Raman spectroscopy has been applied to study a range of chromites (Fe2+, Mg)(Cr, Al, Fe3+)2O4 with variable chromium to aluminum to iron contents to ascertain conclusions about possible correlations between the chromium concentration and the position of the main Raman peaks within this mineral. Our intention was to examine chromite grains from different paragenesis, which vary significantly in their chromium content, to observe changes in the Raman spectra of this mineral. It was found that a negative correlation exists between the chromium number, calculated from the electron microprobe data, and the Raman peak number. Chromite grains with high chromium numbers show a low Raman peak, whereas samples with low chromium number show a higher Raman peak. Therefore, it is possible to infer a relationship between the mineral composition and Raman bands for this type of spinel. The measurements have clearly shown that it is possible to draw precise conclusions about the chromium content of the mineral based on the Raman peak alone. This finding supports a possible application of portable Raman devices on Earth or in space for asteroids and planets.

The Saricicek howardite meteorite shower consisting of 343 documented stones occurred on September 2, 2015 in Turkey and is the first documented howardite fall. Cosmogenic isotopes show that Saricicek experienced a complex cosmic-ray exposure history, exposed during 12-14Ma in a regolith near the surface of a parent asteroid, and that an 1m sized meteoroid was launched by an impact 22 +/- 2Ma ago to Earth (as did one-third of all HED meteorites). SIMS dating of zircon and baddeleyite yielded 4550.4 +/- 2.5Ma and 4553 +/- 8.8Ma crystallization ages for the basaltic magma clasts. The apatite U-Pb age of 4525 +/- 17Ma, K-Ar age of 3.9Ga, and the U,Th-He ages of 1.8 +/- 0.7 and 2.6 +/- 0.3Ga are interpreted to represent thermal metamorphic and impact-related resetting ages, respectively. Petrographic; geochemical; and O-, Cr-, and Ti-isotopic studies confirm that Saricicek belongs to the normal clan of HED meteorites. Petrographic observations and analysis of organic material indicate a small portion of carbonaceous chondrite material in the Saricicek regolith and organic contamination of the meteorite after a few days on soil. Video observations of the fall show an atmospheric entry at 17.3 +/- 0.8kms(-1) from NW; fragmentations at 37, 33, 31, and 27km altitude; and provide a pre-atmospheric orbit that is the first dynamical link between the normal HED meteorite clan and the inner Main Belt. Spectral data indicate the similarity of Saricicek with the Vesta asteroid family (V-class) spectra, a group of asteroids stretching to delivery resonances, which includes (4) Vesta. Dynamical modeling of meteoroid delivery to Earth shows that the complete disruption of a 1km sized Vesta family asteroid or a 10km sized impact crater on Vesta is required to provide sufficient meteoroids 4m in size to account for the influx of meteorites from this HED clan. The 16.7km diameter Antionia impact crater on Vesta was formed on terrain of the same age as given by the He-4 retention age of Saricicek. Lunar scaling for crater production to crater counts of its ejecta blanket show it was formed 22Ma ago.

On March 6, 2016 at 21:36:51 UT , extended areas of Upper Austria, Bavaria (Germany) and the southwestern part of the Czech Republic were illuminated by a very bright bolide. This bolide was recorded by instruments in the Czech part of the European Fireball Network and it enabled complex and precise description of this event including prediction of the impact area. So far six meteorites totaling 1473 g have been found in the predicted area. The first pieces were recovered on March 12, 2016 on a field close to the village of Stubenberg (Bavaria). Stubenberg is a weakly shocked (S3) fragmental breccia consisting of abundant highly recrystallized rock fragments embedded in a clastic matrix. The texture, the large grain size of plagioclase, and the homogeneous compositions of olivine (Fa 31.4 ) and pyroxene (Fs 25.4 ) clearly indicate that Stubenberg is an LL 6 chondrite breccia. This is consistent with the data on O, Ti, and Cr isotopes. Stubenberg does not contain solar wind‐implanted noble gases. Data on the bulk chemistry, IR spectroscopy, cosmogenic nuclides, and organic components also indicate similarities to other metamorphosed LL chondrites. Noble gas studies reveal that the meteorite has a cosmic ray exposure ( CRE ) age of 36 ± 3 Ma and that most of the cosmogenic gases were produced in a meteoroid with a radius of at least 35 cm. This is larger than the size of the meteoroid which entered the Earth's atmosphere, which is constrained to <20 cm from short‐lived radionuclide data. In combination, this might suggest a complex exposure history for Stubenberg.

