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  • 1
    Electronic Resource
    Electronic Resource
    Copenhagen : International Union of Crystallography (IUCr)
    Acta crystallographica 35 (1979), S. 402-404 
    ISSN: 1600-5740
    Source: Crystallography Journals Online : IUCR Backfile Archive 1948-2001
    Topics: Chemistry and Pharmacology , Geosciences , Physics
    Type of Medium: Electronic Resource
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  • 2
    Electronic Resource
    Electronic Resource
    Copenhagen : International Union of Crystallography (IUCr)
    Acta crystallographica 29 (1973), S. 2029-2031 
    ISSN: 1600-5740
    Source: Crystallography Journals Online : IUCR Backfile Archive 1948-2001
    Topics: Chemistry and Pharmacology , Geosciences , Physics
    Type of Medium: Electronic Resource
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  • 3
    Electronic Resource
    Electronic Resource
    Weinheim : Wiley-Blackwell
    Zeitschrift für anorganische Chemie 420 (1976), S. 31-39 
    ISSN: 0044-2313
    Keywords: Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Description / Table of Contents: Preparation, Crystal Structure and Properties of Ag10Si3S11The novel orange-red thiosilicate Ag10Si3S11 is formed besides Ag8SiS6 by the high - temperature reaction between Ag2S, Si and S. The single crystal structure analysis shows the compound to be silver orthothiosilicate thiodisilicate-(1:1) Ag10(SiS4)(Si2S7). The mean Si—S bond lengths are 2.137 Å for SiS4(4-) and 2.129 Å for the hitherto unknown Si2S7(6-). The cation sublattice is slightly imperfect. inferring a certain mobility of the Ag+ ions. Ag10Si3S11 crystallizes in the triclinic space group P1. Lattice constants see „Inhaltsübersicht“.The vibrational spectrum (IR) shows absorptions within the characteristic spectral regions for asymmetric and symmetric stretching vibrations of the SiS4 tetrahedra at 490-515 and 423-433 cm-1.
    Notes: Neben Ag8SiS6 entsteht bei der Hochtemperaturreaktion von Ag2S mit Si und S das bisher unbekannte orangerote Ag10Si3S11. Die Einkristall-Röntgenstrukturanalyse zeigt, daß die Substanz als Silber-orthothiosilicat-thiodisilicat-(1:1) Ag10(SiS4)(Si2S7) zu formulieren ist. Die mittleren Si—S-Bindungslängen betragen 2,137 Å im SiS4(4-), 2,129 Å im bisher noch nicht beobachteten Si2S7(6-). Das Kationenteilgitter ist leicht gestört und deutet auf eine gewisse Beweglichkeit der Ag+-Ionen im Kristall hin. Ag10Si3S11 kristallisiert triklin (P1) mit a = 12,414, b = 13,476, c = 6,459 Å, α = 78,92°, β = 77,61°, γ = 68,71°, Z = 2.Das Schwingungsspektrum (IR) zeigt Absorptionen in den für asymmetrische und symmetrische Valenzschwingungen der SiS4-Tetraeder charakteristischen Bereichen bei 490-515 bzw. 423-433 cm-1.
    Additional Material: 3 Ill.
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  • 4
    Electronic Resource
    Electronic Resource
    Weinheim : Wiley-Blackwell
    Zeitschrift für anorganische Chemie 388 (1972), S. 193-206 
    ISSN: 0044-2313
    Keywords: Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Description / Table of Contents: The structure of Cd4SiS6 (crystal data see „Inhaltsübersicht“) has been solved from single crystal X-ray data. SiS4 and distorted CdS4 tetrahedra (Si-S 2.101-2.132 Å, Cd-S 2.510-2.694 Å) are linked three-dimensionally by sharing corners in such a way that 2/3 of the S atoms have 2 Cd + 1 Si as bonded neighbors (pyramidal coordination), the rest is tetrahedrally cordinated by 4 Cd. The new defect tetrahedral structure, which is also representative for the isotypic series Cd4GeS6, Hg4SiS6 Hg4GeS6 and Cd4GeSe6, has a strongly distorted packing of the S atoms and shows no close relationship to known types. The Si-S bonds contain only very little π-contributions, similar to the Ge-S and Sn-S bonds in thiogermanates and -stannates. The vibrational spectra of Cd4SiS6 are reported and discussed.Cd4SiSe6, isotypic with Cd4SiS6, has been prepared by reaction of CdSe, Si and Se at 800-1000°.
    Notes: Die Struktur des monoklin in der Raumgruppe Cc mit a = 12,310, b = 7,041, c = 12,336 Å, β = 110,38°, Z = 4 kristallisierenden Cd4SiS6 wurde durch eine Röntgenstrukturanalyse aufgeklärt. Diesem neuen Defekt-Tetraeder-Strukturtyp gehören auch Cd1GeS6, Hg4SiS6, Hg4GeS6 und Cd4GeSe6 an. In der Struktur sind SiS4- und verzerrte CdS4-Tetraeder (Si-S 2,101-2,132 Å, Cd-S 2,510-2,694 Å) über alle vier Polyederecken dreidimensional verknüpft, so daß 2/3 der S-Atome einseitig mit 2 Cd + 1 Si, die restlichen tetraedrisch mit 4 Cd verbunden sind. Die Packung der S-Atome ist stark verzerrt; die Struktur hat wenig Ähnlichkeiten mit bekannten Tetraeder-Strukturtypen. Analog zu den Ge—S- und Sn—S-Bindungen in Thiogermanaten bzw. Thiostannaten enthält die Si—S-Bindung nur sehr geringe „-Anteile. Die Schwingungsspektren von Cd4SiS6 werden angegeben und diskutiert.Tiefrotes, mit Cd4SiS6 isotypes Cd4SiS6 wurde aus CdSe, Si und Se bei 800-1000°C dargestellt.
