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We have analyzed 14 impact melt glass samples, covering the compositional range from highly felsic to mafic/basaltic, as part of our effort to provide mid-infrared spectra (7–14 µm) for MERTIS (Mercury Radiometer and Thermal Infrared Spectrometer), an instrument onboard of the ESA/JAXA BepiColombo mission. Since Mercury was exposed to many impacts in its history, and impact glasses are also common on other bodies, powders of tektites (Irghizite, Libyan Desert Glass, Moldavite, Muong Nong, Thailandite) and impact glasses (from the Dellen, El'gygytgyn, Lonar, Mien, Mistastin, and Popigai impact structures) were analyzed in four size fractions of (0–25, 25–63, 93–125 and 125–250 µm) from 2.5 to 19 µm in bi-directional reflectance. The characteristic Christiansen Feature (CF) is identified between 7.3 µm (Libyan Desert Glass) and 8.2 µm (Dellen). Most samples show mid-infrared spectra typical of highly amorphous material, dominated by a strong Reststrahlen Band (RB) between 8.9 µm (Libyan Desert Glass) and 10.3 µm (Dellen). Even substantial amounts of mineral fragments hardly affect this general band shape. Comparisons of the SiO2 content representing the felsic/mafic composition of the samples with the CF shows felsic/intermediate glass and tektites forming a big group, and comparatively mafic samples a second one. An additional sign of a highly amorphous state is the lack of features at wavelengths longer than ∼15 µm. The tektites and two impact glasses, Irghizite and El'gygytgyn respectively, have much weaker water features than most of the other impact glasses. For the application in remote sensing, spectral features have to be correlated with compositional characteristics of the materials. The dominating RB in the 7–14 µm range correlates well with the SiO2 content, the Christiansen Feature shows similar dependencies. To distinguish between glass and crystalline phases of the same chemical composition, a comparison between CF the SCFM index (SiO2/(SiO2 + CaO + FeO + MgO)) ( Walter and Salisbury [1989 ] J. Geophys. Res., 94, 9203–9213) is useful, if chemical compositional data are also available.

Introduction: Mercury’s surface is exposed to a multitude of surface altering effects that have a significant influence on its optical properties. Impact events – small or large, are one of the major surface-altering agents. Inferred from hypothetical modal abundances[1] graphite can comprise up to 4wt% on Mercury’s surface. Graphite as a possible stable phase on Mercury can explain the relatively low albedo of the planet[2]. Our experimental setup probes the hypothetical impact into a graphite- and olivine–bearing, pyroxene-rich (Px(En87)=68wt%;Ol(Fo91)=29wt%,C=3wt%) surface. The effect of post-shock heating and pressure on a powder comprised of silicates with grain sizes ≤125 µm and graphite(hexagonal) was simulated in a classic shock recovery experiment[3]. The experiments were performed in the framework of the BepiColombo mission to Mercury. The onboard Mercury Radiometer and Thermal Infrared Spectrometer (MERTIS) will send thermal emissivity data once it reaches the Hermean orbit in 2025. A spectral database for mid infrared data is currently set up at the Institut für Planetologie in Münster. Published mid infrared data will soon be available and sample related spectral information of interest can be traced via assigned IDs (e.g., IDxxx). Experimental set-up and µ-FTIR: One aliquot of the prepared powder mixture served as a blank(ID467) and was not shocked, the second (ID464) aliquot was filled into an ARMCO-Fe container. The cavity (ø=16mm;depth=2mm) that held the powder was lined with tantalum foil (thickness=50 µm) in order to avoid Fe0-metal contamination from the container. Graphite foil particles vary in size (mean=500µm). The foil was cut with a razor to avoid smearing. The calculated peak pressure at the steel/sample interface reached ca. 60 GPa. Pore space was crushed upon impact and contributed to increase the post-shock temperature significantly[4]. Preliminary spectral results were obtained with a Bruker Hyperion 3000. Spectra were measured in reflectance between 3950cm-1-700cm-1. Reflectivity was calculated by measuring a gold standard equaling the sample’s