JAXA Hayabusa mission success-fully returned particles of the asteroid Itokawa to the earth in 2010. The recovered particles were carefully studied by the preliminary examination (PE) team and the obtained results are providing significant and unique information about the formation and evolution of meteorite parent bodies [1-6]. These particles further revealed that their mineral compositions and oxygen isotopes are close to those of equilibrated LL chon-drites [1,2], which matches with the observation at the orbit [7]. After the PE, JAXA distributed the samples as international AO study and we received 4 new and 3 PE particles. The new samples may contain some exot-ic components that have not been found by the PE study, and are of special interest. We have performed a detailed mineralogical and crystallographic study on these particles and here report the results.

We studied seven Itokawa particles provided by the Japan Aerospace Exploration Agency (JAXA) as first International Announcement of Opportunity (AO) study mainly using electron and synchrotron radiation X-ray beam techniques. All the analyzed particles were collected from the first-touchdown site and composed of olivine and plagioclase with traces of Ca phosphate and chromite, and do not contain pyroxenes. Optical microscopy of these particles shows minor undulatory extinction of olivine and plagioclase, suggesting minor shock metamorphism (shock stage: S2). The electron microprobe analysis shows that olivine is Fo70-73 and plagioclase is An13-10Or5-7. The synchrotron radiation X-ray diffraction (SR-XRD) analysis of olivine crystals gives cell dimensions of a = 4.708 to 4.779 Å, b = 10.271 to 10.289 Å, c = 6.017 to 6.024 Å, corresponding to the Fo content of Fo~70 by Vegard's law. This composition matches the result obtained by the electron microprobe analysis. The olivine compositions of the analyzed particles are consistent with those of LL chondrites. The cell dimensions of two plagioclase crystals (a = 8.180 to 8.194 Å, b = 12.53 to 12.893 Å, c = 7.125 to 7.23 Å, α = 92.6° to 93.00°, β = 116.36° to 116.75°, γ = 90.03° to 90.17°) indicate that their equilibration temperatures are 800°C ± 10°C. This temperature is near the peak metamorphic temperature recorded by equilibrated ordinary chondrites. The size of plagioclase crystals and the homogeneity of olivine compositions indicate that their petrologic type is ≥5. We also analyzed plagioclase by SR iron X-ray absorption near-edge structure (SR-XANES) and found that its Fe3+/(Fe2+ + Fe3+) ratio is approximately 0.5. Such high Fe3+ abundance indicates the formation under a relatively oxidizing environment. Thus, all these analyses have reconfirmed that the Itokawa particles returned by the Hayabusa spacecraft are very weakly shocked equilibrated LL chondrites, which matches the results of the preliminary examination team.

The Almahata Sitta meteorite is the first case of recovered extraterrestrial material originating from an asteroid that was detected in near Earth space shortly before entering and exploding in the high atmosphere. The aims of our project within the 2008 TC3 consortium were investigating Almahata Sitta's (AS) magnetic signature, phase composition and mineralogy, focussing on the opaque minerals, and gaining new insights into the magnetism of the ureilite parent body (UPB). We report on the general magnetic properties and behavior of Almahata Sitta and try to place the results in context with the existing data set on ureilites and ureilite parent body models. The magnetic signature of AS is dominated by a set of low-Ni kamacites with large grain sizes. Additional contributions come from micron-sized kamacites, suessite, (Cr) troilite, and daubreelite, mainly found in the olivine grains adjacent to carbon-rich veins. Our results show that the paleomagnetic signal is of extraterrestrial origin as can be seen by comparing with laboratory produced magnetic records (IRM). Four types of kamacite (I-IV) have been recognized in the sample. The elemental composition of the ureilite vein metal Kamacite I (particularly Co) clearly differs from the other kamacites (II-IV), which are considered to be indigenous. Element ratios of kamacite I indicate that it was introduced into the UPB by an impactor, supporting the conclusions of Gabriel and Pack (2009).

Mikouchi 1 , C. A. Goodrich 2 , V. Hoffmann 3,4 , W. Satake 1 , M. Kaliwoda 4,5 , R. Hochleitner 4,5 , A. M. Gigler 4,5 , K. Sugiyama 6 , and M. E. Zolensky 7 , 1 Dept. of Earth and Planet. Sci., University of Tokyo, Hongo, Bunkyo-ku, Tokyo 113-0033, Japan (mikouchi@eps.s.u-tokyo.ac.jp), 2 Planet. Sci. Inst., Tucson, AZ 85719, USA, 3 Dept. of Geosci., University of Tübingen, 72076 Tübingen, Germany, 4 Dept. of Earth and Envir. Sci., University of München, 80333 München, Germany, 5 Mineral. State Collection, 80333 München, Germany, 6 Inst. for Materials Res., Tohoku University, Aoba-ku, Sendai, Miyagi 980-0812, Japan, 7 ARES, NASA Johnson Space Center, Houston, TX 77058, USA.

