research Group, Institute of Physics, Department of Material Physics, Faculty of Science, Eötvös Loránd University, Pázmány Péter Sétány 1/a, Budapest 1117, Hungary
⁴Department of Biosphere-Geosphere System Science, Okayama University of Science, 1-1 Ridai-cho, Okayama 700-0005, Japan
⁵Department of Applied Physics, Okayama University of Science, 1-1 Ridai-cho, Kita-ku, Okayama 700-0005, Japan
⁶University of Winnipeg, 515 Portage Avenue, Winnipeg, MB, Canada R3B 2E9
⁷Laboratory Astrophysics Group, The Max Planck Institute for Astronomy, Institute of Solid State Physics, The Friedrich Schiller University Jena, Helmholtzweg 3, 07743 Jena, Germany
⁸Savaria University Center, University of West Hungary, Károlyi Gáspár tér 4, Szombathely 9700, Hungary
⁹School of Graduate Studies, Ilia State University, Kakutsa Cholokashvili Avenue 3/5, 0162 Tbilisi, Georgia
¹⁰Department of Earth and Planetary Sciences, Faculty of Science, Kobe University, 1-1 Rokkodai-cho, Nada-ku, Kobe 657-8501, Japan

Received 31 October 2015; Accepted 28 January 2016

Academic Editor: Jin Zhang

Copyright © 2016 Arnold Gucsik et al. This is an open access article distributed under the Creative Commons Attribution License, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

Abstract.

The Tagish Lake meteorite is CI/CM2 chondrite, which fell by a fireball event in January 2000. This study emphasizes the cathodoluminescence (CL) and Raman spectroscopical properties of the Tagish Lake meteorite in order to classify the meteoritic forsterite and its relation to the crystallization processes in a parent body. The CL-zoning of Tagish Lake meteorite records the thermal history of chondrules and terrestrial weathering. Only the unweathered olivine is forsterite, which is CL-active. The variation of luminescence in chondrules of Tagish Lake meteorite implies chemical inhomogeneity due to low-grade thermal metamorphism. The blue emission center in forsterite due to crystal lattice defect is proposed as being caused by rapid cooling during the primary crystallization and relatively low-temperature thermal metamorphism on the parent body of Tagish Lake meteorite. This is in a good agreement with the micro-Raman spectroscopical data. A combination of cathodoluminescence and micro-Raman spectroscopies shows some potentials in study of the asteroidal processes of parent bodies in solar system.

