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  • 1
    Electronic Resource
    Electronic Resource
    Evolution of silicon carbide particles in the atmospheres of carbon stars
    Amsterdam : Elsevier
    Physica 41 (1969), S. 139-143 
    Details
    ISSN: 0031-8914
    Source: Elsevier Journal Backfiles on ScienceDirect 1907 - 2002
    Topics: Physics
    Type of Medium: Electronic Resource
    URL: http://linkinghub.elsevier.com/retrieve/pii/0031-8914(69)90247-X
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  • 2
    Electronic Resource
    Electronic Resource
    The 10-micron interstellar absorption band: Curves of growth for terrestrial and meteoritic olivine particles (1977)
    Springer
    Astrophysics and space science 48 (1977), S. 305-312 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Curves of growth have been determined for the interstellar absorption band at 9.75 μm using infrared spectra of small olivine particles. The mass absorption coefficient was found to depend strongly on the mean radius of the grains. A comparison was made with a sample of Allende meteorite and good agreement was found between the curves of growth for terrestrial and meteoritic olivine.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00648119
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  • 3
    Electronic Resource
    Electronic Resource
    The ultraviolet absorption band at 2175 Å: Correlations with other interstellar features (1977)
    Springer
    Astrophysics and space science 46 (1977), S. 357-369 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The hump in the ultraviolet part of the interstellar extinction curve is interpreted as a broad diffuse absorption band. Its equivalent width is estimated for 36 stars by means of OAO-2 data. The equivalent widths are correlated with the following parameters: colour excessE(B-V), colour excessE(B − V), depth of the band δm max, equivalent widths of the diffuse bands at 5780 and 6284 Å, and the column density of neutral hydrogenN HI. The physical parameters half-width and oscillator strength of the band at 2175 Å are estimated.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00644383
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  • 4
    Electronic Resource
    Electronic Resource
    Equivalent widths of the 10-μm interstellar silicate feature and dust temperatures in infrared sources (1978)
    Springer
    Astrophysics and space science 54 (1978), S. 181-185 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract For 22 infrared sources showing the 10-μm silicate absorption band, the optical depths, dust temperatures and equivalent widths have been calculated for two assumed simple models.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00637906
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  • 5
    Electronic Resource
    Electronic Resource
    The 10- and 20-μm interstellar absorption bands: Comparison with the infrared spectrum of the Nogoya meteorite (1979)
    Springer
    Astrophysics and space science 60 (1979), S. 297-304 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract For submicrometer-sized particles of the carbonaceous chondrite Nogoya and, for comparison purposes, also of terrestrial chamosite, the mass absorption coefficients have been derived from laboratory spectra for the wavenumber range 250–1300 cm−1. Using these data the expected spectrum of an infrared source has been calculated under simple model assumptions and compared with the observed flux from the infrared source OH 26.5+0.6. Although certain discrepancies are left in the 20-μm region it is concluded that phyllosilicates, especially such occurring in carbonaceous chondrites, are interesting candidates for the material of interstellar grains.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00644333
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  • 6
    Electronic Resource
    Electronic Resource
    Laboratory spectra of protosilicates and the interstellar silicate absorption bands (1980)
    Springer
    Astrophysics and space science 68 (1980), S. 159-174 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract Infrared spectra of submicrometre-sized particles of several protosilicates have been used to derive mass absorption coefficients. These data have been applied in order to describe the infrared radiation from the source OH 26.5+0.6 in terms of a simple model. A good fit of the 10 μm absorption feature could be achieved, but some discrepancies remain in the 20 μm region. The reasons for the weakness of the 20 μm band in infrared sources are discussed. The laboratory spectra revealed that the samples contained a small admixture of carbonates. Thus, some statements about the infrared spectrum of submicrometre-sized carbonate particles could also be made.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00641652
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  • 7
    Electronic Resource
    Electronic Resource
    The 11.5 micrometer emission from carbon stars: Comparison with IR spectra of submicrometer-sized silicon carbide grains (1981)
    Springer