Raman spectroscopy is a convenient method to classify polytypes plus polymorphs and to investigate different compositions, structures, and modifications of minerals. This information is required to classify meteorites of different mineral compositions. Our intention was to examine different graphite modifications and to determine the opaque phases within the Almahatta Sitta (AS) meteorite. Our investigation focused on specimens AS39 and AS4. Both are multicomponent breccias, composed of different meteoritic lithologies, that is, anomalous polymict ureilite material, different types of chondrites, and an iron meteorite.[ 1-5 ] The mix of material implicates a crash of variable asteroids within time and space. This means that a primary ureilitic asteroid body has been the target of multiple meteorite or asteroid impacts, which did not completely destroy the asteroid but added new material (from chondritic to iron) to the main mass. For instance, Gabriel and Pack[ 6 ] suggested that the vein metal of monomict ureilites is introduced by the impact of a Ni-poor iron meteorite in a similar scenario as described above. Raman spectroscopy helped to investigate different carbon materials, that is, graphite and diamond. We used single-spectrum acquisition and spatial mappings to identify the different modifications. Furthermore, we classified minor opaque phases such as schreibersite, suessite, daubreelite, cohenite, and kamacite. The investigation of these opaque phases is dealt with in further papers.[1,2]

(1) Section Crystallography, LMU-München, Theresienstr. 41, 80333 Munich, Germany, (2) CeNS, LMU-München, Schellingstr. 4, 80799 Munich, Germany, (3) Mineralogical State Collection, Theresienstr. 41, 80333 Munich, Germany, (4) Earth and Planetary Science, Graduate School of Science, University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan, (5) Geophysics, LMU-München, Theresienstr. 41, 80333 Munich, Germany

Detailed magnetic study on vegetation samples from several strongly polluted and clean sites in Bulgaria is carried out in order to evaluate suitability of different species as passive dust collectors in magnetometry. From each location, available species among lichens, mosses, poplar leaves, dandelion, needles have been sampled. Magnetic susceptibility calculated on mass-specific basis shows wide variability between diamagnetic signal up to 846 × 10 −8 m 3 /kg. Lichens and mosses are found to be the species, showing magnetic signals with the strongest contrast between clean and polluted environment. The main magnetic phase is magnetite-like according to the results from thermomagnetic analysis of susceptibility on magnetic extracts. Scanning electron microscopy (SEM) microphotographs reveal the presence of abundant particulate matter on vegetation surface both with anthropogenic (spherules) and lithogenic origin. Magnetic grain size deduced by the ratio of saturation remanent magnetization (SIRM) and mass-specific magnetic susceptibility (χ) and coercivities (B c and B cr ) suggest that different species accumulate preferentially small SD-like grains from pollution emissions. Contrasting relationship of the ratio of anhysteretic remanent magnetization (ARM) and χ for polluted vs clean sites deduced by needles and lichens may be related to transformation of the accumulated dust particles within lichens’ tissue. This finding indicates that the exact species used as biological dust collector is of importance when studying spatial grain size distribution of magnetic dust particles. Pilot study on polycyclic aromatic hydrocarbons (PAH) content and its relation to magnetic parameters shows good correspondence between high levels of PAHs and high SIRM values for locations affected by non-ferrous industrial production.

Poster Workshop Asteroid 2008TC3. [6] Rochette P., et al. 2009. Meteoritics Planet. Science, 44: 405-427. [7] Sugiura N., Strangway D.W., 1988. In: Kerridge J.F., Matthews M.S., Meteorites and the early Solar System. Univ. Arizona Press, Tucson, 595615. [8] Gattacceca J., et al., 2008. Earth Planet. Sci. Lett. 270: 280-289. [9] Kohout T., et al., 2007. Earth Planet. Science Lett.: 261: 143-151. [10] Steele A., et al., 2009. Characterisation of Diamond in the Almahata Sitta meteorite. DPS conference abstract. [11] Goodrich C.A., 1992. Meteoritics 27: 327-352. [12] Rowe M.W., et al., 1976. NASA Report CR-1411-43, N75-146. [13] Gabriel A.D., Pack A., 2009. 40 Lunar Planetary Science Conference, # 2462. [14] Goodrich C.A., 2009. 40 Lunar Planetary Science Conference, # 1132. 2120.pdf 41st Lunar and Planetary Science Conference (2010)