surface roughness. We used a 100x100 µm2 knife edge aperture to limit obtained spectral data from defined regions of interest (ROIs) and integrated over 256 scans to improve the signal/noise ratio. Preliminary spectral results were obtained from both aliquots, ID467 and ID464. ID464 material was extracted from the steel container, from which spectral information were obtained (Fig.1bottom) and are compared to spectral data of the unshocked aliquot (Fig.1top). Figure 1 top&bottom: ID467 spectra(top). Graphite (bright material) embedded in light grey silicate matrix. Areas with indices in micrograph correlate with spectra of same numbering. Yellow highlighted rectangles are magnified for clarity, RBs are labelled and discussed in text. ID464 spectra are plotted below. Pyroxene is dominant in both aliquots. The CF is located at 1187cm-1 in ID464. Both aliquots show comparable reflectance intensities. Yellow arrows denote CO2-related adsorption in ID467. Results and discussion: We observed a dark pumice-like mass protruding perpendicular to the shockwave propagation direction. The center part of the sample shows a glassy luster (e.g.,Fig.2) which is indicative of melt formation. Figure 2: Light microscope image of graphite (dark) embedded in “fluffy”glassy matrix (arrow). Scale bar is 100 µm. ID464 compacted entirely during impact and shows a clearly distinguishable Christiansen feature (CF; a material characteristic reflectance minimum) at 1187cm-1 (similar to CF(En87)=1193cm-1. The CF of ID467 is difficult to determine. The shallowing of the adsorbed CO2-related absorption band[5] at 3677cm-1 steepens the slope towards shorter wavenumbers. Glassy material was identified in many areas. However, crystalline pyroxene surviving the impact is easily distinguished in the electromagnetic range between 1187cm-1-700cm-1, where vibrational normalmodes/or Reststrahlenbands (RBs) of silicates typically occur. RB1 of ID464 (see Fig. 1 bottom) has a shoulder at 1131cm-1, a double peak at 1103cm-1 and 1074cm-1, and another shoulder at 1043cm-1. RBs of both silicate starting materials occur in this range (En87 at 1131cm-1,1107cm-1,and 1056cm-1, and Fo91 at 1063cm-1and 1056cm-1). The envelope of the RB1 region is identical in ID464 and 467, however, a shoulder peak at 1043cm-1 missing in the unshocked, appears in the shocked aliquot and broadens the base of RB1. Pure En87 has a remarkably invariant(energy-wise) RB at 1010cm-1 (ID467) that shifted to 1006cm-1 in ID464. RB3 of the Mg-pyroxene typical “triplet-RBs” (RB3, RB4, RB5 in Fig. 1 top) at 979cm-1 is similarly invariant, however, olivine has a stable RB nearby, at 981cm-1[6]. This band is shifted to a weak shoulder at 973cm-1, either indicating the absence of olivine due to melt formation, or a shock related shift of the En87-associated RB3. Augmenting chemical analyses will help to disambiguate this. Silicate material in direct contact with graphite displays a foam like texture (Fig. 2). Graphite is an excellent thermal conductor. Silicates and graphite have a large density gradient, when shock waves traverse the individual phases, graphite-grains experience significantly higher post-shock temperatures, and thus help in melting the silicate fraction[7]. Shock-related “pumice” pressed toward the outer cylinder margins is dark and has large, entrained cavities. Future chemical and µ-FTIR analyses of the entire ID464 will improve our understanding of how graphite though chemically inert “catalyzes” processes that either not/or insufficiently take place in its absence. This work was funded by the DLR grants 50 QW 1701 and 50 QW 2201A. MERTIS group are A.N.S,A.M,H.H.,I.W.,M.P.R,K.E.B.,J.H.P.,J.H. The authors thank U.Heitmann, F.Spaleck, P.Pelka and M.Artmeier for careful sample and cylinder preparation References: [1] Vander Kaaden & McCubbin (2015), JGR: Planets, 120(2), 195-209 [2] Klima et al. (2018). Geophysical Research Letters, 45(7), 2945-2953. [3] Langenhorst & Deutsch (1994) EPSL, 125(1-4), 407-420. [4] Güldemeister et al. (2013) Meteoritics & Planetary Science, 48(1), 115-133 [5] Bianchi et al. (1994) Applied Catalysis A: General, 112(2), 219-235. [6] Stojic et al. (2021) Icarus, 357, 114162. [7] Moreau & Schwinger (2021) Physics of the Earth and Planetary Interiors, 310, 106630.