    Astrophysics and space science 79 (1981), S. 405-417 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract In this paper the results of an experimental investigation of the spectra of submicrometersized silicon carbide grains are presented. The grains manufactured from two types of commercial α-SiC were prepared according to the Jena IR spectroscopy program for particulates of cosmic importance. From the spectral records mass absorption coefficients have been derived. These data have been used to make a comparison of the laboratory spectra with the well-known 11.5 μm emission band observed in the spectra of carbon stars, which is probably due to a transition in circumstellar SiC grains. For this aim, a simple model of an optically thin circumstellar envelope containing SiC grains has been calculated. The theoretical profile of the 11.5 μm band derived by means of this model and based on the experimental mass absorption coefficients of SiC grains shows a striking similarity with the observed profile in the spectrum of the carbon star Y CVn. The total amount of SiC dust in the envelope of this star has been estimated at about 1024 g.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00649437
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  • 8
    Electronic Resource
    Electronic Resource
    Can silicon monoxide grains be responsible for the interstellar 9.7 micrometer absorption band? (1981)
    Springer
    Astrophysics and space science 80 (1981), S. 249-255 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract In this paper results of an experimental investigation of the spectra of submicrometersized silicon monoxide grains are presented. The grains manufactured from commercial SiO were prepared according to the Jena IR spectroscopy program for particulates of cosmic importance. The comparison of the laboratory spectra with those derived by means of Mie calculations using published refractive indices of bulk SiO revealed a fundamental discrepancy concerning the number and the positions of the bands. Therefore, the experimental SiO grains are suggested to change their internal structural state by the heating connected with the pressing of the KBr pellets, where the grains are embedded in. This sensitivity against heating by some hundred K rules out that SiO grains can be responsible for the 9.7 μm circumstellar as well as interstellar spectral feature.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00649151
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  • 9
    Electronic Resource
    Electronic Resource
    Cloudy circumstellar dust shells around young variable stars (1994)
    Springer
    Astrophysics and space science 212 (1994), S. 221-229 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract A number of variable stars of the Orion population has been identified with IRAS point sources by us. This finding supports the conclusion that the prominent Algol-like minima in the lightcurves of these stars originate from obscurations by dust clouds in a circumstellar shell. The discussion of the existingUBVR data leads to the remarkable conclusion that the extinction properties of the grain populations contained in individual dust clouds moving in one and the same circumstellar shell are quite different. From the multicolour photometric data of the different Algol-like minima we derived individual values of the reddening parameterR = A v /E(B - V). It covers a remarkable wide range of values from that one typical of the interstellar extinction law up to 7. In the case of SV Cep one of the grain populations produces a virtually neutral extinction. The large values ofR speak in favour of larger than normal (interstellar) dust grains, which may have grown by coagulation processes. The cloudy circumstellar dust shell provides a natural explanation for the observed infrared excess. The properties derived from the optical light variations are fully compatible with the properties deduced from the infrared radiation. The irregularity of the light variations indicates that many clouds are involved and may sometimes superimpose themselves.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00984526
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  • 10
    Electronic Resource
    Electronic Resource
    Problems with the interpretation of the 220 nm interstellar feature (1986)
    Springer
    Astrophysics and space science 128 (1986), S. 71-81 
    Details
    ISSN: 1572-946X
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract The bump in the ultraviolet part of the interstellar extinction curve provides a great challenge in the modelling of interstellar dust. Its shape can be well approximated by a classical dispersion profile with a total halfwidth of 48 nm centred at 217 nm. Apart from few slightly deviating cases the parameters of the band seem to be surprisingly constant in the solar neighbourhood. The equivalent widthW of the 217 nm band shows a very tight correlation with the colour excessE(B-V). Studies of correlations with the strength of diffuse interstellar bands gave no conclusive results as to the nature of the band. The most common interpretation of the 217 nm feature as originating from small graphite grians meets several difficulties. No final decision on the carrier can be made at present.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF00656019
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