# Meteorite falls in Bulgaria: Reappraisal of mineralogy, chemistry, and classification

Vesselin Dekov, Pierre Rochette, Jérôme Gattacceca

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Vesselin Dekov, Pierre Rochette, Jérôme Gattacceca. Meteorite falls in Bulgaria: Reappraisal of mineralogy, chemistry, and classification. Meteoritics and Planetary Science, 2017, 52 (8), pp.1649-1659. 10.1111/maps.12879. hal-01765582

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# Meteorite falls in Bulgaria: Reappraisal of mineralogy, chemistry, and classification

Vesselin DEKOV<fnref n="1" />,<fnref n="2" />* ID, Pierre ROCHETTE<fnref n="3" /> ID, and Jérôme GATTACCECA<fnref n="3" /> ID

*(Received 11 January 2016; revision accepted 15 March 2017)*

**Abstract**–We present a summary of the mineralogy, mineral chemistry, and magnetic characteristics of all the five Bulgarian meteorite falls. We report the first mineralogical descriptions, chemical analyses, and magnetic measurements of the Konevo (1931) and Silistra (1917) meteorites. We classify Konevo as LL5, and Silistra as an ungrouped achondrite with HED affinities. Pavel (1966; previously classified as an H5) is reclassified as H3-anomalous. We also provide precise mineralogy and mineral chemistry of the Virba meteorite (1873, L6), and more details on the mineral chemistry of Gumoschnik (1904, H5).

## INTRODUCTION

Five meteorite falls leading to the recovery of stones have occurred on the territory of Bulgaria (present-day boundaries): Virba (1873; Daubrée 1874), Gumoschnik (1904; Bontschev 1910), Silistra (1917; Dimov et al. 1972), Konevo (1931; Nikolov 1959), and Pavel (1966; Bonev 1966) (Fig. 1; Table 1). Two other falls were witnessed and described (Rasgrad [1740; von Hammer 1815], Ichera [1881; Škorpil 1884]) (Fig. 1), but to the best of our knowledge, the meteorites have not ended in any collection (Rasgrad; perhaps lost after recovery) or have not been recovered after the fall (Ichera). Meunier (1893) reported on another meteorite collected around Tirnowa (probably Turnovo, which corresponds to Veliko Turnovo, Bulgaria) in Roumélie (probably Rumelia, region of the Ottoman Empire including present-day Bulgaria) in 1873 and donated to the Muséum d'Histoire naturelle (Paris, France). However, this meteorite is not represented in the collections of the Muséum National d'Histoire Naturelle (former Muséum d'Histoire naturelle, Paris, France) (Caillet-Komorowski 2006), neither can it be found cataloged in any other meteorite collection in the world (Prior and Hey 1953; Grady 2000). This makes the existence of this meteorite dubious.

Knowledge of the five Bulgarian meteorites is fairly patchy. The most studied meteorites are Gumoschnik

and Pavel: bulk inorganic (Gumoschnik: Penchev et al. 1960; Dimov 1969, 1972, 1973; Pavel: Dimov 1973) and organic (Gumoschnik: Ivanov and Stoyanova 1973, 1984a, 1984b; Ivanov et al. 1984a; Pavel: Ivanov and Stoyanova 1973, 1984a, 1984b; Ivanov et al. 1984a, 1984b) chemistry, mineral chemistry (Gumoschnik: Mason 1963; Dod et al. 1992; Pavel: Dod et al. 1992; Kurchatov et al. 1998), mineralogy (Gumoschnik: Dimov 1969, 1972; Pavel: Kurchatov et al. 1998), and magnetic properties (Gumoschnik: Rochette et al. 2003). For the Virba fall (Daubrée 1874; Meunier 1893; Prior and Hey 1953), mineralogy (optical microscopy; Daubrée 1874; Meunier 1893), olivine composition (Mason 1963), and magnetic properties (Rochette et al. 2003) are reported in general. After a preliminary qualitative chemical study by laser microspectral analysis (Dimov et al. 1972), the Silistra has only recently been investigated in detail (Ruzicka et al. 2014). Konevo was also analyzed by Dimov et al. (1972), but has never been studied in any further detail.

Motivated by the virtual lack of mineralogical and chemical data on the Virba and Konevo meteorites, the scarce mineral chemistry data on the Gumoschnik and Pavel meteorites, the lack of magnetic property data on the Konevo and Pavel meteorites, and related uncertainties in the classification of these meteorites, we undertook a mineralogical-chemical-magnetic study to characterize these meteorites in more detail. Here we

<footnote n="1">¹Tokyo University of Marine Science and Technology, 4-5-7 Konan, Minato-ku, Tokyo 108-8477, Japan</footnote>

<footnote n="2">²Department of Marine Geosciences, IFREMER, Centre de Brest, 29280 Plouzané, France</footnote>

<footnote n="3">³ Aix-Marseille Univ, CNRS, IRD, Coll France, CEREGE, Aix-en-Provence, France</footnote>

<footnote>*Corresponding author. E-mail: vdekov0@kaiyodai.ac.jp</footnote>
<figure><img src="image_2.png" /><figcaption>Fig. 1. Location map of all meteorite falls in Bulgaria. Solid stars = falls with meteorite collected; open stars = witnessed falls without meteorite representation in collections.</figcaption></figure>