Introduction: The IRIS (Infrared and Raman for Interplanetary Spectroscopy) laboratory generates mid-infrared spectra for the ESA/JAXA BepiColombo mission to Mercury. Onboard is a mid-infrared spectrometer (MERTIS-Mercury Radiometer and Thermal Infrared Spectrometer), which will allow to map the mineralogy in the 7-14 µm range [1, 2]. In order to interpret the future data, a database of laboratory spectra is assembled at the Institut für Planetologie in Münster (IRIS) and the DLR in Berlin. So far, we have studied for this purpose natural mineral and rock samples (e.g. 3, 4), impact melt rocks (e.g. 5, 6, 7) and meteorites (e.g. 8, 9, 10, 11). Furthermore, surface processes like regolith formations and space weathering were of interest (e.g. 12, 13, 14). Synthetic analogue materials have become one of the foci of our work, since they allow to produce ‘tailor-made’ materials based on remote sensing data and/or modelling and experiments. These are closer than natural terrestrial materials, which formed usually under different conditions as expected on Mercury [e.g. 1]. We synthesized analogs for surface regions of Mercury and other planetary bodies (15, 16, 17). In this part of our study, we present mixtures based on phase equilibria of peridotite and partial melt compositions which were studied under hermean mantle conditions - temperature, pressure, oxygen fugacity (18,19,20). These experiments suggested that the crustal mineralogy should be dominated by variable abundances of plagioclase, olivine, clino- and orthopyroxene, with unconstrained proportions of silicate glass. Based on the model mineralogy of representative results, we produced mineral/glass mixtures based on the Low-Mg Northern Volcanic Plains (NVP)(Y121, Y131, Y172), High-Mg NVP (Y143, Y144), Smooth Plains (Y140, Y143, Y144), Inter crater Plain and Heavily Cratered Terrains (IcP-HCT) (Y126, Y131, Y132, Y146), and High-Mg Province (Y126, Y131, Y146) [20]. Samples and Techniques: We conducted diffuse reflectance studies of sieved size fractions (0-25 µm, 25-63 µm, 63-125 µm and 125-250 µm) under vacuum conditions, ambient heat, and variable geometries. We used a Bruker Vertex 70v with A513 variable geometry stage. The results will be made available in the IRIS Database [1]. Results: First results show the Christiansen Feature (CF), a characteristic, easy to identify reflectance low (or emission high) ranging from 7.9 µm to 8.2 µm (always average of all size fractions). The Transparency Feature (TF), typical for the finest size fraction (0-25 µm) is in many mineral mixtures less pronounced than for pure mineral phases. Here the individual TF of the components result in a broad feature. The resulting spectra can be divided into three groups – such as dominated by a single glass feature at 9.6 – 9.9 µm, a second groups with forsterite bands 9.4 µm- 9.5 µm, 10.2 µm, 10.6 µm, 11.9 µm and 15.9 µm-16 µm, and a third dominated by pyroxene bands at 8.9-9.1 µm, 9.4-9.5 µm, 9.9 µm, 10.2 µm, 10.4-10.5 µm, 10.6 µm, 10.8-11 µm 11.1-11.3 µm and 11.4-11.6 µm. Plagioclase features, even when the phase is dominating the composition, are usually ‘overprinted’ by forsterite and pyroxene bands. Discussion: A classic way to connect an easy to identify spectral feature in the mid-infrared to the chemical bulk composition is using the CF and the SiO2 content. Both show a strong correlation for both terrestrial rocks [21] and a variety of synthetic analogue samples from earlier studies in this project [15, 16, 17] (Fig.1). Summary & Conclusion: In a next step, we will study these mixtures under more realistic conditions, i.e., high vacuum and high temperature, in order to better simulate the hermean surface. Also, these mixtures will be used to test spectral unmixing routines, which allow to identify abundances of single minerals in a complex mixture of phases. References: [1] Hiesinger et al. (2020) Space Sci. rev. 216, 110 [2] Benkhoff et al. (2022) Space Sci. Rev. 217, 90 [3] Reitze et al.