    Additional Material: 4 Ill.
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  • 5
    Publication Date: 2015-04-19
    Description: The Rosetta Ion and Electron Sensor (IES) has been measuring solar wind ions intermittently since exiting from hibernation in May 2014. On 19 August, when Rosetta was ~80 km from the comet 67P/Churyumov-Gerasimenko (C-G), which was ~3.5 AU from the Sun, IES began to see ions at its lowest energy range, ~4-10 eV. We identify these as ions created from neutral species emitted by the comet nucleus, photo-ionized by solar UV radiation in the neighborhood of the Rosetta spacecraft (S/C) and attracted by the small negative potential of the S/C resulting from the population of thermal electrons. Later, IES began to see higher energy ions that we identify as having been picked up and accelerated by the solar wind. IES continues to measure changes in the solar wind and the development of the pickup ion structure.
    Print ISSN: 0094-8276
    Electronic ISSN: 1944-8007
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 6
    Publication Date: 2014-09-11
    Description: Titan's ionosphere is created when solar photons, energetic magnetospheric electrons or ions, and cosmic rays ionize the neutral atmosphere. Electron densities generated by current theoretical models are much larger than densities measured by instruments onboard the Cassini Orbiter. This model density overabundance must result either from overproduction or from insufficient loss of ions. This is the first of two papers that examines ion production rates in Titan's ionosphere, for the dayside and nightside ionosphere, respectively. The first (current) paper focuses on dayside ion production rates which are computed using solar ionization sources (photoionization and electron-impact ionization by photoelectrons) between 1000 and 1400 km. In addition to theoretical ion production rates, empirical ion production rates are derived from CH 4 , CH 3 + and CH 4 + densities measured by the INMS (Ion – Neutral Mass Spectrometer) for many Titan passes. The modeled and empirical production rate profiles from measured densities of N 2 + and CH 4 + are found to be in good agreement (to within 20%) for solar zenith angles between 15 and 90 degrees. This suggests that the overabundance of electrons in theoretical models of Titan's dayside ionosphere is not due to overproduction but to insufficient ion losses.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 7
    Publication Date: 2017-06-23
    Description: Effects of solar EUV on positive ions and heavy negative charge carriers (molecular ions, aerosol and/or dust) in Titan's ionosphere are studied over the course of almost 12 years, including 78 flybys below 1400 km altitude between TA (Oct 2004) and T120 (June 2016). The RPWS/LP-measured ion charge densities (normalized by the solar zenith angle) show statistically significant variations with respect to the solar EUV flux. Dayside charge densities increase by a factor of ≈2 from solar minimum to maximum, while nightside charge densities are found to anti-correlate with the EUV flux and decrease by a factor of ≈3-4. The overall EUV dependence of the ion charge densities suggest inapplicability of the idealized Chapman theory below 1200 km in Titan's ionosphere. Nightside charge densities are also found to vary along Titan's orbit, with higher values in the sunward magnetosphere of Saturn compared to the magnetotail.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 8
    Publication Date: 2016-09-11
    Description: The importance of the heavy ions and dust grains for the chemistry and aerosol formation in Titan's ionosphere has been well established in the recent years of the Cassini mission. In this study we combine independent in situ plasma (RPWS/LP) and particle (CAPS/ELS, CAPS/IBS, INMS) measurements of Titan's ionosphere for selected flybys (T16, T29, T40 & T56) to produce altitude profiles of mean ion masses including heavy ions and develop a Titan-specific method for detailed analysis of the RPWS/LP measurements (applicable to all flybys) to further constrain ion charge densities, and produce the first empirical estimate of the average charge of negative ions and/or dust grains. Our results reveal the presence of an ion-ion (dusty) plasma below ~ 1100 km altitude, with charge densities exceeding the primary ionization peak densities by a factor ≥ 2 in the terminator and nightside ionosphere ( n e / n i  ≤ 0.1). We suggest that ion-ion (dusty) plasma may also be present in the dayside ionosphere below 900 km ( n e / n i  〈 0.5 at 1000 km altitude). The average charge of the dust grains (≥ 1000 amu) is estimated to be between − 2.5 and − 1.5 elementary charges, increasing toward lower altitudes.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 9
    Publication Date: 2015-01-08
    Description: Ionization of neutrals by precipitating electrons and ions is the main source of Titan's nightside ionosphere. This paper has two goals: (1) characterization of the role of electron impact ionization on the nightside ionosphere for different magnetospheric conditions, and (2) presentation of empirical ion production rates determined using densities measured by the Cassini Ion and Neutral Mass Spectrometer (INMS) on the nightside. The ionosphere between 1000 and 1400 km is emphasized. We adopt electron fluxes measured by the Cassini Plasma Spectrometer Electron-Spectrometer and the Magnetospheric Imaging Instrument as classified by Rymer et al . [2009]. The current paper follows an earlier paper (Paper I), in which we investigated sources of Titan's dayside ionosphere and demonstrated that the photoionization process is well understood. The current paper (Paper II) demonstrates that modeled and empirical ionization rates on the nightside are in agreement with an electron precipitation source above 1100 km. Ion production rate profiles appropriate for different Saturnian magnetospheric conditions, as outlined by Rymer et al ., are constructed for various magnetic field topologies. Empirical production rate profiles are generated for deep nightside flybys of Titan. The results also suggest that at lower altitudes (below 1100 km) another source, such as ion precipitation, is probably needed.
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 10
    Publication Date: 1976-02-01
    Print ISSN: 0044-2313
    Electronic ISSN: 1521-3749
    Topics: Chemistry and Pharmacology
    Published by Wiley
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