1. Introduction

The Tagish Lake meteorite fell on 18th January, 2000, at 16:43 UTC [1]. Tagish Lake fireball event ended with airburst explosions near Carcross, Yukon Territory, Canada, and debris crossed the Yukon-British Columbia boundary, with many fragments finally landing on Taku Arm of Tagish Lake, British Columbia, Canada (59°42′ N, 134°12′ W). The original preatmospheric mass of the Tagish Lake meteorite was estimated at 200,000 [1], 56,000 [2], and 60,000–90,000 kg [3]. Tagish Lake was initially classified as the first CI2 chondrite [4] but has subsequently been regarded as an ungrouped C2 chondrite with affinities to both CM and CI chondrites. Out of the 10 kg recovered in total, about 870 g was collected within about a week after the fall, on 25th-26th January, 2000, from the frozen lake surface [3]. The Tagish Lake meteorite is a brecciated, matrix-dominated material with multiple lithologies [5–9]. Tagish Lake contains sparse olivine-dominated chondrules generally of less than 1 mm diameter, altered CAIs of up to 2 mm diameter, magnetite, individual grains of olivine, Ca-Fe-Mn carbonates (calcite and siderite-magnesite with rarer dolomite), and Fe-Ni sulfides including pyrrhotite (e.g., [1, 5, 6]). The chondrule mesostasis glass material is partially replaced by phyllosilicates indicative of aqueous alteration [10]. Most CAIs are completely altered to phyllosilicates (mainly Mg-rich serpentine, saponite) and carbonates (dolomite, calcite), though some retain spinel-dominant primary material [6]. Tagish Lake matrix is mineralogically similar to that of other aqueously altered carbonaceous chondrites (CM, CI, and CR chondrites) and is composed of Mg-phyllosilicates, fine-grained Fe-Ni sulfides, magnetite, and Fe-Mg carbonates (e.g., [5, 7, 10]). Tagish Lake meteorite is an unshocked (S1) type [1, 6], like most carbonaceous chondrites [1, 11]. Herd et al. [10] identified carboxylic acids, amino acids, and aliphatic and aromatic hydrocarbons in organic fractions. Brown et al. [1] interpreted Tagish Lake meteorite low-temperature (perhaps approaching ~0°C) aqueous alteration to have taken place on a water-bearing parent asteroid, similar to the case of other aqueously altered carbonaceous chondrites, while Hiroi et al. [12] proposed the Tagish Lake meteorite as the first sample of a D-type asteroid. Mittlefehldt [13] concludes that the elemental composition of Tagish Lake is generally closer to CM chondrites than to CI but also found that some of the most volatile elements were higher than in CM. The carbon content, according to Grady et al. [4], is 5.81 wt%, which is higher than typical concentrations for CM or CI carbonaceous chondrites. Carbon in Tagish Lake occurs in carbonate minerals [5], various organic compounds, and nanodiamonds (e.g., [4, 10]). Brown et al. [1] measured oxygen isotopic compositions close to CI chondrites. Grady et al. [4] observed higher concentrations of presolar nanodiamonds in Tagish Lake than in any other meteorite. Mittlefehldt [13] concluded, based primarily on the apparent higher concentrations of presolar nanodiamonds (stardust grains), that the Tagish Lake parent body accreted at larger heliocentric distances than most other carbonaceous chondrites. The organic material in Tagish Lake meteorite was studied by numerous groups including Pizzarello et al. [14] and Nakamura-Messenger et al. [15], who proposed that the organic globules in Tagish Lake material originated from protoplanetary disk.

2. Samples and Experimental Procedure

Our Tagish Lake sample consisted of two thin sections, which are embedded in epoxy resin on a glassy slide. Samples for this study are from Spring 2000 (nonpristine) collection and originate from collection site MG-02 [1, 13]. The sections were prepared by hand using isopropyl alcohol as the only solvent and were set in Struers EpoFix epoxy. The same sections were studied by Izawa et al. [6]; see their Figures C-D, 4, and 8. One area has been selected from each of the slides, each containing forsterite-rich chondrules in fine-grained matrix.

Chondrule olivine in Tagish Lake is dominantly forsteritic in composition, with Ca, Cr, and Mn as the most common minor elements (e.g., [6, 16]). Chondrule olivine in the thin section studied here (the same as that used by Izawa et al. [6]) has an average Cr₂O₃ content of 0.30 wt% and MnO content of 0.03 wt% [6]. The grains are chemically homogeneous in SEM X-ray map [6] and are compositionally close to end-member forsterite (average chondrule olivine composition Fo98.9 for this section, Izawa et al. [6], their Table ). CL color imaging was obtained using a luminoscope (ELM-3R) with a cooled charge-coupled device (CCD) camera, which was operated with electron beams generated by excitation voltage at 10 kV and beam current of 0.5 mA. This system also contains a cold cathode discharge tube and a vacuum chamber. The diameter of electron beam spot at a few mm size on the sample surface was controlled by a magnet. The Nikon imaging system (DS-5Mc) was used to convert CL images to digital data.

JSM-5410LV Scanning Electron Microscope (SEM) consisting of MiniCL detector with a multialkali photomultiplier tube was used to obtain CL scanning images at high magnification. A grating monochromator of the SEM-CL facility was used with the following operating conditions: 1200 grooves/mm, a focal length of 0.3 m, F of 4.2, limit of resolution of 0.5 nm, and slit width of 4 mm at the inlet and outlet. CL spectral data were recorded by a photon counting method using a photomultiplier tube (Hamamatsu, R2228) and converted to digital data.

