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  • Lunar and Planetary Science and Exploration  (6)
  • Geophysics  (5)
  • X-ray structure determination  (2)
  • 2015-2019  (7)
  • 2010-2014  (4)
  • 1990-1994  (2)
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  • 1
    Electronic Resource
    Electronic Resource
    Weinheim : Wiley-Blackwell
    Zeitschrift für anorganische Chemie 608 (1992), S. 33-42 
    ISSN: 0044-2313
    Keywords: Diacylphosphines ; Di-cyclohexoylposphine ; Diadamant-1-oylphosphine ; keto-enol tautomerism ; NMR-parameters, thermodynamic data ; X-ray structure determination ; very short O‥H‥O bridge ; Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Description / Table of Contents: Acyl- and Alkylidenephosphines. XXXII. Di-cyclohexoyl- and Diadamant-1-oylphosphine - Keto-Enol Tautomerism and StructureLithium dihydrogenphosphide · DME (1) [12] and cyclo-hexoyl or adamant-1-oyl chloride react in a molar ratio of 3:2 to give lithium di-cyclo-hexoylphosphide · DME and the corresponding diadamant-1-oylphosphide.2THF (1) resp. Treatment of these two compounds with 85% tetrafluoroboric acid. diethylether adduct yields di-cyclo-hexoyl- (1b) and diadamant-1-oylphosphine (1c). In nmr spectroscopic studies 1b over a range of 203 to 343 K, a strong temperature dependence of the keto-enol equilibrium is found; thermodynamic data characteristic for the formation of the enol tautomer (ΔH0 = -4.3 kJ. mol-1; ΔS0 = -9.2 J. mol-1. K (-1) are compared of 1,3-diketones.The enol tautomer of diadamant-1-oylphosphine (E-1c) as obtained from a benzene solution in thin colourless plates, crystallizes in the monoclinic space group P21/c {a = 722.2(2); b = 1085.5(4); c = 2434.8(5) pm; ß = 96.43(2)° at -100 ± 3°C; Z = 4}. An X- ray structure analysis (Rw = 0.033) shows bond lengths and angles to be almost identical within the enolic system (P—C 179/180; C—O 130/129; C—C(adamant-1-yl) 152/153 pm; C—P—C 99°; P—C—O 124°/124°; P—C—C 120°/120°; C—C—O 116°/116°. The geometry of the very strong, but probably asymmetric O‥H‥O bridge is discussed (O—H 120/130, O‥O 245 pm).
    Notes: Aus Lithium-dihydrogenphosphid · DME (1) [12] und cyclo-Hexoyl- bzw. Adamant-1-oyl-chlorid im Molverhältnis 3:2 zugängliches Lithium-di-cyclo-hexoylphosphid · DME und -diadamant-1-oylphosphid · 2THF 1) reagieren mit 85proz. Tetrafluoroborsäure · Diethylether-Addukt zu Di-cyclo-hexoyl- 1b) und Diadamant-1-oylphosphan (1 c). Die Lage des Keto-Enol-Gleichgewichts zwischen 203 und 343 K sowie thermodynamische Daten zur Bildung des Enol-Isomers ΔH0= -4,3kJ.Mol-1; ΔS0;=-9,2 J · mol-1 · K-1 () wurden NMR-spektroskopisch an einer 2 M Lösung des bei +20°C flüssigen Di-cyclo-Hexoyl-Derivates 1b in d8-Toluol ermittelt und mit Werten von 1,3-Diketonen verglichen.Das farblose, sich aus Benzol in dünnen Plättchen abscheidende Enol-Tautomer des Diadamant-1-oylphosphans (E-1 c) kristallisiert monoklin in der Raumgruppe P21/c {a = 722,2(2) b = 1085,5(4); c = 2434,8(5) pm; ß = 96,43(2)° bei - 100 ± 3°C; Z = 4}. Nach den Ergebnissen der Röntgenstrukturanalyse (Rw=0,033) weist das Molekül in beiden des Hälften des Enolrings nahezu identische Bindungslängen und -winkel auf P—C 179/180; C—O 130/129; C—C(Adamant-1-yl) 152/153 pm; C—P—C 99°; P—C—O 124°/124°; P—C—C 120°/120°; C—C—O 116°/116°. Die Geometrie der sehr starken, aber vermutlich asymmetrischen O‥H‥O-Brücke wird diskutiert (O—H 120/130; O‥O 245 pm).
