Steps toward interstellar silicate mineralogy - VI. Dependence of crystalline olivine IR spectra on iron content and particle shape

By D. Fabian, T. Henning, C. Jäger, H. Mutschke, J. Dorschner, O. Wehrhan. 2001

225 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Atmospheric Science

View Paper: https://www.semanticscholar.org/paper/746af6c81a5c844ebaea9925634fa7f41c19bf7e

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In Astronomy and Astrophysics

1. M. Galametz
2. F. Galliano
3. S. Madden
4. A. Tielens
5. K. Gordon
6. B. Whitney
7. W. Koeppen
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In Atmospheric Science

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2. B. Whitney
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6. Marvin L. Cohen
7. K. Gordon
8. V. Hamilton

Citations in the corpus

• Spitzer IRS Spectroscopy of IRAS-discovered Debris Disks (2006, background): “1SiO4, Fabian et al. 2001), crystalline enstatite (MgSiO3, Jaeger et al. 1998), and amorphous carbon (Zubko et al. 1996), and Bruggeman Effective Medium Theory (Bohren & Huffman 1983).”
• Thermal infrared (vibrational) spectroscopy of Mg–Fe olivines: A review and applications to determining the composition of planetary surfaces (2010, methodology): “To enable better analysis of circumstellar dust spectra, Fabian et al. (2001) undertook a study to compare the calculated mass absorption coefficients for randomly oriented ellipsoidal particles, spheres, and distributions of ellipsoids to measured powder spectra of olivine.”
• The SAGE-Spec Spitzer Legacy Program: The Life Cycle of Dust and Gas in the Large Magellanic Cloud (2010, background): “O stretching mode from corundum (Al2O3) or spinel (MgAl2O3) grains (Posch et al. 1999; Fabian et al. 2001; Sloan et al. 2003; Lebzelter et al. 2006).”
• A 10 μm spectroscopic survey of Herbig Ae star disks: Grain growth and crystallization (2005, background): “Furthermore, a comparison between calculations of the mass absorption coefficients of small crystalline silicates with measurements shows that we cannot get good agreement using homogeneous spherical particles (see for example Fabian et al. 2001).”
• Global distribution, composition, and abundance of olivine on the surface of Mars from thermal infrared data (2008, methodology): “The resulting density profile is gravitationally unstable and will reorganize to achieve a gravitationally stable interior placing Mg-rich olivine near the surface and Fe-rich olivine at depth [ Elkins-Tanton et al., 2005 ].”