<table><caption>Table 1. Main characteristics of Bulgarian meteorites ordered by fall date. Data from this work, Meteoritical Bulletin, and Grady (2000).</caption><thead><tr><th>Meteorite</th><th>Fall date</th><th>Latitude, longitude</th><th>Class</th><th>Total initial mass (g)</th><th>Mass available (g)</th><th>Collection<sup>1</sup></th><th>Logχ</th><th>Fa%</th></tr></thead><tbody><tr><td>Rasgrad</td><td>1740</td><td>43° 30′N, 26° 32′E</td><td>–</td><td>25 000</td><td>none</td><td>none</td><td></td><td></td></tr><tr><td>Virba</td><td>1873</td><td>43° 32′N, 22° 38′E</td><td>L6</td><td>3 600</td><td>185</td><td>2, 3, 4, 5, 6, 8</td><td>4.86 ± .04</td><td>25.9 ± 0.5</td></tr><tr><td>Ichera?</td><td>1881?</td><td>42° 43′N, 26° 31′E</td><td>–</td><td>?</td><td>none</td><td>none</td><td></td><td></td></tr><tr><td>Gumoschnik</td><td>1904</td><td>42° 54′N, 24° 42′E</td><td>H5</td><td>5 700</td><td>706</td><td>1, 2, 3, 4, 5, 7, 9</td><td>5.25 ± .03</td><td>19.2 ± 0.2</td></tr><tr><td>Silistra</td><td>1917</td><td>43° 28′N, 25° 31′E</td><td>Ungrouped achondrite</td><td>0.15</td><td>0.12</td><td>1</td><td>2.56</td><td></td></tr><tr><td>Konevo</td><td>1931</td><td>42°32′N, 26°10′E</td><td>LL5</td><td>90</td><td>1.5</td><td>1</td><td>4.00</td><td>28.4 ± 0.2</td></tr><tr><td>Pavel</td><td>1966</td><td>43° 28′N, 25° 31′E</td><td>H3 anomalous</td><td>2970</td><td>64</td><td>3, 7, 9</td><td>5.11 ± .02</td><td>19.7 ± 1.9</td></tr></tbody></table>

report the results of this investigation and combine them with some basic data from the previous studies in a synthesis on the meteorite falls in Bulgaria.

Our systematic study of the historic meteorite collection from Bulgaria emphasizes the interest of performing such a revisit of poorly characterized historical collections.

## MATERIAL AND METHODS

Subsamples of all five meteorites were obtained from the Museum of Mineralogy, Petrology and Mineral Resources at the University of Sofia (Sofia, Bulgaria)

(Gumoschnik, Silistra, and Konevo meteorites), Muséum national d'Histoire naturelle (Paris, France) (Virba meteorite), and Meteorite Laboratory (Gifhorn, Germany) (Pavel meteorite).

Polished blocks of all subsamples were investigated by reflected light optical microscopy (Olympus BX60 polarizing microscope) for mineral identification and texture. We were not able to determine the shock stage of these meteorites, because the shock classification relies largely on transmitted light microscopy.

Chemical compositions and backscattered electron (BSE) images of the minerals were acquired on the C-coated polished sections using a Cameca SX 100

<footnote n="1">¹Collection codes: 1 Sofia, 2 Vienna, 3 Berlin, 4 Paris, 5 London, 6 Vatican, 7 Moscow, 8 Chicago, 9 Bartoschewitz (not exhaustive); in italic, collection where we obtained magnetic susceptibility data.</footnote>

<footnote>New classifications are highlighted in bold.</footnote>
electron microprobe (EMP) (V = 15 kV, I = 20 nA, electron beam diameter of 2 µm). Standards used were: FeS₂ (S Kα and Fe Kα), Ni metal (Ni Kα), Co metal (Co Kα), Cu metal (Cu Kα), albite (Si Kα and Na Kα), Al₂O₃ (Al Kα), TiMnO₃ (Ti Kα and Mn Kα), Cr₂O₃ (Cr Kα), forsterite (Mg Kα), wollastonite (Ca Kα), orthoclase (K Kα), apatite (P Kα), and V metal (V Kα), and detection limits (wt%) were 0.05 for S, 0.06 for Fe, 0.10 for Ni, 0.08 for Co, 0.12 for Cu, 0.03 for Si, 0.03 for Na, 0.02 for Al, 0.04 for Ti, 0.05 for Mn, 0.05 for Cr, 0.02 for Mg, 0.04 for Ca, 0.03 for K, 0.03 for P, and 0.06 for V.

Magnetic measurements were performed in CEREGE using an Agico MFK-1 Bridge for magnetic susceptibility and Micromag Vibrating Sample Magnetometer for hysteresis. Magnetic susceptibility of larger samples of Gumoschnik, Pavel, and Virba were previously measured in Berlin, Moscow, Paris, and Vatican collections using a Bartington MS2 bridge or a SM30 probe from ZH Instruments (see Rochette et al. [2003] for results and detailed methodology). Magnetic susceptibility provides, regardless of sample size and shape, a rapid way to estimate the amount of magnetic minerals (mostly metal in ordinary chondrite), which allows discriminating between LL, L, and H classes. Magnetic hysteresis measurements need small fragments (<1 g), provide more quantitative measurement of metal amount, and allow also more detailed assessment of magnetic mineralogy: presence of tetrataenite, identification of paramagnetic contribution due to iron in silicates, etc. (see Gattacceca et al. 2014).

Measurements of the O isotope composition were performed at CEREGE using laser fluorination technique (see Suavet et al. 2010).

## MINERALOGY, CHEMISTRY, AND CLASSIFICATION

### Virba

This meteorite fell in an oak forest nearby Virba village (Vidin district) on June 6, 1873 (Daubrée 1874; Meunier 1893; Prior and Hey 1953). The fall had been accompanied by a sonic effect and the meteorite is said to have penetrated about 1 m into the soil (Daubrée 1874). Total original mass was ~3.6 kg (Daubrée 1874). The main mass of 3.06 kg is housed in the Natural History Museum at Budapest (Hungary), but it is unsuitable for scientific investigations due to damage caused by a fire during the anticommunist revolt of 1956 (Embey-Isztin, personal communication). Only 185 g remain in other collections (Table 1).