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  • 2
    ISSN: 0044-2313
    Keywords: Lithium bis(2,2-dimethylpropionl)arsenide · DME ; tetrakis(2,2-dimethylpropionyl)diarsine ; X-ray structure determination ; Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Description / Table of Contents: Acyl- and Alkylidenearsines VII Synthesis and Structure of Tetrakis(2,2-dimethylpropionyl)diarsineLithium dihydrogenarsenide and 2,2-dimethylpropionyl chloride in a molar ratio of 3:2 react at -40 to -50°C in tetrahydrofuran or 1,2-dimethoxyethane to give the corresponding etherate of lithium bis(2,2-dimethylpropionyl)arsenide (2a). Treatment of these solutions with stoichiometric amounts of 85% tetrafluoroboric acid · diethylether adduct yields yelloworange tetrakis(2,2-dimethylpropionyl)diarsine (5) in 64 or 62% yield resp., but not the expected bis (2,2-dimethylpropionyl)arsine (4a). The very air-sensitive compound crystallizes in the monoclinic space group P21/n {-100 ± 3° C; a = 1224.6(3); b = 1419.7(3); c = 1333.1(3) pm; β = 96.22(2)°; Z = 4}. According to the X-ray structure analysis (Rw = 0.036) the molecule shows synclinal conformation; the two diacylarsyl-subunits are twisted against one another by an angle of 86°. As in another acylarsine [1] the As—C distances (203 to 205 pm) were found to be significantly longer then the standard value of 196 pm. Further characteristic bond lengths and angles are: As- 242; C—O 120 to 121 pm; As—As—C 88 to 107°; As—C—O 118 to 122°
    Notes: Wird das jeweilige, aus Lithiumdihydrogenarsenid und 2,2-Dimethylpropionylchlorid im Molverhältnis 3:2 bei -40 bis -50°C in TetrahydrofuranTetrahydrofuran (THF); 1,2-Dimethoxyethan (DME); Bis( 1,2-dimethylamino)ethan (TMEDA); Tetramethylsilan (TMS). oder 1,2-Dimethoxyethan gebildete, aber nicht isolierte Etherat des Lithium-bis(2,2-dimethypropionyl)arsenids (2a) mit 85proz. Tetrafluorborsäure · Diethylether-Addukt weiter umgesetzt, so erhält man nach der üblichen Aufarbeitung des Ansatzes nicht Bis(2,2-dimethylpropionyl)arsan (4a), sondern mit 64- bzw. 62proz.Ausbeute Tetrakis(2,2-dimethylpropionyl)diarsan (5). Die äußerst oxydationsempfindliche gelborange Verbindung kristallisiert monoklin in der Raumgruppe P21/n {-100 ± 3° C; a = 1224,6(3); b = 1419,7(3); c = 1333,1(3)pm; β = 96,22(2)°; Z = 4}. Nach den Ergebnissen der Röntgenstrukturanalyse (Rw = 0,036) weist das Molekül mit zwei um 86° gegeneinander verdrehten Hälften die synclinale Konformation auf; die As—C-Abstände liegen mit 203 bis 205 pm wie in einem anderen Acylarsan [1] deutlich über dem Standard von 196 pm. Weitere Charakteristische Bindungslängen und -winkel sind: As—As242; C—O 120 bis 121 pm; As—As—C 88 bis 107°; As—C—O 118 bis 122°.
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  • 3
    Publication Date: 2014-11-22
    Description: The Rocknest aeolian deposit is similar to aeolian features analyzed by the Mars Exploration Rovers (MER) Spirit and Opportunity. The fraction of sand 〈150 micron in size contains approx. 55% crystalline material consistent with a basaltic heritage, and approx. 45% X-ray amorphous material. The amorphous component of Rocknest is Fe-rich and Si-poor, and is the host of the volatiles (H2O, O2, SO2, CO2, and Cl) detected by the Surface Analysis at Mars (SAM) instrument and of the fine-grained nanophase oxide (npOx) component first described from basaltic soils analyzed by MER. The similarity between soils and aeolian materials analyzed at Gusev crater, Meridiani Planum and Gale crater implies locally sourced, globally similar basaltic materials, or globally and regionally sourced basaltic components deposited locally at all three locations.
