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  • 1
    ISSN: 0749-1581
    Keywords: Humic substances ; Quantification ; 13C NMR ; DEPT ; SEMUT-90 ; J-resolved ; Volume integration ; Chemistry ; Analytical Chemistry and Spectroscopy
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Notes: Partial structures of a reference groundwater humic substance were quantified by J-resolved two-dimensional 13C NMR spectroscopy applied in its phase-sensitive variant. The results agree with those obtained by the one-dimensional techniques DEPT (distortionless enhancement by polarization transfer) and SEMUT-90 (subspectral editing using a multiple quantum trap), thus demonstrating the accuracy of both methods. However, the two-dimensional technique is recommended, because quantification is based on only one spectrum. Quantification provides the ratio of different substructures (carbons belonging to ketones, carboxylic acids, different aromatics, carbohydrates, paraffinic C, CH, CH2 and CH3 groups) and, in combination with elemental analysis, the partition of hydrogen between C and O (83% bonded to C and 17% to O). Also, insight is obtained into the biogenesis of the humic acids. Aromatic moieties probably originate mainly from lignin rather than from other aromatic compounds. CH—O moieties mainly belong to carbons in ethers and alcohols and only to a small extent to carbons in carbohydrates, as shown by comparing NMR results with gas chromatographic analysis of the carbohydrate part performed by other workers. The ratio of paraffinic CH:CH2:CH3 is about 1:1:1; the high proportion of paraffinic methyl groups cannot yet be explained.
    Additional Material: 3 Ill.
    Type of Medium: Electronic Resource
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  • 2
    ISSN: 0749-1581
    Keywords: NMR ; 13C NMR ; 17O NMR ; Cyclohexanones ; Orbital interactions ; Polar effects ; Substituent-induced shifts ; Chemistry ; Analytical Chemistry and Spectroscopy
    Source: Wiley InterScience Backfile Collection 1832-2000
    Topics: Chemistry and Pharmacology
    Notes: The carbon-13 chemical shifts were assigned for all ring positions in cyclohexanone and 4-tert-butylcyclohexanone with H, F, Cl, Br, I, MeO, MeS, MeSe, Me2N, Me or tert-butyl in the 2-position. The substituent-induced shifts were calculated by difference from unsubstituted cyclohexanone or 4-tert-butylcyclohexanone. Both stereoisomers (cis and trans) were available for the 4-tert-butylcyclohexanones in all but one case. Comparison of the substituent-induced shifts for the cis (equatorial 2-substituent) and trans (axial 2-substituent) isomers provides stereochemical insight into the interactions between the 2-substituent and the carbonyl group that bring about non-additivity of the substituent effects. In the 2-equatorial isomer, the dipole-dipole interaction between the functional groups causes non-additivities for the C-2 carbon that depend largely on the electronegativity of the 2-substituent. In the 2-axial isomer, hyperconjugation or other orbital interactions between the groups cause non-additivities for the C-2 carbon that depend largely on the polarizability in addition to the electronegativity of the 2-substituent.
    Additional Material: 3 Tab.
    Type of Medium: Electronic Resource
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  • 3
    Publication Date: 2013-08-31
    Description: A 100 Mbit/s FDDI (fiber distributed data interface) network interface unit is described that supports real-time data, voice and video. Its high-speed interrupt-driven hardware architecture efficiently manages stream and packet data transfer to the FDDI network. Other enhancements include modular single-mode laser-diode fiber optic links to maximize node spacing, optic bypass switches for increased fault tolerance, and a hardware performance monitor to gather real-time network diagnostics.
    Keywords: OPTICS
    Type: NASA, Washington, Technology 2000, Volume 2; p 268-275
    Format: application/pdf
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  • 4
    Publication Date: 2019-06-28
    Description: An improved AOTF-based imaging spectrometer that offers several advantages over prior art AOTF imaging spectrometers is presented. The ability to electronically set the bandpass wavelength provides observational flexibility. Various improvements in optical architecture provide simplified magnification variability, improved image resolution and light throughput efficiency and reduced sensitivity to ambient light. Two embodiments of the invention are: (1) operation in the visible/near-infrared domain of wavelength range 0.48 to 0.76 microns; and (2) infrared configuration which operates in the wavelength range of 1.2 to 2.5 microns.
    Keywords: OPTICS
    Format: application/pdf
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  • 5
    Publication Date: 2019-07-13
    Description: Interstellar CO A-X bands in the spectrum of zeta Oph were recorded at high Sound-to-Noise (S/N) with grating G160M of the Goddard High Resolution Spectrograph on the Hubble Space Telescope. Isotopic fractionation of CO is severe: CO-12/CO-13 = 167, C(16)O/C(18)O approximately equal to 1550 and C(16)O/C(17)O is greater than 5900 are found where C-12/C-13 = 70, O-16/O-18 = 500, and O-16.O-17 = 2600 are observed or expected. Standard models of the zeta Oph cloud predict CO-12/CO-13 is less than or approximately 70. The higher observed ratio suggests that photodissociation of CO, not the isotopic charge exchange reaction ((13)C(+) + CO reversible reaction (12)C(+) + (13)(CO), is the dominant influence on the CO-12/CO-13 ratio.
    Keywords: ASTROPHYSICS
    Type: The Astrophysical Journal, Part 1 (ISSN 0004-637X); 420; 2; p. 756-771
    Format: text
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  • 6
    Publication Date: 2019-08-17
    Description: An acousto-optic tunable filter (AOTF) is employed to generate a display by driving the AOTF with a RF electrical signal comprising modulated red, green, and blue video scan line signals and scanning the AOTF with a linearly polarized, pulsed light beam, resulting in encoding of color video columns (scan lines) of an input video image into vertical columns of the AOTF output beam. The AOTF is illuminated periodically as each acoustically-encoded scan line fills the cell aperture of the AOTF. A polarizing beam splitter removes the unused first order beam component of the AOTF output and, if desired, overlays a real world scene on the output plane. Resolutions as high as 30,000 lines are possible, providing holographic display capability.
    Keywords: OPTICS
    Type: NAS 1.71:NPO-18736-1-CU
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  • 7
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    In:  Other Sources
    Publication Date: 2019-08-28
    Description: The interstellar spectrum of HD 169454 reveals Na D and Ca K absorption at about + 100 km/s. Measurements made at high resolution resolve 4 narrow (about 2-3 km/s) features whose N(Ca II)/N(Na I) ratios are small. This high-velocity gas is, therefore, unique in that it resembles local quiescent gas, not shocked gas. Redshifted gas is also seen in moderate-resolution spectra of faint stars lying in the same portion of the sky as HD 169454. The resulting picture is one in which a supernova explosion or stellar winds within the Sct OB3 association at a distance of about 1.5 kpc is pushing quiescent gas away from the sun. The gas is seen only in stars estimated to be at most 3 kpc, but greater than 2 kpc, away. If HD 169454 is at this greater distance, its absolute magnitude would be about -9, making it the second most luminous B star in the Galaxy.
    Keywords: ASTROPHYSICS
    Type: Astronomical Journal (ISSN 0004-6256); 104; 2 Au; 691-695
    Format: text
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  • 8
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    In:  Other Sources
    Publication Date: 2019-08-28
    Description: The present conference discusses theoretical and observational views of star formation, spectroscopic constraints on the evolution of massive stars, very low mass stars and brown dwarfs, asteroseismology, globular clusters as tests of stellar evolution, observational tests of stellar evolution, and mass loss from cool evolved giant stars. Also discussed are white dwarfs and hot subdwarfs, neutron stars and black holes, supernovae from single stars, close binaries with evolved components, accretion disks in interacting binaries, supernovae in binary systems, stellar evolution and galactic chemical evolution, and interacting binaries containing compact components.
    Keywords: ASTROPHYSICS
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  • 9
    Publication Date: 2019-07-13
    Description: The B I 2496.8 A resonance line and HST/GHRS echelle spectra are used with model atmospheres and synthetic spectra to derive the B abundance of the F dwarfs Procyon (Alpha Canis Minoris), Theta Ursae Majoris, and Iota Pegasi. The B abundance of Theta UMa and Iota Peg is similar to that derived by Boesgaard and Heacox (1978) from the B II resonance line in spectra of A- and B-type stars. These two dwarfs show normal abundances of Li, Be, and B. Procyon, which is highly depleted in Li and Be, is depleted in B by a factor of at least 3. Comparison of the spectra of Procyon and the halo dwarf HD 140283 shows that the B abundance assigned by Duncan et al. (1992) to three halo dwarfs is not greatly overestimated as a result of contamination of the B I line by an unidentified line.
    Keywords: ASTROPHYSICS
    Type: Astronomical Society of the Pacific, Publications (ISSN 0004-6280); 105; 687; p. 468-475.
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  • 10
    Publication Date: 2019-07-13
    Description: Numerous weak lines from interstellar atomic species toward Zeta Ophiuchi were observed with the Goddard High-Resolution Spectrograph. Of particular note are the first interstellar detection of cobalt and the detection of boron in this sight line. These measurements provide estimates for the amount of depletion for the two elements. Boron, a volatile, and cobalt, a refractory element, display the depletion pattern found by Savage et al. (1992). The abundance of phosphorus in the H II region associated with the star was obtained from a detection of P III. Additional weak lines from S I, C I, Ni II, and Cu II were detected for the first time; these lines provide the basis for refinements in oscillator strength and column density. Analysis of the neutral sulfur data indicates that the atomic gas is more widely distributed than the molecular material in the main component.
    Keywords: ASTROPHYSICS
    Type: Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X); 413; 1; p. L51-L54.
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