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Buckminster Fullerene and Interstellar Extinction
Acta Astronomica, 2023Most of over 500 Diffuse Interstellar Bands (DIBs) can not be assigned to any carrier. Only the infrared DIBs at 9348-9632 Å are known to be absorption lines of the buckminster fullerene cation C60+. We show that equivalent width of the 9577 Å DIB is correlated with the bump area on the ultraviolet extinction curve and with interstellar reddening E(B-V)
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Astrofizika, 1986
A model of two-layer cylindrical interstellar dust grains is used to calculate the interstellar extinction curves in the visible and near infrared regions of the spectrum and the ratio R /sub V/ of the total to the selective extinction. It is assumed that the core of the two-layer grains consists of ''astronomical silicate'' and the mantle of dirty ice
V B Il'In
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A model of two-layer cylindrical interstellar dust grains is used to calculate the interstellar extinction curves in the visible and near infrared regions of the spectrum and the ratio R /sub V/ of the total to the selective extinction. It is assumed that the core of the two-layer grains consists of ''astronomical silicate'' and the mantle of dirty ice
V B Il'In
exaly +2 more sources
The interstellar extinction curve
Publications of the Astronomical Society of the Pacific, 1993The history of the study of interstellar extinction is briefly discussed. The methods used to determine the extinction law are presented and compared, and the main difficulties involving the application of certain methods are shown. This paper emphasizes the necessity of investigating single-clou extinction curves instead of ill-defined long distance ...
J. Krelowski, J. Papaj
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Interstellar Dust and Extinction
Annual Review of Astronomy and Astrophysics, 1987The ultraviolet (UV) region of the spectrum has been crucial in providing information on the nature of the material and size distribution of the particles of interstellar dust. Before there were any measurements of the UV properties of interstellar extinction, interstellar particles were believed to be composed primarily of dirty ices.
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Features of the interstellar extinction curve
Astrophysics and Space Science, 1975The extinction curves for spherical particles are subject to the errors of the particle material’s refractive index. Their sensitivity to these errors has been investigated and is found to be dependent upon wavelength. For graphite, significant errors are produced in the far ultraviolet part of the extinction curve; for silicates, in the near ...
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Interstellar Extinction and Polarisation
1991In Chapter 1 we referred briefly to the early measurements of interstellar extinction over the UBV wavelength range that gave an approximately 1/λ extinction coefficient amounting typically to ~ 1–2 mag/kpc. We now discuss both extinction and polarisation observations in more detail with a view to using this data as discriminants for grain models in ...
F. Hoyle, N. C. Wickramasinghe
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1969
Many observations became understandable only when astronomers realized that there are huge clouds of gas and dust in interstellar space, by which the light of far-off stars is dimmed and reddened. In order to reduce our observations for this effect, we have to find how this extinction depends on wavelength; our results will also help to understand the ...
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Many observations became understandable only when astronomers realized that there are huge clouds of gas and dust in interstellar space, by which the light of far-off stars is dimmed and reddened. In order to reduce our observations for this effect, we have to find how this extinction depends on wavelength; our results will also help to understand the ...
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1987
Matter is present in the Galaxy not only in the form of stars. Characteristic absorption lines in all wavelength ranges reveal the presence of gas scattered throughout space between stars. In addition to the gas, Trumpler has shown that in the galactic disk, dust produces a dimming of the light coming from distant stars, and modifies the energy ...
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Matter is present in the Galaxy not only in the form of stars. Characteristic absorption lines in all wavelength ranges reveal the presence of gas scattered throughout space between stars. In addition to the gas, Trumpler has shown that in the galactic disk, dust produces a dimming of the light coming from distant stars, and modifies the energy ...
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Interstellar Extinction and Diffuse Absorption Features
Astrophysics and Space Science, 1975The equivalent width of the λ 2175 A band, W 2175, well known as the big bump in the interstellar extinction curves, has been found to be closely correlated with the colour excess E B-V as well as with the extinction differences E 8−6 and E 8−6 defined to characterize quantitatively the steep slopes of the extinction curves in the far ultraviolet.
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1987
Many observations became understandable only when astronomers realized that there are huge clouds of gas and dust in interstellar space, by which the light of far-off stars is dimmed and reddened. In order to reduce our observations for this effect, we have to find how this extinction depends on wavelength; our results will also help to understand the ...
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Many observations became understandable only when astronomers realized that there are huge clouds of gas and dust in interstellar space, by which the light of far-off stars is dimmed and reddened. In order to reduce our observations for this effect, we have to find how this extinction depends on wavelength; our results will also help to understand the ...
openaire +1 more source