    Keywords: Lunar and Planetary Science and Exploration
    Type: ARC-E-DAA-TN11260
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  • 4
    Publication Date: 2019-07-13
    Description: Rocks enriched in Ge have been discovered in Gale Crater, Mars, by the Alpha-particle X-ray spectrometer (APXS) on the Mars Science Lab (MSL) rover, Curiosity. The Ge concentrations in Gale Crater (commonly 〉50 ppm) are remarkably high in comparison to Earth, where Ge ranges from 0.5-4.0 ppm in igneous rocks and 0.2-3.3 ppm in siliciclastic sediment. Primary meteoritic input is not likely the source of high Ge because Ge/Ni in chondrites (approx.0.003) and irons (〈0.04) is lower than in Gale rocks (0.08-0.2). Earth studies show Ge is a useful geochemical tracer because it is coherent with Si during magmatic processes and Ge/Si varies less than 20% in basalts. Ge and Si fractionate during soil/regolith weathering, with Ge preferentially sequestered in clays. Ge is also concentrated in Cu- and Zn-rich hydrothermal sulfide deposits and Fe- and Mnrich oxide deposits. Other fluid-mobile elements (K, Zn, Cl, Br, S) are also enriched at Gale and further constrain aqueous alteration processes. Here, we interpret the sediment alteration history and present a possible model for Ge enrichments at Gale involving fluid alteration of the protolith.
    Keywords: Geophysics
    Type: JSC-CN-32857 , Lunar and Planetary Science Conference; Mar 16, 2015 - Mar 20, 2015; The Woodlands, TX; United States
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  • 5
    Publication Date: 2019-07-13
    Description: MSL Curiosity investigated the Windjana sandstone outcrop, in the Kimberley area of Gale Crater, and obtained mineralogical analyses with the CheMin XRD instrument. Windjana is remarkable in containing an abundance of potassium feldspar (and thus K in its bulk chemistry) combined with a low abundance of plagioclase (and low Na/K in its chemistry). The source of this enrichment in K is not clear, but has significant implications for the geology of Gale Crater and of Mars. The high K could be intrinsic to the sediment and imply that the sediment source area (Gale Crater rim) includes K-rich basalts and possibly more evolved rocks derived from alkaline magmas. Alternatively, the high K could be diagenetic and imply that the Gale Crater sediments were altered by K-rich aqueous fluids after deposition.
    Keywords: Geophysics
    Type: JSC-CN-32824 , Lunar and Planetary Science Conference; Mar 16, 2015 - Mar 20, 2015; The Woodlands, TX; United States
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  • 6
    Publication Date: 2019-07-13
    Description: The Mars rover Curiosity has encountered silica-enriched bedrock (as strata and as veins and associated halos of alteration) in the largely basaltic Murray Fm. of Mt. Sharp in Gale Crater. Alpha Particle X-ray Spectrometer (APXS) investigations of the Murray Fm. revealed decreasing Mg, Ca, Mn, Fe, and Al, and higher S, as silica increased (Fig. 1). A positive correlation between SiO2 and TiO2 (up to 74.4 and 1.7 wt %, respectively) suggests that these two insoluble elements were retained while acidic fluids leached more soluble elements. Other evidence also supports a silica-retaining, acidic alteration model for the Murray Fm., including low trace element abundances consistent with leaching, and the presence of opaline silica and jarosite determined by CheMin. Phosphate stability is a key component of this model because PO4 3- is typically soluble in acidic water and is likely a mobile ion in diagenetic fluids (pH less than 5). However, the Murray rocks are not leached of P; they have variable P2O5 (Fig. 1) ranging from average Mars (0.9 wt%) up to the highest values in Gale Crater (2.5 wt%). Here we evaluate APXS measurements of Murray Fm. bedrock and veins with respect to phosphate stability in acidic fluids as a test of the acidic alteration model for the Lower Mt. Sharp rocks.