(2020) Min. Pet. 114, 453-463 [4] Reitze et al.(2021) EPSL 554, 116697 [5] Morlok et al.(2016) Icarus 264, 352-368 [6] Morlok et al.(2016) Icarus 278, 162-179 [7] Reitze et al.(2021) JGR (Planets) 126, e06832 [8] Weber et al. (2016) MAPS 51, 3-30 [9] Morlok et al. (2017) Icarus 284, 431-442 [10] Morlok et al. (2020) MAPS 55, 2080-2096 [11] Martin et al. (2017) MAPS 52, 1103-1124 [12] Weber et al. (2020) EPSL 530, 115884 [13] Weber et al. (2021) EPSL 569, 117072 [14] Stojic et al. (2021) Icarus 357, 114162 [15] Morlok et al. (2017) Icarus 296, 123-138 [16] Morlok et al. (2019) Icarus 324, 86-103 [17] Morlok et al. (2021) Icarus 361, 114363 [18] Charlier et al. (2013) EPSL 363, 50-60 [19] Namur et al. (2016) EPSL 439, 117-128 [20] Namur and Charlier (2017) Nature Geosci. 10, 9-13 [21] Cooper at al. (2002) JGR 107, 5017-5034 [22] Morlok et al. (2020) Icarus 335, 113410 Figure 1: Comparison of the Christiansen Feature (CF), a characteristic reflectance low, to the SiO2 bulk composition. The results from this study (red circles) fall along the regression line for terrestrial intermediate rocks.

The paper analyses literary transfer of Polish literature to the journal Merkur: Deutsche Zeitschrift für europäisches Denken. The editorial archives of Merkur for the years 1947–1978 are stored in Deutsches Literaturarchiv Marbach. This primary source enables an exploration of connections between the selection of literary translations and West German debates on the relationships be- tween politics and literature. The analysis of the archival material pertaining to Polish literature is placed in a comparative context. The article proposes a detailed matrix of questions allowing a systematic description of journal poetics based on editorial archives. These include, among others, the selection and composition of individual texts, relationships between the texts proper and paratexts, as well as connections between the general programme of the journal and the structure of individual issues. NCN, 2019/33/B/HS2/00017. 66 1 82 105 Welt der Slaven

The Mercury Radiometer and Thermal Infrared Spectrometer (MERTIS) is part of the payload on the joint ESA-JAXA BepiColombo Mission, launched in October 2018. The spectrometer is designed to map surface composition, identify rock-forming minerals, map surface mineralogy, and study surface temperature variations. The surface of Mercury undergoes large temperature variations depending on solar irradiation. Mineral spectra show significant changes in spectral features with changing temperature. In preparation of the experiment, we developed a thermal model that calculates surface temperatures based on appropriate insolation conditions and thermo-physical properties. This model has been validated with lunar parameters and hence been applied to the conditions of Mercury. Here we present surface temperature maps based on MESSENGER albedo and topography data. The results have been compared to previous models and measurements of Mercury's surface temperatures. The surface of Mercury undergoes large temperature variations each diurnal period. At the equator temperatures vary between less than 100 K during the night up to 700 K at local noon at longitudes 0° W and 180° W, and up to 570 K at longitudes 90° W and 270° W. Due to the 3:2 spin orbit resonance local noon at longitudes 0° W and 180° W coincide with perihelion, while longitudes 90° W and 270° W experience local noon at aphelion, which results in “hot” and “warm” poles around the equator. At 45° N surface temperatures at local noon reach 645 K (0° W and 180° W) and 510 K (90° W and 270° W).