The first studies of the Virba ordinary chondrite described its basic mineralogy on the basis of optical microscopy and chemical tests (observations after

treatment with a weak HCl): FeNi minerals (Daubrée 1874; Meunier 1893), Fe-sulfide (Daubrée 1874; Meunier 1893), Mg-rich olivine (Daubrée 1874), and enstatite (Daubrée 1874). Later works reported on its olivine composition (Fa₂₅, based on X-ray diffraction; Mason 1963) and magnetic susceptibility (logχ = 4.86 ± 0.04, with χ in 10⁻⁹ m³ kg⁻¹, average of three samples; Rochette et al. 2003).

Our petrographic observations confirm that the Virba is a strongly metamorphosed ordinary chondrite. The troilite (Table 2) is always fissured (Figs. 2A and 2B) and very often associated with FeNi metal. Virba contains the entire range of FeNi native minerals from the most Ni-rich tetrataenite through the varieties with increasing Fe content (taenite and kamacite) up to the Ni-poor kamacite (Table 2). The two endmembers of the FeNi native metal series, Ni-rich (tetrataenite), and Fe-rich (Ni-poor kamacite), form either intimate, fine, eutectic-like microtexture, or segregate at the contact with troilite (Figs. 2A and 2B). Accessory native Cu (2–10 µm) is frequently observed in Virba, occurring within FeNi metal close to the FeNi metal-troilite contact (Figs. 2A and 2B). It was analyzed by EMP, but the results are not reported in Table 2 because the grain size was too small to ensure correct quantification.

Some glassy shock veins with finely dispersed droplets of FeNi metal and troilite are present (Fig. 2C). Well-preserved chondrules of olivine and pyroxene are rare. The composition of olivine (Fa₂₅.₉±₀.₅, n = 9), low-Ca pyroxene (Fs₂₂.₃±₁.₁-Wo₁.₈±₀.₃, n = 9), as well as Co content of kamacite (0.96 wt%) is typical for equilibrated L chondrites (Tables 2 and 3). Chromite is fissured (Figs. 2A and 2B) and with composition Chro₈₄.₅-Sp₁₂.₀-Ulvö₃.₄₁ (Table 3) if normalized using just the three main spinel endmembers (chromite, spinel, and ulvöspinel). Accessory anhedral merrillite and apatite (50–100 µm) are interstitial among the silicates (Fig. 2D). Their structural formulae calculated on the basis of the chemical composition (Table 3) are: (Mg₁.₈₀Fe₀.₂₀Mn₀.₀₁) Ca₁₈Na₁.₉(P₁₃.₉Si₀.₀₂)O₅₆ for merrillite and Ca₄.₉₈ Na₀.₀₇(PO₄)₃.₁₄(OH,F,Cl) for apatite.

All data obtained confirm the previous classification as a L6 chondrite.

### Gumoschnik

This ordinary chondrite shower was observed over the villages of Vrabevo, Gumoschnik, and Debnevo (Troyan district) at 06:20 P.M. on April 28, 1904 (Bontschev 1910). Strong thunder accompanied a bolide flight from north to south and the fall of six stones (total weight 5.669 kg): 3.815 kg (Vrabevo), 1.475 kg (Gumoschnik), and 0.253 kg (Debnevo), and three smaller pieces of 0.083, 0.026, and 0.017 kg (Bontschev 1910).
<table><caption>Table 2. Composition (EMP data) of sulfides and native metals in the Virba, Gumoshnik, Konevo, and Pavel meteorites.</caption><thead><tr><th rowspan="2">Mineral</th><th rowspan="2">Meteorite</th><th rowspan="2">#<sup>1</sup></th><th>S</th><th rowspan="2">Fe</th><th rowspan="2">Ni</th><th rowspan="2">Co</th><th rowspan="2">Cu</th><th rowspan="2">Total</th><th rowspan="2">Structural formulae</th></tr><tr><th>(wt%)</th></tr></thead><tbody><tr><td rowspan="4">Troilite</td><td>Virba</td><td>10</td><td>36.6</td><td>63.8</td><td>&lt;0.10</td><td>&lt;0.08</td><td>&lt;0.12</td><td>100.4</td><td>Fe<sub>1.00</sub>S<sub>1.00</sub></td></tr><tr><td>Gumoschnik</td><td>10</td><td>36.4</td><td>63.5</td><td>0.10</td><td>&lt;0.08</td><td>0.30</td><td>100.3</td><td>Fe<sub>1.00</sub>S<sub>1.00</sub></td></tr><tr><td>Konevo</td><td>8</td><td>36.4</td><td>63.0</td><td>0.10</td><td>&lt;0.08</td><td>&lt;0.12</td><td>99.5</td><td>Fe<sub>0.99</sub>S<sub>1.00</sub></td></tr><tr><td>Pavel</td><td>12</td><td>36.5</td><td>62.0</td><td>&lt;0.10</td><td>&lt;0.08</td><td>&lt;0.12</td><td>98.6</td><td>Fe<sub>0.98</sub>S<sub>1.02</sub></td></tr><tr><td rowspan="3">Tetrataenite</td><td>Virba</td><td>13</td><td>&lt;0.05</td><td>49.1</td><td>50.3</td><td>0.10</td><td>0.70</td><td>100.2</td><td>Fe<sub>0.50</sub>Ni<sub>0.49</sub>Cu<sub>0.01</sub></td></tr><tr><td>Gumoschnik</td><td>3</td><td>&lt;0.05</td><td>50.2</td><td>49.8</td><td>&lt;0.08</td><td>0.36</td><td>100.4</td><td>Fe<sub>0.51</sub>Ni<sub>0.48</sub></td></tr><tr><td>Pavel</td><td>3</td><td>&lt;0.05</td><td>44.8</td><td>53.3</td><td>&lt;0.08</td><td>&lt;0.12</td><td>98.5</td><td>Fe<sub>0.50</sub>Ni<sub>0.50</sub></td></tr><tr><td rowspan="4">Taenite</td><td>Virba</td><td>2</td><td>&lt;0.05</td><td>68.0</td><td>31.6</td><td>0.25</td><td>0.12</td><td>100.0</td><td>Fe<sub>0.69</sub>Ni<sub>0.31</sub></td></tr><tr><td>Gumoschnik</td><td>5</td><td>&lt;0.05</td><td>64.4</td><td>35.4</td><td>0.10</td><td>0.25</td><td>100.2</td><td>Fe<sub>0.65</sub>Ni<sub>0.34</sub></td></tr><tr><td>Konevo</td><td>14</td><td>&lt;0.05</td><td>63.4</td><td>34.8</td><td>1.35</td><td>0.20</td><td>99.8</td><td>Fe<sub>0.65</sub>Ni<sub>0.34</sub>Co<sub>0.01</sub></td></tr><tr><td>Pavel</td><td>2</td><td>&lt;0.05</td><td>64.8</td><td>32.1</td><td>0.12</td><td>&lt;0.12</td><td>97.0</td><td>Fe<sub>0.70</sub>Ni<sub>0.30</sub></td></tr><tr><td rowspan="3">Kamacite</td><td>Virba</td><td>5</td><td>&lt;0.05</td><td>94.3</td><td>4.93</td><td>0.96</td><td>&lt;0.12</td><td>100.3</td><td>Fe<sub>0.94</sub>Ni<sub>0.05</sub>Co<sub>0.01</sub></td></tr><tr><td>Gumoschnik</td><td>15</td><td>&lt;0.05</td><td>94.1</td><td>6.20</td><td>0.51</td><td>&lt;0.12</td><td>100.8</td><td>Fe<sub>0.94</sub>Ni<sub>0.06</sub></td></tr><tr><td>Konevo</td><td>11</td><td>&lt;0.05</td><td>93.2</td><td>3.86</td><td>3.18</td><td>&lt;0.12</td><td>100.3</td><td>Fe<sub>0.93</sub>Ni<sub>0.04</sub>Co<sub>0.03</sub></td></tr><tr><td rowspan="3">Ni-poor kamacite</td><td>Pavel</td><td>15</td><td>&lt;0.05</td><td>91.0</td><td>6.23</td><td>0.51</td><td>&lt;0.12</td><td>97.8</td><td>Fe<sub>0.90</sub>Ni<sub>0.10</sub></td></tr><tr><td>Virba</td><td>2</td><td>&lt;0.05</td><td>97.5</td><td>2.78</td><td>0.60</td><td>&lt;0.12</td><td>100.9</td><td>Fe<sub>0.97</sub>Ni<sub>0.03</sub>Co<sub>0.01</sub></td></tr><tr><td>Gumoschnik</td><td>4</td><td>&lt;0.05</td><td>97.5</td><td>3.58</td><td>0.38</td><td>&lt;0.12</td><td>101.5</td><td>Fe<sub>0.96</sub>Ni<sub>0.03</sub></td></tr></tbody></table>

