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  • ASTROPHYSICS  (589)
  • Inorganic Chemistry  (309)
  • Alpha-scintillation; DEPTH, sediment/rock; Description; Dredge; DRG; Event label; Identification; Kara Sea; Lake_Uksh_K; Lake Uksh, Karelia, Russia; Mass; NOAA and MMS Marine Minerals Geochemical Database; NOAA-MMS; Radium; Sedov (1909); Sedov-1934; SEDOV34_74; Width
  • NUCLEAR ENGINEERING
  • 1980-1984  (705)
  • 1935-1939  (61)
  • 1905-1909  (134)
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  • 1
    Electronic Resource
    Electronic Resource
    Weinheim : Wiley-Blackwell
    Zeitschrift für anorganische Chemie 476 (1981), S. 214-220 
    ISSN: 0044-2313
    Keywords: Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Description / Table of Contents: Vibrational Spectrum of α-Te2MoO7 and a Proposal for the Structure of Telluromolybdates of Divalent CationsInfrared and Raman spectra of α-Te2MoO7 have been recorded and discussed in relation to their known crystalline structure. The comparison of these spectra with those of telluromolybdates of the type MIITeMoO6, allows us to propose a structural model for these phases, which is totally consistent with the spectroscopic findings.
    Notes: Die IR- und Raman-Spektren von α-Te2MoO7 wurden aufgenommen und an Hand der bekannten kristallographischen Daten zugeordnet. Durch Vergleich dieser Spektren mit demjenigen einiger Telluromolybdate des Typs MIITeMoO6 kann für diese Phasen ein Strukturvorschlag gegeben werden, der sich durch die spektroskopischen Daten einwandfrei rechtfertigen läßt.
    Additional Material: 2 Ill.
    Type of Medium: Electronic Resource
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  • 2
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    In:  CASI
    Publication Date: 2014-09-16
    Description: Observations at the 2.6 mm line of CO reveal the presence of a large number of molecular clouds at high galactic latitude. If the velocity dispersion of the clouds is a measure of their scale height, the mean distance of the ensemble detected is 100 pc. The clouds are unusual in that either they are not gravitationally bound or they are very deficient in CO relative to molecular hydrogen. These clouds represent a heretofore unrecognized component of the local interstellar medium. If they are pervasive in the Milky Way, they probably represent the small molecular cloud component of the interstellar medium.
    Keywords: ASTROPHYSICS
    Type: NASA. Goddard Space Flight Center Local Interstellar Medium, No. 81; p 231-234
    Format: text
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  • 3
    Publication Date: 2019-06-28
    Description: Morphological evidence is presented (in the form of 3-A-bandpass Fabry-Perot images made with a CCD camera) that the two bright emission-line systems seen toward the galaxy NGC 1275 arise from a high-velocity impact of a foreground galaxy upon the accretion flow of gas cooling in the center of the Perseus cluster. The uniquely high optical-line luminosity of NGC 1275, in comparison with other central galaxies in clusters observed to have cooling flows, may be explained by energy deposited during the collision. Using additional information from 21-cm and extinction measurements, a rough model of the interaction is developed. Problems remain with this model - such as the likelihood of a gas-rich system penetrating to the cluster center. The kinematic structure of the optically emitting gas shows additional complex structure near the nucleus of NGC 1275.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X); 275; L27-L31
    Format: text
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  • 4
    Publication Date: 2019-06-28
    Description: The Einstein Imaging Particle Counter observed a major X-ray flare in its entirety during a 5-hr period of simultaneous observations, with the IUE, of the dM5e flare star Proxima Centauri in August, 1980. The detailed X-ray light curve, temperature determinations during various intervals, and UV line fluxes obtained before, during, and after the flare indirectly indicate a 'two-ribbon flare' prominence eruption. The calculated ratio of coronal to bolometric luminosity for the event is about 100 times the solar ratio. The Proxima Cen corona is analyzed in the context of static loop models, in light of which it is concluded that less than 6% of the stellar surface seems to be covered by X-ray emitting active regions.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal; vol. 267
    Format: text
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  • 5
    Publication Date: 2019-06-28
    Description: The 1.24-sec pulsations of Her X-1 in the energy range 13-75 keV have been analyzed in data obtained from the UCSD/MIT experiment on HEAO 1 during observations of the source on three dates in February 1978 and three in August 1978. Observational results are (1) the main pulse broadens somewhat with increasing energy; (2) the pulsation light curve undergoes pronounced changes at the leading edge of the main pulse from day to day; (3) spectral hardening within the main pulse is confirmed; (4) a 40-60 keV spectral feature in the spectrum is confirmed; (5) this feature is resolved, the pulse width broadening is greater than 20%, and its centroid varies with pulsation phase; and (6) the 13-75 keV spectrum does not noticeably vary from day to day, except for an overall intensity factor. Some implications of these results for the prevailing models of Her X-1 and the HZ Her-Her X-1 system are briefly discussed.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal; vol. 240
    Format: text
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  • 6
    Publication Date: 2019-06-28
    Description: X-ray spectra of GX 339-4 measured on three occasions in 1977 and 1978 are presented. These are the first reported measurements above 10 keV. The spectra can be described as the superposition of a soft component, which is dominant below about 20 keV, and a hard component at higher energy. Simultaneous measurements at lower energy show that the soft component vanished during the observation in early 1978. The behavior of these two components is similar to that of the spectrum of Cygnus X-1; this reinforces the previously noted resemblance in rapid X-ray variability.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal; vol. 262
    Format: text
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  • 7
    Publication Date: 2019-06-28
    Description: On five occasions in 1977 and 1978, Cygnus X-1 was observed using the low-energy detectors of the UCSD/MIT Hard X-ray and Low-Energy Gamma Ray experiment on the HEAO 1 satellite. Rapid (times between 0.08 and 1000 sec) variability was found in the 10-140 keV band. The power spectrum was white for frequencies between 0.001 and 0.05 Hz and was proportional to the inverse of the frequency for frequencies between 0.05 and 3 Hz, indicating correlations on all time scales less than approximately 20 s. The shape of the energy spectrum was correlated with intensity; it was harder at higher intensity. If the emission is produced by Comptonization of a soft photon flux in a hot cloud, the heating of the cloud cannot be constant; it must vary on time scales up to approximately 20 s. A variable accretion rate could cause the observed effects.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal; vol. 246
    Format: text
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  • 8
    Publication Date: 2019-07-13
    Description: The photon number spectrum integrated over the impulsive part of the event is shown to fit a thermal bremsstrahlung function with a temperature of 330 + or - 70 keV at energies between 151 and 487 keV. At lower energies, the data points lie considerably below this function, indicating a broad absorption feature extending down to values less than or equal to 28 keV, the lowest energy measured. The upper energy of this absorption feature varies from 100 to 150 keV on a time scale less than or equal to 0.5 s. This event is interpreted as a typical gamma ray burst, even though it is still considered remotely possible that it is of solar origin. The spectral features, together with their variability, are interpreted in terms of electron interactions at the cyclotron resonance frequency in magnetic fields of 10 to the 12th - 10 to the 13th gauss close to the surface of a neutron star.