    Keywords: Lunar and Planetary Science and Exploration
    Type: JSC-CN-35224 , Lunar and Planetary Science Conference; Mar 21, 2016 - Mar 25, 2016; The Woodlands, TX; United States
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  • 7
    Publication Date: 2019-07-13
    Description: The eolian bedform within Gale Crater referred to as "Rocknest" was investigated by the science instruments of the Curiosity Mars rover. Physical, chemical and mineralogical results are consistent with data collected from soils at other landing sites, suggesting a globally-similar composition. Results from the Curiosity payload from Rocknest should be considered relevant beyond a single, localized region with Gale Crater, providing key insights into planetary scale processes.
    Keywords: Geophysics
    Type: JSC-CN-27936 , Lunar and Planetary Science Conference; Mar 18, 2013 - Mar 22, 2013; The Woodlands, TX; United States
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  • 8
    Publication Date: 2019-07-13
    Description: A significant portion of the soil of the Rocknest dune is crystalline and is consistent with derivation from unweathered basalt. Minerals and their compositions are identified by X-ray diffraction (XRD) data from the CheMin instrument on MSL Curiosity. Basalt minerals in the soil include plagioclase, olivine, low- and high-calcium pyroxenes, magnetite, ilmenite, and quartz. The only minerals unlikely to have formed in an unaltered basalt are hematite and anhydrite. The mineral proportions and compositions of the Rocknest soil are nearly identical to those of the Adirondack-class basalts of Gusev Crater, Mars, inferred from their bulk composition as analyzed by the MER Spirit rover.
    Keywords: Geophysics
    Type: JSC-CN-27905 , 44th Lunar and Planetary Science Conference; Mar 18, 2013 - Mar 22, 2013; The Woodlands, TX; United States
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  • 9
    Publication Date: 2019-07-13
    Description: The Alpha Particle X-ray spectrometer (APXS) on the Curiosity rover in Gale Crater [1] is the 4th such instrument to have landed on Mars [2]. Along the rover's traverse down-section toward Glenelg (through sol 102), the APXS has examined four rocks and one soil [3]. Gale rocks are geochemically diverse and expand the range of Martian rock compositions to include high volatile and alkali contents (up to 3.0 wt% K2O) with high Fe and Mn (up to 29.2% FeO*).
    Keywords: Lunar and Planetary Science and Exploration
    Type: JSC-CN-27938 , Lunar and Planetary Science Conference; Mar 18, 2013 - Mar 22, 2013; TheWoodlands, TX; United States
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  • 10
    Publication Date: 2019-07-30
    Description: Characterizing the history of aqueous activity at the martian surface has been an objective of the Mars Exploration Rovers (MER) and the Mars Science Laboratory (MSL). Although the geologic context of the three landing sites are different, comparisons across the datasets can provide greater insight than using data from one mission alone. The Alpha Particle X-ray Spectrometer (APXS) is common to all three rovers (Spirit at Gusev crater, Opportunity at Meridiani Planum, and Curiosity at Gale crater) and provides a consistent basis for these comparisons. Soil and Dust: Fine grained basaltic soils and dust are remarkably uniform in chemical composition across multiple landing sites. These similarities in the concentrations of major, minor, and a few trace elements (Fig. 1) are indicative of planet-wide consistency in the composition of source materials for the soils. S and Cl vary by a factor of two in the soil and dust, but there is no clear association with any bulk cation (e.g., no correlation between S and total Ca, Mg, or Fe in soils). These volatile elements, however, are clearly associated with the nanophase-ferric iron component in the soil established by Mssbauer spectroscopy [1,2]. S and Cl likely originated as acidic species from volcanic out-gassing and subsequently coalesced on dust and sand grain surfaces, possibly with an affinity towards Fe3+ sites. Importantly, given the mobility of S and Cl in aqueous exposures, soil samples maintaining the typical molar S/Cl ratio of ~3.7:1 indicate minimal interactions with liquid water after the addition of S and Cl. In contrast to this well-established baseline, soil samples have been discovered at all three landing sites with atypical S/Cl ratios (e.g., subsurface soils), indicative of a more complex aqueous history.
    Keywords: Lunar and Planetary Science and Exploration
    Type: JSC-E-DAA-TN70395 , International Conference on Mars; Jul 22, 2019 - Jul 25, 2019; Pasadena, CA; United States
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