Further details of the CL equipment and analytical procedure can be seen in Kayama et al. [17]. The OriginPro 8J SR2 software containing a peak fitting option (peak analyzer) was used for the correction and deconvolution of each emission center.

Micro-Raman analyses were carried out using the LabRam Confocal Spectrometer (632 nm excitation) of the Laboratory Astrophysics Group of the Max Planck Institute for Astronomy (Jena, Germany). Single spectrum was acquired with an integration time of 30 sec at 3 accumulations, and spectral range of 100–4400 cm⁻¹ and 20x and 50x objectives were used for the collection of Raman spectra. Here, we present Raman results selecting the most representative Raman spectrum.

3. Results

3.1. Optical Microscopy

The studied area contains a strongly aqueous-altered porphyritic chondrule (~800 μm diameter), which has a fine-grained accretionary rim. The formerly glassy chondrule mesostasis has been replaced by phyllosilicates, which has been discernible in the optical images (Figures 1(a) and 1(c)). The individual olivine phenocrysts range is 10–50 μm in the longest dimension, but a large 300 μm amoeboid olivine aggregate occurs in the chondrule. The second chondrule is less altered, which is an intermediate between granular (TLa left side of chondrule) and barred texture (TLa right-side of chondrule). The mesostasis has been altered to a phyllosilicate-dominant material. In both chondrules the olivine crystals show zoned structure, which may correspond to structural inhomogeneity or lattice strain. The area TLb is composed of mineral-fragment rich groundmass, which contains a strongly altered forsterite chondrule (Figures 2(a) and 2(b)).

(a)

(b)

(c)

(d)

(e)

(f)

Figure 1: Optical microscope ((a) reflected light and (c) cross-polarized modes), scanning electron microscope ((e) backscattered electron microscope and (b) cathodoluminescence), and cathodoluminescence color ((d) and (f) at high magnification of the selected grain) images of TLa area showing a forsteritic barred chondrule. Scale: width of the chondrule is around 1 mm.

(a)

(b)

(c)

(d)

(e)

(f)

Figure 2: Optical microscope ((a) reflected light and (c) cross-polarized modes), scanning electron microscope ((e) backscattered electron microscope and (b) cathodoluminescence), and cathodoluminescence color ((d) and (f) at high magnification of the selected grain) images of TLb area showing a highly altered forsteritic chondrule. Scale: width of the chondrule is around 1 mm.

3.2. Cathodoluminescence Spectral Features and Imaging Properties

In the area TLa, both chondrules have dull red color, but mesostasis of the barred part of the right-side chondrule has grayish green color (Figures 1(d) and 1(f)). It is important to note that these parts could also be trapped bits of diamond polishing compounds. The mesostasis has a number of red luminescent grains. On the backscattered electron (BSE) image the granular-barred chondrule has a lighter alteration rim including metal (Fe-Ni) and phyllosilicates (Figure 1(e)). The olivine grains in the chondrules show zoned higher luminescence (MiniCL image) according to the distribution of activator elements (Figure 1(b)). The alteration rims for both chondrules are composed of nonluminescent minerals (dominantly phyllosilicates). The dull luminescent grains have higher luminescent and nonluminescent rims. The change of luminescence intensity in adjacent grains is due to inhomogeneous distribution of CL activator elements. Inside the olivine, blue and light yellow inclusions occur.

CL area b (TLb) is composed primarily of strongly altered chondrule fragments (less than 300 μm) and isolated olivine fragments. The matrix is composed of phyllosilicates, carbonates, sulfides, magnetite, and organic material. Moreover, Izawa et al. [6] observed that the carbonate grains usually have a “streak” in the scanning electron microscope-cathodoluminescence (SEM-CL) images due to the long lifetime (phosphorescence rather than luminescence) (Figure 2(b)). Mineral fragments in the matrix have red luminescence color, whereas the nonaltered inner part of the chondrule has a blue luminescence color and red rim (Figures 2(d) and 2(f)). In the BSE image (Figure 2(e)), the inner part of the chondrule is dark and has a “spongy” texture. The alteration rim has lighter BSE contrast and contains metallic grains. The dark BSE indicates a predominance of low-Z elements like Mg, Si, and O, consistent with forsterite [6]. The MiniCL image shows homogenous strong luminescence intensity for the whole inner part of the chondrule (Figure 2(b)).

The CL spectra show broad luminescence centers at 400–460, 600–650, and 700 nm. TLb1 has less intensity in the 600–700 nm region than TLb2, while, in contrast to both TLb spectra, the TLa spectra have no luminescence center at 400 nm. Instead, they have broad shoulders at 600–650, 700–720, and 750 nm (Figure 3(a)). After the peak fitting procedure (see Samples and Experimental Procedure), a peak at 400 nm (TLb1-2 only) and shoulders at 600–650 and 700–800 nm can be identified (Figure 3(b)). On the energy scale (Figure 3(c)), broad shoulders occur at 0–2 eV, and a broad peak appears at 2.5–3.5 eV.

(a)

(b)

(c)

Figure 3: (a) Cathodoluminescence spectra of TLa and TLb areas in forsterite showing three major regions centered at 400–460, 600–650, and 700–800 nm. (b) CL spectra of forsterite grains followed by a peak fitting procedure. (c) CL intensity versus energy plot of the Tagish Lake forsterite. The 1.74 eV peak corresponds to Cr³⁺, and the 1.94 eV peak is assigned to Mn²⁺.

3.3. Raman Spectra

Raman spectral features (Figure 4) of the selected forsterite grain (TLb) contain several very weak (vw) as well as weak (w) positions at 222, 322, 390, 432, 541, 582, 605, 668, and 735 cm⁻¹ and three medium strong peaks (m) at 637, 916, and 963 cm⁻¹. The spectrum is dominated by a very strong (vs) doublet peak at 823 and 855 cm⁻¹ with a shoulder peak centered at 876 cm⁻¹ (Figure 4).

Figure 4: Raman spectrum of Tagish Lake forsterite showing a dominant doublet peak at 823 and 855 cm⁻¹, which are assigned to symmetric and asymmetric stretching vibrational modes of the isolated SiO₄ tetrahedra [18].

4. Discussion

4.1. Cathodoluminescence Microscopy and Spectroscopy of Forsterite from Tagish Lake Meteorite

Cathodoluminescence properties of forsterite in meteorites were previously studied in the Kaba CV3 chondrite by Gucsik et al. [19, 20]. Similar to those, forsterite crystals in Tagish Lake show red-dull red luminescence. The lack of luminescence in fractures as well as decreased luminescence intensity in forsterite adjacent to fractures likely reflects increased concentration of Fe²⁺ in such regions, because of its quenching effect. The two broad centers at 630 nm in the red region and at 700–800 nm in the IR region can be caused by Mn²⁺ ion as activator, and by the Cr³⁺ activator, which may cause structural defects. The broad luminescence centered at 400 nm in case of the TLb area corresponds to a structural defect. Recently, Gucsik et al. [21] described a tendency that an increasing supercooling rate during the crystallization process of experimentally grown forsterite chondrules leads to a gradual cathodoluminescence color change ranging from red to greenish blue. They found that the red CL color corresponds to growth rates of 20–100 micrometers/sec, whereas blue or greenish blue colors correspond to rates of ~1000 micrometers/sec. Nishido et al. [22] pointed out that CL-zoning records the thermal history of chondrules. During terrestrial weathering, Fe²⁺ cations are attached in the fractures resulting in quenching of luminescence. The unweathered meteoritic olivine (forsterite), on the other hand, is CL-active. The variation of luminescence intensity in chondrules of area A indicates chemical inhomogeneity due to low degree of thermal metamorphism. At the duller red luminescence centers of area TLa the olivine has a fayalitic component, whereas the light luminescent patches are purely forsterite. The fractures in chondrules are nonluminescent, which is caused by either enrichment of divalent Fe due to parent body aqueous alteration, terrestrial weathering, or shock-driven diffusion of Fe²⁺ into the olivine lattice. The blue luminescence center in area TLb is ascribed to intrinsic defects centers associated with either Al³⁺ substitution for Si⁴⁺ in tetrahedral sites or lattice deformation due to substitution of Ca²⁺ and Ti⁴⁺ ions in octahedral sites [22, 23]. The broad emission at 650 nm (TLa, TLb) is assigned to Mn²⁺ impurity centers in M2 positions of forsterite [22, 23]. Finally, the broad emission bands at 720 nm and higher wavenumber is attributed to Cr³⁺ substitutions in the M1 and M2 sites, as well as interstitial positions of forsterite [22, 23].

