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Table 7
Comparison continued from previous table.
| Characteristics of | Characteristics of | Ratio(R) | Observational | |
| 10 μm feature | 18 μm feature | 18 μm/10 μm | characteristics | |
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| Our work | Shifts shortwards with | No shift in this | R Decreases with | Dust temperatures 200–350 K |
| (2010) | graphite inclusions | feature is indicated | volume fractions of | are derived from composite |
| & no broadening of | graphite; increases | grain models fit the | ||
| this feature is | with porosity & | observed IRAS-LRS curve | ||
| indicated | varies between 0.2–0.6 | as well as for 2 stars | ||
| selected in this paper | ||||
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| Lee & | No shift is indicated | Not studied | R not determined | Core-mantle grain model fit |
| Draine (1985) | well with the observed | |||
| IR emission from BN object | ||||
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| Jones | Feature is | Feature is | R not determined | No comparison was made |
| (1988) | enhanced | enhanced | ||
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| Greenberg | Grains with silicate cores | This feature | R not determined | Pure silicate does not fit |
| & Hage (1990) | & refractory organic | was not | the observed emission in | |
| materials as mantles | studied | comets but porous grains | ||
| with ~60–80% porosity | and CHON particles fit the | |||
| fit the 10 μm feature | observed IR emission from | |||
| observed in comets | cometary dust | |||
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| Ossenkopf | Feature shifts shortwards | Did not find | R ~ 0.3–0.5 | Grain models based on optical |
| et al. (1992) | (~0.3 μm) & broadens | any shift in | for most inclusions | constants of |
| (FWHM 2–2.7 μm) | this feature | & is enhanced to | astronomical Si (Draine 1985) | |
| with Al2O3 inclusions | 0.68 for MgO | do not fit the observed | ||
| observed IR emission from | ||||
| circumstellar dust | ||||
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| Henning & | No appreciable shift | Feature shifts | R ~ 0.41–0.47 | