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  • 1
    Monograph available for loan
    Monograph available for loan
    The abundance of the elements (1961)
    New York [u.a.] : Interscience
    Associated volumes
    Details Availability
    Call number: M 93.0136/7
    In: Interscience monographs and texts in physics and astronomy
    Type of Medium: Monograph available for loan
    Pages: XI, 283 S.
    Series Statement: Interscience monographs and texts in physics and astronomy 7
    Language: English
    Location: Upper compact magazine
    Branch Library: GFZ Library
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  • 2
    Electronic Resource
    Electronic Resource
    THE CHEMICAL COMPOSITION OF THE INTERSTELLAR MEDIUM (1972)
    Oxford, UK : Blackwell Publishing Ltd
    Annals of the New York Academy of Sciences 194 (1972), S. 0 
    Details
    ISSN: 1749-6632
    Source: Blackwell Publishing Journal Backfiles 1879-2005
    Topics: Natural Sciences in General
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1111/j.1749-6632.1972.tb12691.x
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  • 3
    Electronic Resource
    Electronic Resource
    Monochromatic photographs of giantHii regions in the Magellanic Clouds (1977)
    Springer
    Astrophysics and space science 46 (1977), S. 371-378 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Narrow band-pass direct photographs have been secured of the central region of 30 Doradus and of several other nebulosities in the Magellanic Clouds. We have utilized an image tube camera attached to the Yale one-meter telescope at the Cerro Tololo Interamerican Observatory. Interference filters whose band passes were selected to allow for the radial velocities of the Magellanic Clouds have been utilized to record monochromatic images of [Nii] λ6584, Hα, Hei λ5876, and [Oiii] λ5007. In 30 Doradus the main filamentary structures appear to be very similar in Hα, Hei, [Nii], and [Oiii] at least in the inner regions where most spectroscopic measurements have been made. The features appear to be material bounded rather than radiation bounded and the excitation differences are very small. Likewise, in NGC 346 in the Small Magellanic Cloud the [Oiii] and Hα images are very similar, but in N44 in the Large Magellanic Cloud excitation differences do appear. The implications of these observations for chemical compositions of nebulosities in the Magellanic Clouds would appear to be that spectroscopic and scanner studies should be supplemented by monochromatic photographs. Some nebulosities can be handled by simple models while for others excitation differences must be taken into account.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00644384
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  • 4
    Electronic Resource
    Electronic Resource
    The spectrum of the manganese star ι Coronae Borealis (1970)
    Springer
    Astrophysics and space science 8 (1970), S. 262-266 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Iota Coronae Borealis is a manganese mercury star with a rich spectrum of sharp lines. We tabulate equivalent widths element by element from data obtained at Lick 120-inch telescope.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00650889
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  • 5
    Electronic Resource
    Electronic Resource
    A spectroscopic study of moderately bright planetary nebulae (1979)
    Springer
    Astrophysics and space science 62 (1979), S. 397-437 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Spectroscopic results are presented for most of the nebulae observed in a programme involving some forty planetaries measured with an image tube scanner at Lick Observatory and with a photo-electric spectrum scanner at Mt. Wilson Observatory. The spectroscopic range normally covered, λ 3700 to λ 8700 is supplemented for a few objects with appropriate photographic data calibrated photoelectrically for the region λ 3120-λ 3800. Available published photoelectric data are also employed to improve the calibration of the finally adopted system of intensities. The main thrust of the programme is to investigate weaker lines, arising from less abundant ions, or due to less favorable excitation conditions. Information pertaining to additional ions gives further diagnostic data on the nebular plasma. For a given nebula, different diagnostics suggest different values of the electron temperature and density. These are believed to represent actual variations in physical conditions from point to point within the nebula, although in some instances, they may reflect inadequacies in atomic parameters, particularly collisional cross-sections. The spectroscopically most interesting nebulae show a wide variation in physical conditions, indicated by lines ranging in excitation from those of Mgi to [Fevii]. Relatively cool clouds of denser material appear to be immersed in a high excitation plasma excited by a hot central star.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00645478
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  • 6
    Electronic Resource
    Electronic Resource
    The spectrum of the manganese-scandium star ϕ Herculis (1970)
    Springer
    Astrophysics and space science 8 (1970), S. 267-274 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Among manganese stars, ϕ Herculis is of great interest because of the unusual strength of the scandium lines. We present intensity measurements for numerous lines ofCii, Mgi, Mgii, Siii, Caii, Scii, Tiii, Crii, Mni, Mnii, Fei, Feii, Coii, Srii,Yii, and Zrii.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00650890
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  • 7
    Electronic Resource
    Electronic Resource
    The solar abundance of beryllium (1974)
    Springer
    Solar physics 36 (1974), S. 11-19 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The solar abundance of beryllium is deduced from high-resolution Kitt Peak observations of the λ3130.43 and λ3131.08 lines of Be II interpreted by the method of spectrum synthesis. The results are in good agreement with those previously obtained by Grevesse and by Hauge and Engvold and indicate that in the photospheric layers, beryllium is depleted below the chondritic value by a factor of about two. We find |Be} ≡ log N(Be)/N(H)+ 12 = 1.08.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00151536
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  • 8
    Electronic Resource
    Electronic Resource
    The solar abundance of thulium (1974)
    Springer
    Solar physics 36 (1974), S. 21-23 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The solar spectrum contains one relatively unblended line λ 3131.258 Tm ii which yields a thulium abundance of log N(Tm)/N(H) + 12 = {Tm} = 0.80 ± 0.10, with the Corliss and Bozman f-value. A recent beam-foil experiment suggests that the thulium abundance may be reduced to {Tm} = 0.30.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00151537
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  • 9
    Electronic Resource
    Electronic Resource
    The solar abundance of silver (1972)
    Springer
    Solar physics 25 (1972), S. 30-43 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Low noise, high resolution spectral scans have been obtained for the resonance lines of silver λ3280.7 and λ3382.9, observed at the centre of the solar disk. A double pass-monochromator is used in conjunction with the Snow telescope at Mount Wilson; the transparency of the sky is monitored during the observations in order to achieve required accuracy. The data are analyzed by the method of spectral synthesis wherein we employ a model atmosphere resembling Elste's (1968) model and checked by limb-darkening observations. The present kinematical model adopts a macroturbulent velocity of 2.2 km s−1 and no microturbulence. With this model line profiles can be reproduced without invoking implausibly large collisional damping constants. The silver abundance turns out to be {Ag}=log[N(Ag)/N(H)]+12;=0.85, a factor of four under the value found from the Type I carbonaceous chondrites.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00155742
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  • 10
    Electronic Resource
    Electronic Resource
    The solar abundance of gold (1972)
    Springer
    Solar physics 23 (1972), S. 13-17 
    Details
    ISSN: 1573-093X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract From 13 scans obtained with a double-band pass spectrograph at the Snow telescope at Mount Wilson, interpreted by the method of spectral synthesis, the abundance of gold turns out to be log [N(Au)/N(H)] + 12 = 0.70, assuming loggf = − 0.57.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00153887
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