The energetic CL spectra were deconvolved using the Mott-Seitz model [22]. This model obtains activation energies of temperature-quenching luminescence from a proposed nonradiative transition increasing with increasing sample temperature [24, 25]. The activation energies for red emissions are centered at 1.8 and 1.74 eV for TLa-b, where the 1.74 eV peak corresponds to Cr³⁺ and the 1.94 eV peak corresponds to Mn²⁺. The activation energy in blue region (TLb) appears as broad band at 3.15 eV, which corresponds to a crystallographic defect center, probably microdefect centers due to the rapid cooling history of forsterite [21] (Figure 3(b)).

4.2. Raman Spectroscopy

According to Chopelas [26] and Kolesov and Geiger [18] Raman properties of forsterite should be divided into two major spectral regions such as librational and translational modes as well as stretching vibrations of SiO₄. In our study, two peaks centered at 222 and 322 cm⁻¹ are assigned to translation [T (SiO₄)] and liberation [R (SiO₄)] of the SiO₄. A peak at 432 cm⁻¹ is a vibrational mode and a vibration at 582 cm⁻¹ belongs to . In our Tagish Lake meteoritic forsterite, there are two stretching modes centered at 541 and 605 cm⁻¹. Peaks at 823 and 855 cm⁻¹ are related to vibrational modes and a shoulder peak at 876 and two weak bands are assigned to stretching vibration. Four Raman spectral positions of the meteoritic forsterite centered at 390, 637, 668, and 735 cm⁻¹ are still poorly understood. Compared to other meteoritic forsterite (see [19, 27] and references therein), neither shock metamorphism nor thermal effects were found in the Raman properties of our Tagish Lake meteoritic forsterite. However, the Raman characteristics of our forsterite sample contains some signatures of the rapid cooling (e.g., Raman peaks centered at 390, 637, 668, and 735 cm⁻¹) [18], which are in a good agreement with the cathodoluminescence results of this study.

4.3. Forsterite Grains of Cometary Dust

It is known that the dust of comets in the form of silicate and carbon grains, as well as the fine-grained icy particles that make the cometary halo, causes the appearance of weak continuous spectrum of comets [28]. Recently forsterite mineral has been detected in the cometary dust [29]. It means that forsterite might be the noticeable component of the cometary silicate halos.