Feldspars are major components of terrestrial planetary surfaces. For future space application and the setup of a comprehensive reference database, Na- and K-rich alkali feldspars, NaAlSi3O8 – KAlSi3O8, have been investigated by infrared reflectance spectroscopy. We related the feldspar spectra to the chemical composition and state of Al,Si order/disorder. The infrared measurements were analyzed with respect to band shifts and peak shapes using the autocorrelation function. Natural samples served as starting materials. Some samples were treated by the alkali exchange method to produce pure end-members, which were then heated to generate various states of Al,Si disorder. X-ray diffraction (XRD) methods served to determine the Al,Si distribution. Our autocorrelation allowed to differentiate between the compositional and the order/disorder influences seen in the spectra in the wavelength range between 7 μm up to 14 μm (1429 cm− 1 to 714 cm− 1). Space missions often analyze the surfaces of planetary bodies using remote sensing. Therefore, our results are essential to characterize and distinguish alkali feldspars on the surfaces of terrestrial planetary bodies like Mercury., Deutsches Zentrum für Luft- und Raumfahrt https://doi.org/10.13039/501100002946

Introduction: The purpose of the IRIS (Infrared and Raman for Interplanetary Spectroscopy) laboratory is to produce laboratory spectra for the mid-infrared spectrometer MERTIS (Mercury Radiometer and Thermal Infrared Spectrometer) on the ESA/JAXA BepiColombo mission to Mercury. This device will map the mineralogy of the hermean surface spectral features in the 7-14 µm range, with a spatial resolution of ~ 500 meters [1,2]. For the interpretation the data from MERTIS, we need laboratory spectra for comparison. A wide range of natural mineral and rock samples such as terrestrial impact rocks and meteorites [e.g., 3-5] was studied for this purpose. Since we do not have natural samples from surface of Mercury, we produced synthetic analogs based on MESSENGER data and laboratory experiments [6-9]. A central component for such mixtures will be glass to replicate material formed by impact events and lava extrusion and explosive volcanism (i.e., pyroclastic debris) [e.g. 10]. We present results of our ongoing study of synthetic glasses. These synthetic glasses will be studied in the mid-infrared to obtain spectra for the IRIS database, the material will also used for future mixtures and experiments. Samples and Techniques: Sample Production: In order to simulate the petrologic evolution of magmas on early Mercury, we synthesized analog material under controlled temperature, pressure and oxidation state [7-9]. The glass was produced following a procedure described in [11] with the oxidation state controlled by exposing the sample to a CO-CO2 gas-mixture equivalent to four orders of magnitude below the iron-wüstite buffer (IW-4). For in-situ studies we selected run products from earlier, similar laboratory experiments [9]. Infrared Spectroscopy: For the bulk powder FTIR diffuse reflectance analyses, powder size fractions 0-25 µm, 25-63 µm, 63-125 µm, and 125-250 µm were measured, in addition to a polished sample. We used a Bruker Vertex 70 v infrared system with a MCT detector at the IRIS laboratories at the Institut für Planetologie in Münster. Analyses were conducted under low pressure to reduce atmospheric bands, analyses were made in reflectance from 2-20 µm. FTIR microscope analyses for in-situ studies in polished blocks and thin sections were conducted using a Bruker Hyperion 1000/2000 System at the Hochschule Emden/Leer. We used a 250×250 µm sized aperture. In addition, a Perkin-Elmer Spotlight-400 FTIR spectrometer at the University of Manchester was used to map samples using an adjoining Focal Plane Array (FPA) mapping unit with a resolution of 6.25 µm × 6.25 µm. Results: Figure 1 gives an example of an area mapped using micro-FTIR. Sample 131_1 is based on the MESSENGER derived composition of the Mercurian High Magnesium Regions (HMg) [9]. Spectra in Fig.2 are of the Mg-poor (5.2 wt%) glassy component in this sample. Compared with spectra of glasses based on the Inter Crater Planes (ICP) (21.5 wt% MgO), 123_3 (17.7 wt% MgO) and 126_3 (12.2 wt% MgO), we see generally spectra typical for glassy materials. The single Reststrahlenband (RB) shifts with increasing MgO from 9.3 µm to 9.9 µm, and the CF from 7.9 µm to 8.2 µm. The two examples for bulk powders (Fig.3) have low MgO contents: 1.6 wt% (Low Mg C) and 4.7 wt % (Low Mg B) [9]. Different grain size fractions show intensity correlated with increasing grain size (Fig. 3). The RB and CF features are basically similar for all size fractions, but an characteristical Transparency Feature (TF) appears in the finest fraction (0-25 