<figure><img src="image_3.png" /><figcaption>Fig. 2. Photomicrographs of textures and mineralogy of the Virba meteorite (polished sections). A) Fissured troilite (tr), chromite (chr), kamacite (ka), tetrataenite (tta), and native Cu (Cu⁰) (optical polarizing microscope, reflected light, ×N). B) Same as in (A) in BSE (EMP). C) Shocked glass vein with dispersed FeNi metal and troilite droplets (optical polarizing microscope, reflected light, ‖N). D) Merrillite (me) within silicate (olivine [ol], low-Ca pyroxene [opx]), and FeNi metal (kamacite [ka], taenite [ta]) matrix (BSE-EMP). (Color figure can be viewed at wileyonlinelibrary.com.)</figcaption></figure>

Several studies have described the mineralogy (olivine, low-Ca pyroxene, augite, FeNi metal, troilite, chromite, and glass) and bulk chemistry of the stones

Gumoschnik and Debnevo pointing out their similar composition (Bontschev 1910; Penchev et al. 1960; Dimov 1969, 1972, 1973). Mineral chemistry studies

<footnote n="1">¹Number of analyses.</footnote>
<table><caption>Table 3. Composition (EMP data) of silicates, chromites, and phosphates in the Virba, Gumoschnik, Konevo, and Pavel meteorites.</caption><thead><tr><th rowspan="2">Mineral</th><th rowspan="2">Meteorite</th><th rowspan="2">#<fnref n="1" /></th><th colspan="10">SiO<sub>2</sub></th><th rowspan="2">Total</th><th rowspan="2">Endmembers</th></tr><tr><th>Al<sub>2</sub>O<sub>3</sub></th><th>TiO<sub>2</sub></th><th>FeO</th><th>Cr<sub>2</sub>O<sub>3</sub></th><th>MnO</th><th>MgO</th><th>CaO</th><th>Na<sub>2</sub>O</th><th>K<sub>2</sub>O</th><th>P<sub>2</sub>O<sub>5</sub></th><th>NiO</th><th>CoO</th><th>V<sub>2</sub>O<sub>3</sub></th></tr></thead><tbody><tr><td rowspan="3">Olivine</td><td>Virba</td><td>9</td><td>38.1</td><td>&lt;0.02</td><td>&lt;0.04</td><td>23.2</td><td>&lt;0.05</td><td>0.49</td><td>37.3</td><td>0.04</td><td>&lt;0.03</td><td>&lt;0.03</td><td>0.04</td><td>&lt;0.08</td><td>&lt;0.07</td><td>&lt;0.06</td><td>99.4</td><td>Fa25.9±0.5</td></tr><tr><td>Gumoschnik</td><td>15</td><td>39.4</td><td>&lt;0.02</td><td>&lt;0.04</td><td>17.9</td><td>&lt;0.05</td><td>0.46</td><td>42.2</td><td>&lt;0.04</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.08</td><td>&lt;0.07</td><td>&lt;0.06</td><td>100.1</td><td>Fa19.2±0.2</td></tr><tr><td>Konevo</td><td>5</td><td>37.4</td><td>0.02</td><td>&lt;0.04</td><td>25.8</td><td>0.08</td><td>0.46</td><td>36.5</td><td>0.04</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.08</td><td>&lt;0.07</td><td>&lt;0.06</td><td>100.3</td><td>Fa28.4±0.2</td></tr><tr><td rowspan="3">Low-Ca<br>pyroxene</td><td>Pavel</td><td>27</td><td>39.6</td><td>0.04</td><td>0.05</td><td>18.2</td><td>0.08</td><td>0.47</td><td>41.6</td><td>0.04</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.08</td><td>&lt;0.07</td><td>&lt;0.06</td><td>100.1</td><td>Fa19.7±1.9 (range 11.8-23.7)</td></tr><tr><td>Virba</td><td>9</td><td>54.4</td><td>0.16</td><td>0.17</td><td>15.0</td><td>0.09</td><td>0.46</td><td>27.4</td><td>0.86</td><td>0.03</td><td>&lt;0.03</td><td>&lt;0.03</td><td>0.10</td><td>&lt;0.07</td><td>&lt;0.06</td><td>98.7</td><td>Fs22.3±1.1*Wo1.8±0.3</td></tr><tr><td>Gumoschnik</td><td>3</td><td>56.6</td><td>0.17</td><td>0.16</td><td>11.2</td><td>0.14</td><td>0.52</td><td>30.7</td><td>0.54</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.08</td><td>&lt;0.07</td><td>&lt;0.06</td><td>100.1</td><td>Fs16.8±1.0*Wo1.0±0.3</td></tr><tr><td