Cometary halos might be influenced by the fluxes of solar corpuscular radiation, solar wind, and plasma clouds. Solar flares might play an important role in the processes of interaction of radiation with the cometary atmospheres. The proton flares with outflows of protons with energy of more than 12 GeV are rare phenomena. Proton flares with the energy of 10 MeV < < 100 MeV are more frequent. At the distance of 1 AU from the Sun, the proton fluxes of the solar wind can vary within 10⁸–10¹⁰ cm⁻²s⁻¹ [30]. Relativistic particles require not less than 8 min for propagation at the distance of 1 AU and the electrons of 50 KeV or ions of 100 MeV amu⁻¹ require 18 min and for ions 1 MeV amu⁻¹ they require 2.9 hours. For large and small solar flares the characteristic values of released energies can be expressed as  erg. for electrons (of 20 KeV and higher) and  erg. for protons (of 20 MeV and higher). Among the important phenomena is also the ejection of fast particles with velocity exceeding 1000 kms⁻¹. Taking into account the velocities of the main components of solar wind around 380 kms⁻¹–800 kms⁻¹, it is necessary to note that the propagation of solar wind is limited by the dimensions of the heliosphere of about 100 AU (astronomical unit). The release of a significant amount of energy during the solar flares takes place for a short period of time, in average, for tens of minutes. The fluxes of solar electrons and protons colliding with cometary halos might cause an intensive cathodoluminescence of the grains of halos. The intensity of cathodoluminescence of halos grains can be especially high after solar proton flares. When halos grains are bombarded by electrons or protons, its surface can start luminescing. The duration of cathodoluminescence of cometary grains might vary from some minutes to several hours. Too long exposure of cosmic luminophors to high-energy electrons (protons) can cause the luminophor destruction resulting in a full or partial loss of their luminescence properties. The practical detection of cathodoluminescence of cometary grains will depend on (1) quantum yield () of cathodoluminescence of the matter of the given grains and (2) albedo () of the given halos. Numerically, for the case of cathodoluminescence and will be favorable for detection from ground based telescopes.

Forsterite, quartz, and some other minerals are luminescing in red and blue spectral regions under the action of the fluxes of electrons. The spectra of luminescence of these minerals are often characterised by wide structureless bands in the red region with a peak near 600 nm.

We have obtained CL spectra of Tagish Lake forsterite with maximum near 440 and 650 nm. CL spectra of this forsterite are characterised in featureless nature with two main bumps. When the comet approaches the Sun, its electromagnetic and corpuscular radiation could excite intense luminescence of the cometary halo, including cathodoluminescence of the forsterite grains. CL luminescence of such forsterite particles may also be characterised in featureless emissions in blue and red parts of the spectrum. Such luminescence emissions will be superimposed on the faint solar continuum scattered by the cometary grains. The active cometary phenomena including outbursts and flares are characterised in release of the inner substance of cometary nuclei (relict dust and relict ice). Among the relicts might be pristine forsterite grains with the different sizes and shapes. The spectra of cometary outbursts have in many cases featureless character especially in blue range (maxima within 440–490 nm). Investigation of the cometary spectra obtained in time of outbursts might be as the effective tool for revealing of pristine cometary substance including presolar forsterite. Laboratory data of CL of Tagish Lake forsterite (obtained by us) might be suitable comparative sources in investigation of the cometary dust (cometary astromineralogy). It will be especially useful for revealing of presolar minerals of cometary substance.

5. Conclusions

(i)The CL zonation in Tagish Lake forsterite reflects rapid cooling and crystallization of the chondrule melts, preserving both structural defects (responsible for the blue CL emission) and inhomogeneities of activator elements, as well as possible remobilization of activators by later fluid processes on the parent asteroid.(ii)We conclude that a combination of scanning electron microscope-cathodoluminescence and Raman spectroscopy would be a powerful tool to understand not only the asteroidal processes but also the astromineralogical aspects of crystallization in the early solar system.(iii)Moreover, these techniques would be applied to the mineralogical investigations for the future sample-return missions, too.

Conflict of Interests

The authors declare that there is no conflict of interests regarding the publication of this paper.

Acknowledgments

Matthew M. R. Izawa acknowledges funding from NSERC and the Mineralogical Association of Canada, Arnold Gucsik was partly supported by the NRF Free-Standing Fellowship Program at the Department of Geology, University of Johannesburg, South Africa. Authors are grateful to Dr. Phil McCausland (University of Western Ontario, Canada) for lending the Tagish Lake meteorite thin section for this study.

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