µm). The Low Mg B sample has the TF at 11.7 µm, the CF at 7.8 µm and the RB at 9.4 µm. Low-Mg C shows the CF from 7.6 µm to 7.7 µm, the RB at 9.2 µm – 9.3 µm and a TF at 11.6 µm. Summary & Conclusions: The sieved size fractions of the bulk glass material show typical features for highly crystalline materials. They follow a trend of band shifts for CF and RB towards longer wavelengths with increasing MgO contents [3,4]. We will present further glasses cover higher MgO contents (>6 wt%) to provide material for the whole range of expected Mercurian regolith glass compositions [7-9]. However, for a complete picture of the hermean surface, we expect mixtures of glassy and crystalline material. This will be the next step in our study, where we will obtain spectra of mixtures representing various regions on Mercury [e.g.7,8]. Furthermore, the impact of space weathering, which changes the structural and thus spectroscopic properties of grain surfaces will be taken into account [12,13,14]. References: [1] Rothery D.A. et al. (2020) Space Space Rev. 216, 66 [2] Hiesinger H. et al. (2020) in prep. [3] Morlok et al. (2020) Icarus 335, 113410 [4] Morlok et al. (2019) Icarus 324, 86-103 [5] Weber et al. (2020) Earth and Planetary Science Letters 530, 115884 [6] Weider S.Z. et al. (2015) Earth and Planetary Science Letters 416, 109-120 [7] Namur and Charlier (2017) Nature Geoscience 10, 9-15 [8] Namur O. et al. (2016) Earth and Planetary Science Letters 448, 102-114 [9] Namur O. et al. (2016) Earth and Planetary Science Letters 439, 117-128 [10] Fasset C.I. (2016) Journal of Geophysical Research: Planets 121, 1900-1926 [11] Renggli C. and King P. (2018) Rev.Min.Geochem 84, 229-255 [12] Weber I. et al. (2020) Earth & Planetary Science Letters 530, 115884 [13] Stojic et al. (2020) Icarus (submitted) [14] Stojic et al. (2020) LPSC 51, 1875

The imaging spectrometer MERTIS (Mercury Radiometer and Thermal Infrared Spectrometer) is part of the payload of ESA/JAXA’s BepiColombo mission, launched in 2018 [1,2]. The instrument consists of an IR-spectrometer and radiometer, which will observe the surface in the wavelength range of 7–14µm and 7–40μm, respectively. In preparation of the mission, we are investigating Mercury analog minerals at the IRIS (Infrared and Raman for Interplanetary Spectroscopy) laboratory of the Institut für Planetologie at the Westfälische Wilhelms-Universität Münster. We study typical rock-forming minerals, e.g., pyroxenes, olivines, and feldspars, as well as mineral mixtures.Here we present results of a deconvolution model used to quantify mineral specific abundances of mineral mixtures [4,5]. Planetary surfaces are composed of a variety of different minerals, therefore the obtained spectral data reflects a mixture of these minerals. In order to quantify the mineral abundances a non-linear unmixing model is necessary. Our model is based on the Hapke reflectance theory [6-8] and is applied to data obtained at the IRIS laboratory [9]. Results of olivine and pyroxene mixtures, as well as grain size mixtures, will be presented at the meeting.We used olivine (Fo91) from Dreiser Weiher, Germany, and pyroxene (En87) from Bamble, Norway and a range of mineral mixtures for IR measurements. Samples are sieved in grain size fractions of The pure pyroxene and olivine spectra clearly show characteristic Christiansen features and Reststrahlen bands for all applied geometries and increasing phase angles result in decreased intensities. The reflectance increases from pyroxene and pyroxene-rich mixtures to olivine and olivine-rich mixtures. Moreover, the olivine-rich mixtures exhibit more olivine reflectance features, compared to pyroxene-rich mixtures [11].Our studies of pyroxene grain size analysis focus on pyroxene mixtures of 50%fine/50%coarse and 30%fine/70%coarse material. Generally, the intensities increase with increasing grain sizes. The transparency feature is evident for small grain sizes and the 50%fine/50%coarse mixture.At IRIS laboratory, we will further investigate planetary analog material and their mineral mixtures applying various analytical techniques. With these data we are establishing a database that will enable the correct interpretation of MERTIS results. This work has been funded by DLR grant 50 QW 1701 in the framework of the BepiColombo mission. [1] Hiesinger H. et al. (2010) PSS58, 144-165. [2] Benkhoff J. et al. (2010) PSS58, 2-20. [3] Grumpe A. et al (2017) Icarus299, 1-14. [4] Rommel D. et al. (2017) Icarus284, 126-149. [5] Hapke B. (1981), JGR86(B4), 3039-3054. [6] Hapke B. (2002), Icarus157, 523-534. [7] Hapke B. (2012), 2ndCambr. Univ. Press., NY. [8] Bauch, K.E. et al. (2019) LPSC L, Abstract#2521. [9] Weber I. et al. (2019) LPSC L, Abstract#2326. [10] Weber, I. et al. (2020) LPSC LI, Abstract#1889.

