Abstract
The large-scale brightness of most of the sky at wavelengths from 10 µm to 30 µm is dominated by thermal emission from interplanetary dust. Measurement of this ‘zodiacal emission’ has long been of interest for many reasons. The IRAS survey has provided comprehensive brightness measurements in the infrared, covering the celestial sphere with solar elongation angles ranging from 60° to 120°. These data have stimulated numerous approaches to segregation and modeling of the zodiacal emission. Current models provide a reasonable basis for study of the interplanetary dust, but are severely stressed when one wishes to know the ‘residual’ sky brightness. The nature, status, and implications of various models are reviewed.
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© 1988 Springer-Verlag
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Hauser, M.G. (1988). Models for infrared emission from zodiacal dust. In: Lawrence, A. (eds) Comets to Cosmology. Lecture Notes in Physics, vol 297. Springer, Berlin, Heidelberg. https://doi.org/10.1007/BFb0118784
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DOI: https://doi.org/10.1007/BFb0118784
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