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  • 1
    Electronic Resource
    Electronic Resource
    ESR-Untersuchungen an bestrahlten PhosphatgläsernProfessor Günther Rienäcker zum 70. Geburtstage am 13. Mai 1974 gewidmet. (1974)
    Weinheim : Wiley-Blackwell
    Zeitschrift für anorganische Chemie 405 (1974), S. 286-298 
    Details
    ISSN: 0044-2313
    Keywords: Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Description / Table of Contents: ESR Studies of Radiation Processes in Phosphate GlassesRadiation processes in phosphate glasses are investigated by ESR and optical measurements. ESR shows a hole-centre in the systems K2O/P2O5 and K2O/MGO/P2O5 which depends on manner and concentration of the cations. Its nature is explained in somewhat a different way than given by BEEKENKAMP or by MIURA and HASEGAWA. Another hole-centre which is independent of cations is discussed in agreement with optical investigations. The electrons set free by radiation react with O2 solved in the glass or with cations. The particels Ag0, Ag2+, Ag+2 have been found and Agn+4 may be present too in the system K2O/MgO/Ag2O/P2O5. The system K2O/MgO/Tl2O/P2O5 shows analogous reactions, but full explanation of the lines could not yet be given.
    Notes: Durch ESR-Untersuchungen und Vergleiche mit optischen Messungen werden Aussagen über die durch Bestrahlung in Phosphatgläsern ablaufenden Vorgänge gemacht. In den Systemen K2O/P2O5 und K2O/MgO/P2O5 wird durch ESR-Messungen ein kationenabhängiges Lochzentrum gefunden, dessen Natur in Abweichung von den Modellen nach BEEKENKAMP und nach MIURA u. HASEGAWA erklärt wird. Ein weiteres kationenunabhängiges Lochzentrum wird in Übereinstimmung mit optischen Untersuchungen gedeutet. Die durch Bestrahlung freigesetzten Elektronen lagern sich an im Glas gelösten Sauerstoff (O2) an oder reagieren mit den Kationen. Im System K2O/MgO/Ag2O/P2O5 werden die Teilchen Ag0, Ag2+, Ag+2 gefunden und Agn+4 wahrscheinlich gemacht. Für das System K2O/MgO/Tl2O/P2O5 gelten analoge Verhältnisse. Eine ausführliche Zuordnung konnte aber dabei noch nicht vorgenommen werden.
    Additional Material: 6 Ill.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1002/zaac.19744050309
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    Paper (German National Licenses)
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  • 2
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    First apsidal motion and light curve analysis of 162 eccentric eclipsing binaries from LMC (2020)
    EDP Sciences
    Details
    Publication Date: 2020-08-01
    Description: We present an extensive study of 162 early-type binary systems located in the LMC galaxy that show apsidal motion and have never been studied before. For the ample systems, we performed light curve and apsidal motion modelling for the first time. These systems have a median orbital period of 2.2 days and typical periods of the apsidal motion were derived to be of the order of decades. We identified two record-breaking systems. The first, OGLE LMC-ECL-22613, shows the shortest known apsidal motion period among systems with main sequence components (6.6 years); it contains a third component with an orbital period of 23 years. The second, OGLE LMC-ECL-17226, is an eccentric system with the shortest known orbital period (0.9879 days) and with quite fast apsidal motion period (11 years). Among the studied systems, 36 new triple-star candidates were identified based on the additional period variations. This represents more than 20% of all studied systems, which is in agreement with the statistics of multiples in our Galaxy. However, the fraction should only be considered as a lower limit of these early-type stars in the LMC because of our method of detection, data coverage, and limited precision of individual times of eclipses.
    Print ISSN: 0004-6361
    Electronic ISSN: 1432-0746
    Topics: Physics
    Published by EDP Sciences
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  • 3
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    CzeV1731: The unique doubly eclipsing quadruple system (2020)
    EDP Sciences
    Details
    Publication Date: 2020-10-01
    Description: We report the discovery of the relatively bright (V = 10.5 mag), doubly eclipsing 2+2 quadruple system CzeV1731. This is the third known system of its kind, in which the masses are determined for all four stars and both the inner and outer orbits are characterized. The inner eclipsing binaries are well-detached systems moving on circular orbits: pair A with period PA = 4.10843 d and pair B with PB = 4.67552 d. The inner binaries contain very similar components (q  ≈  1.0), making the whole system a so-called double twin. The stars in pair B have slightly larger luminosities and masses and pair A shows deeper eclipses. All four components are main-sequence stars of F/G spectral type. The mutual orbit of the two pairs around the system barycenter has a period of about 34 yr and an eccentricity of about 0.38. However, further observations are needed to reveal the overall architecture of the whole system, including the mutual inclinations of all orbits. This is a promising target for interferometry to detect the double at about 59 mas and ΔMbol 〈  1 mag.
    Print ISSN: 0004-6361
    Electronic ISSN: 1432-0746
    Topics: Physics
    Published by EDP Sciences
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  • 4
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    The period-gap cataclysmic variable CzeV404 Her: A link between SW Sex and SU UMa systems (2021)
    EDP Sciences
    Details
    Publication Date: 2021-08-01
    Description: Context. We present a new study of the eclipsing cataclysmic variable CzeV404 Her (Porb = 0.098 d) that is located in the period gap. Aims. This report determines the origin of the object and the system parameters and probes the accretion flow structure of the system. Methods. We conducted simultaneous time-resolved photometric and spectroscopic observations of CzeV404 Her. We applied our light-curve modelling techniques and the Doppler tomography method to determine the system parameters and analyse the structure of the accretion disk. Results. We found that the system has a massive white dwarf MWD = 1.00(2) M⊙, a mass ratio of q = 0.16, and a relatively hot secondary with an effective temperature T2 = 4100(50) K. The system inclination is i = 78.8°. The accretion disk spreads out to the tidal limitation radius and has an extended hot spot or line region. The hot spot or line is hotter than the remaining outer part of the disk in quiescence or in intermediate state, but does not stand out completely from the disk flux in (super)outbursts. Conclusions. We claim that this object represents a link between two distinct classes of SU UMa-type and SW Sex-type cataclysmic variables. The accretion flow structure in the disk corresponds to the SW Sex systems, but the physical conditions inside the disk fit the behaviour of SU UMa-type objects.
    Print ISSN: 0004-6361
    Electronic ISSN: 1432-0746
    Topics: Physics
    Published by EDP Sciences
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