Aubrites Peña Blanca Spring and Norton County were studied in the mid-infrared reflectance as part of a database for the MERTIS (Mercury Radiometer and Thermal Infrared Spectrometer) instrument on the ESA/JAXA BepiColombo mission to Mercury. Spectra of bulk powder size fractions from Peña Blanca Spring show enstatite Reststrahlen bands (RB) at 9 µm, 9.3 µm, 9.9 µm, 10.4 µm, and 11.6 µm. The transparency feature (TF) is at 12.7 µm, the Christiansen feature (CF) at 8.1–8.4 µm. Micro-FTIR of spots with enstatite composition in Norton County and Peña Blanca Spring shows four types: Types I and II are similar to the bulk powder spectra but vary in band shape and probably display axis orientation. Type III has characteristic strong RB at 9.2 µm, 10.4 µm, and 10.5 µm, and at 11.3 µm. Type IV is characterized by a strong RB at 10.8−11.1 µm. Types III and IV could show signs of incipient shock metamorphism. Bulk results of this study confirm earlier spectral studies of aubrites that indicate a high degree of homogeneity and probably make the results of this study representative for spectral studies of an aubrite parent body. Spectral types I and II occur in all mineralogical settings (mineral clasts, matrix, melt, fragments in melt vein), while spectral type III was only observed among the clasts, and type IV in the melt. Comparison with surface spectra of Mercury does not obtain a suitable fit, only type IV spectra from quenched impact glass show similarity, in particular the 11 µm feature. Results of this study will be available upon request or via the IRIS database (Münster) and the Berlin Emissivity Database (BED).

Mercury is an extreme planet with the largest temperature excursion in the Solar System that may affect spectral properties of the surface. Evidences suggest plagioclase, pyroxene, and olivine, with lesser amounts of quartz as possible mineralogy of Mercury’s surface. Furthermore, the presence of abundant sulfide in hollows has been proposed. Here, we measure the emissivity and reflectance of mixtures composed of a silicate and a sulfide component at different temperatures.

The thesis focuses on the developement and role of Czechoslovak advertising and promotional agency Merkur, which was the main organization for the management of the commercial and promotional activities of socialist Czechoslovakia. The aim of thesis is description of its origins, development as well as the concrete advertising campaigns to give a comprehensive picture of its existence and production. The work is divided into four main chapters. The first chapter is focused on the political and historical background of the agency's establishment. It brings important milestones in the media development and the overall social-political climate in the socialist promotion area not only during the establishment period but also throughout her existence. The second chapter is devoted to the position and characteristic of advertising in the Czechoslovak period. It describes the origin of television and radio advertising as well as the advertising agencies in Czechoslovakia, with an emphasis on foreign trade agency Rapid, which played an important role in Merkur's work. The penultimate part of the thesis deals with the origins and development of Merkur itself, the subject of its activity, its employment base and its structure. The final chapter describes the promotional tools used by the company and analyzes...