Book Chapter10.1007/1-4020-3844-5_11
The Cool Interstellar Medium
Alain Abergel,Laurent Verstraete,Christine Joblin,René J. Laureijs,Marc-Antoine Miville-Deschenes +4 more
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TL;DR: In this paper, the authors review the ISO results on the cool and low-excitation regions of the interstellar medium, where T gas≲ 500 K, nH ∼ 100−105 cm−3 and the electron density is a few 10−4.
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Abstract: Infrared spectroscopy and photometry with ISO covering most of the emission range of the interstellar medium has led to important progress in the understanding of the physics and chemistry of the gas, the nature and evolution of the dust grains and also the coupling between the gas and the grains. We review here the ISO results on the cool and low-excitation regions of the interstellar medium, where T gas≲ 500 K, nH ∼ 100–105 cm−3 and the electron density is a few 10−4.
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2
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References
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TL;DR: In this article, the average extinction law over the 3.5 micron to 0.125 wavelength range was derived for both diffuse and dense regions of the interstellar medium. And the validity of the law over a large wavelength interval suggests that the processes which modify the sizes and compositions of grains are stochastic in nature.
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A survey of interstellar H I from L-alpha absorption measurements. II
TL;DR: The Copernicus satellite surveyed the spectral region near L alpha to obtain column densities of interstellar HI toward 100 stars as discussed by the authors, and the value of the mean ratio of total neutral hydrogen to color excess was found to equal 5.8 x 10 to the 21st power atoms per (sq cm x mag).
Interstellar dust grains
TL;DR: In this article, the authors survey the observed properties of interstellar dust grains: the wavelength-dependent extinction of starlight, including absorption features, from UV to infrared; optical luminescence; and optical luminance.
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Dust Grain Size Distributions and Extinction in the Milky Way, LMC, and SMC
TL;DR: In this paper, the authors construct size distributions for carbonaceous and silicate grain populations in different regions of the Milky Way, LMC, and SMC, and adopt a fairly simple functional form for the size distribution, characterized by several parameters.
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