    Keywords: ASTROPHYSICS
    Type: Gamma ray transients and related astrophysical phenomena; Workshop; Aug 05, 1981 - Aug 08, 1981; La Jolla, CA
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  • 9
    Electronic Resource
    Electronic Resource
    Weinheim : Wiley-Blackwell
    Zeitschrift für anorganische Chemie 472 (1981), S. 193-199 
    ISSN: 0044-2313
    Keywords: Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Description / Table of Contents: Raman Spectra of the Rare Earth OrthovanadateThe laser-Raman spectra of the tetragonal rare earth orthovanadates of the type LnVO4 (Ln = Pr to Lu) as well as those of ScVO4 and YVO4 has been recorded and interpreted with the aid of both, the site symmetry and the factor group analysis, using also IR data reported previously. The influence of the cations on the internal vibrations of the anion are discussed in detail.
    Notes: Die Laser-Raman-Spektren der tetragonalen Orthovanadate der Seltenen Erden des Typs LnVO4 (Ln = Pr bis Lu) sowie diejenigen von ScVO4 und YVO4 wurden aufgenommen und an Hand einer „Site-Symmetrie“-bzw. Faktorgruppenanalyse gedeutet. Auch Daten früher durchgeführter IR-Messungen wurden herangezogen. Der Einfluß der Kationen auf die inneren Anionenschwingungen wurde eingehend diskutiert.
    Additional Material: 2 Ill.
    Type of Medium: Electronic Resource
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  • 10
    ISSN: 0044-2313
    Keywords: Chemistry ; Inorganic Chemistry
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Description / Table of Contents: Crystal and Molecular Structures of (1-Ferrocenyl-1-oxo-ethyl)tricarbonylcyclopentadienyltungsten and μ-[(1-oxo-ethyl)cyclopentadienyl] (tricarbonylmangan)tricarbonylcyclopentadienyltungstenX-ray analysis of (1-ferrocenyl-1-oxo-ethyl)tricarbonylcyclopentadienyltungsten C5H5FeC5H4COCH2W(CO)3C 5H5 (I) and μ-[(1-oxo-ethyl)cyclopentadienyl](tricarbonylmangan)tricarbonylcyclopentadienyltungsten (CO)3MnC5H4COCH2W(CO)3C5H5 (II) were carried out. The two compounds crystallize in the triclinic centrosymmetric space group P1 with the lattice parameters a = 12.99 Å, b = 11.409 Å, c = 6.530 Å,α = 90.83°, β = 92.62°, γ = 110.37° for I and a = 6.886 Å, b = 20.860 Å, c = 6.907 Å,α = 97.20°, β = 67.77°, γ = 97.35° for II. The refinement of the atomic parameters led to final discrepancy factors of R = 0.059 for I and R = 0.086 for II.The existence of ligands with electron donor behaviour and the σ-bonds W—C have no significant effect on the bond distances of the carbonyl groups.
    Notes: Es wurden die Röntgenkristallstrukturanalysen des (1-Ferrocenyl-1-oxo-ethyl)tricarbonylcyclopentadienylwolfram C5H5FeC5H4COCH2W(CO)3C 5H5 (I) und des μ-[(1-oxo-ethyl)cyclopentadienyl](tricarbonylmangan)tricarbonylcyclopentadienylwolfram (CO)3MnC5H4COCH2W(CO)3C5H5 (II) durchgeführt. Beide Substanzen kristallisieren in der triklinen zentrosymmetrischen Raumgruppe P1 mit den Gitterkonstanten a = 12,990 Å, b = 11,409 Å, c = 6,530 Å,α = 90,83°, β = 92,62°, γ = 110,37° für I und a = 6,886 Å, b = 20,860 Å, c = 6,907 Å,α = 97,20°, β = 67,77°, γ = 97,35° für II. Die Verfeinerung der Atomparameter mit Least-squares-Methoden erfolgte bis zu R-Werten von R = 0,059 bei I und R = 0,086 bei II.Die Anwesenheit verschiedener als Elektronendonatoren wirkender Liganden und die σ-Bindungen W—C haben keinen signifikanten Einfluß auf die Bindungsabstände der Ketogruppe.
    Additional Material: 2 Ill.
    Type of Medium: Electronic Resource
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