rowspan="2">Pavel</td><td>Konevo</td><td>2</td><td>54.6</td><td>0.19</td><td>0.19</td><td>15.7</td><td>0.14</td><td>0.49</td><td>27.9</td><td>0.89</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.08</td><td>&lt;0.07</td><td>&lt;0.06</td><td>100.1</td><td>Fs23.5±0.2*Wo1.7±0.1</td></tr><tr><td></td><td>23</td><td>56.4</td><td>0.20</td><td>0.06</td><td>12.3</td><td>0.47</td><td>0.58</td><td>29.4</td><td>0.69</td><td>0.07</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.08</td><td>&lt;0.07</td><td>&lt;0.06</td><td>100.2</td><td>Fs19.0±6.3 (range 7.8-32.6)*</td></tr><tr><td rowspan="3">Clinopyroxene</td><td>Virba</td><td>2</td><td>53.1</td><td>0.51</td><td>0.49</td><td>5.23</td><td>0.82</td><td>0.21</td><td>15.7</td><td>21.6</td><td>0.60</td><td>&lt;0.03</td><td>0.26</td><td>&lt;0.08</td><td>&lt;0.07</td><td>&lt;0.06</td><td>98.7</td><td>Fs8.58*Wo4.5</td></tr><tr><td>Gumoschnik</td><td>4</td><td>54.5</td><td>0.76</td><td>0.35</td><td>5.57</td><td>0.68</td><td>0.32</td><td>20.9</td><td>15.7</td><td>0.47</td><td>&lt;0.03</td><td>0.15</td><td>&lt;0.08</td><td>&lt;0.07</td><td>0.06</td><td>99.4</td><td>Fs12.6*Wo2.3</td></tr><tr><td>Konevo</td><td>2</td><td>52.7</td><td>0.48</td><td>0.44</td><td>6.04</td><td>0.87</td><td>0.27</td><td>16.5</td><td>20.7</td><td>0.39</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.08</td><td>&lt;0.07</td><td>&lt;0.06</td><td>98.4</td><td>Fs9.75*Wo4.28</td></tr><tr><td rowspan="3">Chromite</td><td>Pavel</td><td>2</td><td>53.8</td><td>0.63</td><td>0.17</td><td>13.0</td><td>2.29</td><td>0.81</td><td>17.5</td><td>11.3</td><td>0.88</td><td>0.04</td><td>&lt;0.03</td><td>&lt;0.08</td><td>&lt;0.07</td><td>&lt;0.06</td><td>100.5</td><td>Fs29.4*Wo2.47</td></tr><tr><td>Virba</td><td>6</td><td>0.10</td><td>5.90</td><td>2.59</td><td>31.1</td><td>56.5</td><td>0.71</td><td>2.29</td><td>&lt;0.04</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.08</td><td>&lt;0.07</td><td>0.84</td><td>100.1</td><td>Chro84.5*Sp12.0*UlvÖ3.41</td></tr><tr><td>Gumoschnik</td><td>5</td><td>1.00</td><td>6.55</td><td>1.66</td><td>29.2</td><td>55.8</td><td>0.91</td><td>2.96</td><td>0.49</td><td>0.04</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.08</td><td>&lt;0.07</td><td>0.80</td><td>99.4</td><td>Chro83.0*Sp14.8*UlvÖ2.23</td></tr><tr><td rowspan="2">Merrillite<br>Apatite</td><td>Pavel</td><td>5</td><td>0.07</td><td>6.25</td><td>3.36</td><td>32.6</td><td>54.8</td><td>0.10</td><td>1.81</td><td>&lt;0.04</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.08</td><td>0.07</td><td>0.69</td><td>99.7</td><td>Chro84.6*Sp11.0*UlvÖ4.37</td></tr><tr><td>Virba</td><td>4</td><td>0.11</td><td>6.50</td><td>2.11</td><td>28.4</td><td>56.9</td><td>0.68</td><td>3.28</td><td>&lt;0.04</td><td>0.03</td><td>&lt;0.03</td><td>&lt;0.03</td><td>&lt;0.08</td><td>&lt;0.07</td><td>&lt;0.06</td><td>98.0</td><td>Chro81.8*Sp15.4*UlvÖ2.80</td></tr><tr><td rowspan="2">Apatite</td><td>Virba</td><td>3</td><td>0.06</td><td>&lt;0.02</td><td>&lt;0.04</td><td>0.84</td><td>&lt;0.05</td><td>&lt;0.05</td><td>3.48</td><td>47.1</td><td>2.74</td><td>0.05</td><td>46.0</td><td>&lt;0.08</td><td>&lt;0.07</td><td>&lt;0.06</td><td>100.3</td><td>-</td></tr><tr><td></td><td>2</td><td>0.14</td><td>&lt;0.02</td><td>&lt;0.04</td><td>0.47</td><td>&lt;0.05</td><td>&lt;0.05</td><td>0.05</td><td>53.7</td><td>0.42</td><td>&lt;0.03</td><td>42.1</td><td>&lt;0.08</td><td>&lt;0.07</td><td>&lt;0.06</td><td>97.0</td><td>-</td></tr></tbody></table>