Introduction: New discoveries in cold (Antarctica) and hot desert areas have significantly increased the number of Martian meteorites (SNC) to more than 50 (unpaired) [1,2]. Martian meteorites are classified in four main groups in terms of their pe-trology and mineralogy, namely Orthopyroxenite (1 published member), Chassignites (dunite, 2), Nakhlites (clinopyroxenite, 7) and Shergottites (42) which are additionally subdivided in basal-tic, olivine-phyric, olivine-opx phyric, lherzolitic and one wehrlite [1]. Magnetism of shergottites: Recently, geochemical studies revealed that independently from the " old " scheme shergottites can be divided into 3 different subgroups based on their trace element and isotopic signature (enriched, depleted, and intermediate suite) [3]. This is interpreted as additionally reflecting the heterogeneity of the magma reservoirs [4]. The petrology and mineralogy of the lherzolitic shergottites is quite homogeneous (neglecting secondary processes) [5,6]. Their magnetic signature was found to follow specific trends, mainly depending on shock degree and terrestrial alteration effects, the latter in turn strongly depending on size/weight (TKW) of the individual Martian meteorites [7-9]. However, the magnetic signature of the members of the other shergottite groups appears quite scattered and was not found to follow distinct trends so far. In this study, we tried to (re-) compile published and original data, specifically addressing and incorporating new shergottite finds, concerning their magnetic signature in order to evaluate likely trends or groupings (such as for lherzolites). Additionally, the effects of secondary processes such as terrestrial alteration on the magnetic characteristics of the SNC were studied using the NWA 2975 (basaltic), SaU 005/008 and NWA 1068 (oliv.-phyric) and DaG 476 (oliv.-opx phyric) clans representing large sets of sample sizes and weights (TKW). The main result of our investigations is that only sufficiantly large sample sets and the respective databases allow to get insight and to eventually control these secondary processes in a satisfying manner.

The substantial amounts of iron taken up by plants give rise to unstimulated formation of iron oxide particles inside their photosynthetic organs which, given the presence of ample reductants such as glucose. contain Fe(II) and thus are ferro(or ferri-)magnetic (magnetite Fe3O4). Besides this, other (heavy and light) metals are absorbed by plants both from aerosol deposited on leaves and via the roots. Since the uptake rates of different metals are linked by biochemical factors, it should be feasible to correlate magnetic signals from leaves/needles which are due to magnetite to the burden of other, toxic heavy metals. If this be proven, there are ramifications for biomonitoring escaping the need and expenses of traditional analytics. In this paper, thermodynamic and biochemical (bioinorganic) requirements for magnetite formation and doing this kind of biomonitoring are discussed.1 If given in sufficiently high doses, all heavy metals (HM) are toxic of course, but THM referred to those which are hazardous when given in small amounts. but over a longer period of time. E.g. for being neurotoxic.2 Bidentate ligands bind to one single metal ion via two different atoms.3 Effect or impact indicators/monitors are organisms that demonstrate specific or unspecific effects in response to exposure to a certain element or compound or a number of substances (MARKERT, 2008).4 It is important to note, that all considerations given in this paper are made under the assumption, that the magnetic signal of the vegetation species originate from the magnetic-like phases formed inside the plant tissues. However we used in recently published studies (JORDANOVA et al., 2008, 2009) non-washed material. which means, that the largest contribution of the magnetic signal derives from dust particles, which are mechanically attached to the surface of the plant investigated. Therefore, an unwashed plant can be handled as a "dust collector" of atmospheric fallout measurements.

Yamato 000593, a nakhlite, was analyzed in terms of its magnetic record and magnetomineralogy. The natural remanent magnetization (NRM: 3.55-6.07 x 10(-5) Am(2)/kg) was thermally demagnetized at similar to 320 degrees C, and it was unstable against alternating field demagnetization. Based on analyses of thermomagnetic Curves, the temperature dependence of hysteresis parameters, and microscopic observations, the magnetic minerals mainly consist of magnetite (0.68 wt% of the sample, including similar to 5% Fe(2)TiO(4)) of less than 100 mu m in size, associated with minor amounts of monoclinic pyrrhotite (<0.069 wt% of the sample) and goethite. Thermal demagnetization of NRM at similar to 330 degrees C is explained due to an offset of magnetization of antipodal NRM components of magnetite, whereas it is not due to a pyrrhotite Curie point. Large magnetite grains show exsolution texture With ilmenite laths, and are Cut by silicate (including goethite) veins that formed along cracks. Numerous single-domain (SD) and pseudo-single-domain (PSD) magnetite grains are scattered in the mesostasis and adjacent olivine grains. Moderate coercive forces of H(C) = 6.8 mT and H(RC) = 31.1 mT Suggest that Yamato 000593 is fundamentally able to carry a stable NRM; however, NRM was found to be unstable. Accordingly, the meteorite was possibly crystallized at 1.3 Ga under an extremely weak or absent magnetic Field, or was demagnetized by impact shock at 12 Ma (ejection age) on Mars. This finding differs from the results Of previous paleomagnetic Studies of SNC (shergottites, nakhlites, chassignites, and orthopyroxenite) Martian meteorites. The significant dipole magnetic field resulting from the molten metallic core was probably absent during the Amazonian Epoch (after 1.8 Ga) on Mars.