2008/12/10 by Jian Gao, Biwei Jiang, B. W. Jiang +1 · 1 citation
Chemistry · Earth and Planetary Sciences · Physics and Astronomy · #Absorption (acoustics) #Amorphous solid #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Atmospheric Ozone and Climate #Chemistry #Cosmic dust #Crystallography #Extinction (optical mineralogy) #Feature (linguistics) #Galactic Center #Galaxy #Interstellar medium #Materials science #Optics #Physics #Silicate #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.5047/eps.2008.12.006
published as Earth Planets Space 62:61-67,2010 · 6 pages, 6 figures, uses eps.cls. Accepted for publication in "Earth, Planets and Space" (special issue on Cosmic Dust)
arxiv created 2008/12/10 · openalex publication_date 2010/01/01 · arxiv updated 2014/11/18 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Observationally, both the 3.4μm aliphatic hydrocarbon C-H stretching absorption feature and the 9.7μm amorphous silicate Si-O stretching absorption feature show considerable variations from the local diffuse interstellar medium (ISM) to Galactic center (GC): both the ratio of the visual extinction (AV) to the 9.7μm Si-O optical depth (Δτ 9.7 μm ) and the ratio of A V to the 3.4 μm C-H optical depth (Δτ 3.4 μm ) of the solar neighborhood local diffuse ISM are about twice as much as that of the GC. In this work, we try to explain these variations in terms of a porous dust model consisting of a mixture of amorphous silicate, carbonaceous organic refractory dust (as well as water ice for the GC dust).