<footnote n="1">¹Number of analyses.</footnote>
<figure><img src="image_4.png" /><figcaption>Fig. 3. Photomicrographs of textures and mineralogy of the Gumoschnik meteorite (polished sections). A) Silicate matrix with chondrules (ch) and FeNi metal (white) (optical polarizing microscope, reflected light, ‖ N). B) Barred olivine (ol) chondrule with a glass matrix of plagioclase composition and surrounded by FeNi metal (white) (BSE-EMP). C) Troilite (tr), chromite (chr), kamacite (ka), taenite (ta), and native Cu (Cu⁰) (optical polarizing microscope, reflected light, ×N). D) Troilite (tr), kamacite (ka), taenite (ta), and native Cu (Cu⁰) (BSE-EMP). E) Shocked glass vein with dispersed FeNi metal and troilite droplets (optical polarizing microscope, reflected light, ‖ N). (Color figure can be viewed at wileyonlinelibrary.com.)</figcaption></figure>

report the compositions of olivine (Fa₁₉.₂₋₂; Mason 1963; Dod et al. 1992) and low-Ca pyroxene (Fs₁₆.₂₋₂; Dod et al. 1992). Measured magnetic susceptibility is $logχ = 5.26 ± 0.05$, with $χ$ in $10^{-9} m^3 kg^{-1}$ (Rochette et al. 2003), i.e., typical for an H chondrite.

Our petrographic observations confirm that the Gumoschnik is a moderately metamorphosed ordinary chondrite with well-defined chondrules. Troilite (Table 2) is rarely fissured and often associated with FeNi metal (Fig. 3C). Gumoschnik (like Virba) has the whole range of FeNi native minerals from tetrataenite (the most Ni-rich) to Ni-poor kamacite (Table 2).

Different FeNi native minerals are clearly separated from each other (Figs. 3C and 3D). Native Cu (2–10 µm) occurs in the FeNi native minerals at the contact troilite-FeNi metal (Figs. 3C and 3D).

Shocked glass veins with dispersed or localized at the vein boundaries FeNi metal and troilite droplets (Fig. 3E) are rare. The olivine composition (Fa₁₉.₂±₀.₂, n = 15; Table 3) is within the compositional range determined previously (Fa₁₉.₂₋₂; Mason 1963; Dod et al. 1992). The ferrosilite component of low-Ca pyroxene measured in this study (Fs₁₆.₈±₁.₀, n = 3; Table 3) is within the compositional range measured previously
<figure><img src="image_5.png" /><figcaption>Fig. 4. Photographs of the whole Silistra stone showing its inner face (A) and one exterior side (B). The small ellipse superimposed on the two views allows visualization of the rotation. (Color figure can be viewed at wileyonlinelibrary.com.)</figcaption></figure>

(Fs<sub>16-21</sub>; Dod et al. 1992). Clinopyroxene composition is Fs<sub>12.6</sub>-Wo<sub>32.3</sub> (n = 4; Table 3). Chromite is rare, fissured (Fig. 3C) and with composition CrHo<sub>8.3</sub>-Sp<sub>14.8</sub>-Ulvö<sub>2.23</sub> (Table 3).

Olivine and low-Ca pyroxene composition, as well
as Co content in kamacite (0.51 wt%) are typical for
equilibrated H chondrites. Our observations confirm the
previous H5 classification of Gumoschnik with possible
shock stage S5 (based on melt vein presence).

Silistra

The Silistra meteorite is a small (0.15 g) single
stone, which was not previously investigated and
declared as a meteorite, despite a detailed description
of the circumstances of the fall and recovery by a
teacher in natural sciences from Silistra High School.
It was identified as a meteorite by our investigations,
reported in Ruzicka et al. (2014). It appears as black
pumice with no visible crystals and has extremely high
porosity (86%). One side of the stone is rounded and
coated with translucent material (fusion crust), whereas
the other side is a broken surface (Fig. 4). Saturation
magnetization (M<sub>S</sub>) is 0.007 Am<sup>2</sup> kg<sup>-1</sup> and indicates
that metallic iron is present in very low concentrations,
with a maximum content of about 30 ppm. Magnetic
susceptibility (logχ = 2.57, χ in 10<sup>-9</sup> m<sup>3</sup> kg<sup>-1</sup>) is lower
than in HED meteorites (Rochette et al. 2009), and
can entirely be accounted for by silicate paramagnetism
(Gattacceca et al. 2008). Oxygen isotopic composition

of the Silistra meteorite (Δ¹⁷O of -0.27 ± 0.02) lies on
the HED fractionation line (Greenwood et al. 2005),
indicating that it is not terrestrial pumice and likely
derives from the melting of HED material. Major
element composition revealed by EMP is also typical
of eucrite: Na₂O = 0.26 wt%, MgO = 9.2 wt%,
SiO₂ = 48.5 wt%, Al₂O₃ = 14.1 wt%, CaO = 9.9 wt%,
TiO₂ = 0.12 wt%, Cr₂O₃ = 0.38 wt%, FeO = 15.1 wt
%, and Fe/Mn = 29. Whether Silistra's melting
occurred during the entry in the Earth's atmosphere
(making it a thickened foamy fusion crust detached
from a normal HED meteorite), or at the surface of
Vesta (e.g., as an impact melt) remains to be clarified.
Ongoing complex characterization using various
geochemical and physical techniques should allow us to
propose an in-depth interpretation of this mysterious
material in a forthcoming publication. We therefore
refrain from reporting further data in the present
paper.

Konevo

This ordinary chondrite fell in the backyard of Mr.
P. Sevkov, Konevo village (Nova Zagora district) at
about 01:00 A.M. on May 26, 1931 (Nikolov 1959). The
flight path of the bolide had an E-W direction and was
reportedly accompanied by sonic and lightning effects.
The meteorite was the size of a chicken egg with an
original mass of ~80–100 g (Nikolov 1959). During the
fall, it broke into several pieces and only one of them
<figure><img src="image_6.png" /></figure>

<figure><img src="image_7.png" /></figure>

<figure><img src="image_8.png" /><figcaption>Fig. 5. Photomicrographs of textures and mineralogy of the Konevo meteorite (polished sections; optical polarizing microscope, reflected light). A) Fissured troilite (tr) with shock-induced twinning (×N). B) Troilite (tr), taenite (ta), kamacite (ka), and native Cu (Cu⁰) (||N). C) Fusion crust (right-hand side) with skeletal magnetite (mt), taenite (ta), chromite (chr), and shocked veins of taenite (ta) (left-hand side) (||N). (Color figure can be viewed at wileyonlinelibrary.com.)</figcaption></figure>

(~1.47 g) reached the Museum of Mineralogy, Petrology and Mineral Resources (University of Sofia) as a donation by Mr. E. Koen (geologist). There has been only one attempt to investigate the chemistry of this meteorite (Dimov et al. 1972), but no quantitative data were provided by this study.

The texture of this meteorite is typical of an equilibrated ordinary chondrite, with poorly defined chondrules and fine-grained plagioclase. Plagioclase grain size is mostly below 50 µm indicating a metamorphic type 5 (Van Schmus and Wood 1967). The Konevo meteorite shows clear evidence of shock: troilite is fissured and shows stress twinning (Fig. 5A), silicates and chromite are fissured, beneath the fusion crust there is a zone of a veinlet net filled with taenite (Fig. 5C).

The main minerals in the Konevo meteorite are olivine, low-Ca pyroxene, clinopyroxene, sodic plagioclase, chromite, troilite, and FeNi native minerals (tetrataenite, taenite, and kamacite) (Tables 2 and 3). Troilite (Figs. 5A and 5B; Table 2) is the most abundant opaque phase and the only sulfide identified. Grains of taenite and kamacite are always in close intergrowths (Fig. 5B). A particle of native Cu (~5 µm across) was found in a taenite-kamacite grain (Fig. 5B). EMP analyses indicated an equilibrated silicate composition: olivine Fa₂₈.₄±₀.₂ (n = 5), low-Ca pyroxene Fs₂₃.₅±₀.₂-Wo₁.₇±₀.₁ (n = 2), and clinopyroxene Fs₀.₇₅-Wo₄₂.₈ (n = 2) (Table 3). Chromite grains are rare (Fig. 5C), rich in Fe and Cr, and with a mean composition CrHo₈.₆-Sp₁₁.₀-UlvO₄.₃₇ (Table 3). Fusion crust is composed of glass matrix with skeletal magnetite crystals (Fig. 5C).

Magnetic susceptibility (logχ = 3.99, with χ in 10⁻⁹ m³ kg⁻¹) and saturation magnetization (M_s = 4.05 Am² kg⁻¹) are typical of LL chondrites (Rochette et al. 2003; Gattacceca et al. 2014).

The olivine and low-Ca pyroxene compositions, the Co versus Ni content of kamacite and taenite (Brearley and Jones 1998), abundance of tetrataenite relative to kamacite and taenite, as well as magnetic properties all indicate the Konevo meteorite belongs to the LL group. Therefore, it is classified as a LL5 ordinary chondrite.

## Pavel

This meteorite fell nearby the Pavel village (Veliko Turnovo district) at about 02:00 P.M. on February 28, 1966 (Bonev 1966). The fall of two stones (2.962 kg and 6 g) was accompanied by sonic effects (crash, peals, and whistle) and a dust trail directed W-E. The larger meteorite made a hole of irregular shape, inclined W-E and ~0.3 m deep (Bonev 1966). The main mass was housed in the meteorite collection of the
<figure><img src="image_9.png" /><figcaption>Fig. 6. Photomicrographs of textures and mineralogy of the Pavel meteorite (polished sections; optical polarizing microscope, reflected light). A) Olivine (ol) chondrule in a matrix of silicates and FeNi metal (white) (|| N). B) Troilite (tr), taenite (ta), and chromite (chr) (×N). C) Fusion crust with skeletal magnetite (mt) (|| N). D) Shocked veins of taenite (ta) (|| N). E) Hollow vein with walls of glass with scattered droplets of troilite and FeNi metal, troilite (tr), and taenite (ta) (|| N). F) Close-up of the vein with troilite (tr) droplets in the glass matrix (|| N). (Color figure can be viewed at wileyonlinelibrary.com.)</figcaption></figure>

Museum of Mineralogy, Petrology and Mineral Resources (University of Sofia) until 2000 when it was stolen.

Previous studies report on the mineralogy (olivine, augite, plagioclase, kamacite, taenite, troilite, chromite, magnetite, apatite (?), and glass) (Dimov 1973; Kurchatov et al. 1998), bulk chemistry (Dimov 1973), and mineral chemistry (Dod et al. 1992; Kurchatov et al. 1998) of the meteorite. The measured composition of olivine is Fa₁₉-₂₀ and that of low-Ca pyroxene is Fs₁₇-₂₂ (Dod et al. 1992). Kurchatov et al. (1998) reported olivine and pyroxene compositions (EMP data), but have not presented the mineral endmembers;

we have further calculated them for comparison with our data.

The Pavel meteorite is brecciated and contains a number of well-defined complete or fragmented chondrules. The average apparent chondrule diameter is 500 ± 186 µm (n = 32) intermediate between that of H and L chondrites (300 and 700 µm, respectively; see Weisberg et al. 2006).

Troilite (Table 2) is fissured, often associated with FeNi metal and frequently with a number of small (<2 µm) pores (Fig. 6B). Pavel has the entire range of FeNi native minerals: tetrataenite, taenite, and kamacite (Table 2; Fig. 6B). We have not observed native Cu.
The olivine average composition (Fa<sub>19.7±1.9</sub>, n = 27; Table 3) is within the compositional range determined previously (Fa<sub>19-20</sub>, Dod et al. 1992; Fa<sub>22.1</sub>, estimated from Kurchatov et al. 1998). The observed range, from Fa<sub>11.8</sub> to Fa<sub>23.7</sub>, as well as the percentage mean deviation (PMD, as defined in Van Schmus and Wood 1967) of 5.2% indicate that Pavel is an unequilibrated chondrite with petrographic grade 3, and that the previous H5 classification has to be revised. The ferrosilite component of low-Ca pyroxene measured in this study (Fs<sub>19.0±6.3</sub>, n = 23; Table 3) is comparable to that measured previously (Fs<sub>17-22</sub>, Dod et al. 1992; Fs<sub>15.6</sub>, estimated from Kurchatov et al. 1998). The observed range, from Fs<sub>7.7</sub> to Fs<sub>32.6</sub>, and PMD of 26% confirm that Pavel is a type 3 chondrite. Clinopyroxene composition (Fs<sub>29.4</sub>-Wo<sub>24.7</sub>, n = 2, Table 3) is comparable to that estimated from the previously reported data (Fs<sub>30.0</sub>-Wo<sub>38.8</sub>, Kurchatov et al. 1998) in respect to the ferrosilite component only. Chromite is rare, fissured (Fig. 6B), and with composition Chro<sub>81.8</sub>-Sp<sub>15.4</sub>-Ulvö<sub>2.80</sub> (Table 3). Fusion crust is composed of glass matrix with skeletal magnetite crystals (Fig. 6C). A glass zone (plagioclase composition) cut through by a veinlet net filled with taenite underlies the fusion crust (Fig. 6D). We observed a hollow vein (~50 µm across) with glass walls (with approximately olivine composition) containing dispersed droplets of troilite and FeNi metal (Figs. 6E and 6F). A likely scenario of this unusual vein formation may include (1) shock-induced melting, (2) shock rebound generating a gaseous cavity in the previously compressed dissolved gas rich melt vein, and (3) flowing of the melt with elongated bubble and metal-sulfide droplet formation (Fig. 6F).

Magnetic susceptibility of the Pavel meteorite is $logχ = 5.11 ± 0.02 10^{-9} m^3 kg^{-1}$ on two pieces of a total mass of 10.1 g. It is intermediate between the average values for H and L falls, $5.32 ± 0.10$ (n = 145) and $4.87 ± 0.10$ (n = 144), respectively (Rochette et al. 2003). Accordingly, saturation magnetization $M_s = 26 Am^2 kg^{-1}$ (measured on 321 mg) is low compared to that of H chondrites (average $40.5 ± 7.0 Am^2 kg^{-1}$, measured on 25 falls in Gattacceca et al. 2014) and is actually much closer to that of L chondrites (average $17.9 ± 6.1 Am^2 kg^{-1}$ measured on 31 falls). This indicates that the metal amount in the Pavel meteorite is significantly lower than that of the average H chondrite and closer to the average L content.

Olivine composition is almost equilibrated and points toward classification as H chondrite. Metal composition points to the same conclusion, with a Co (respectively Ni) content in kamacite of 0.51 wt% (respectively 6.23 wt%) similar to the $0.46 ± 0.02$ wt% (respectively $6.67 ± 0.48$ wt%) observed in H3 chondrites (Rubin 1990). However, the metal content (estimated by magnetic measurements) and the average

chondrule size are closer to that of L chondrites. Therefore, we propose classification as H3-anomalous, although a H/L3 classification could be argued (Trigo-Rodríguez et al. 2009). The olivine Fa PMD of 5.2% suggests a subtype 3.9 (Sears et al. 1980). A shock stage S5 (based on melt vein presence) may be proposed.

## CONCLUSIONS

The present overview of the meteorites fallen in Bulgaria, besides its catalog and historical interest, demonstrates that there are still “discoveries” to be made in historical collections around the world, thus validating the importance of long-term curation in natural history museums, and the efforts of curators to preserve their collections from the hazards of history. On a total of five meteorites from Bulgaria, we classified two previously unclassified meteorites (Konevo as LL5, and Silistra as ungrouped achondrite), and reclassified Pavel as H3-anomalous.

*Acknowledgments*—We thank Mrs. E. Neykova (Museum of Mineralogy, Petrology and Mineral Resources, University of Sofia), Dr. B. Zanda (Muséum national d’Histoire naturelle, Paris), and Mr. R. Bartoschewitz (Meteorite Laboratory, Gifhorn) for providing the meteorite samples for our study. We are also indebted to Drs. N. Jordanova and D. Jordanova (both from the Geophysical Institute, Bulgarian Academy of Sciences), who performed initial magnetic susceptibility measurements on the Konevo, Silistra, and Gumoschnik meteorites and thrilled our interest in this meteorite collection. This research was partly supported by a Marie Curie Intra European Fellowship (7th European Community Framework Programme; grant no. 253182, IsoBAB) to V. Dekov, which is greatly appreciated. We confirm that we have no conflict of interest to declare.

*Editorial Handling*—Dr. Adrian Brearley

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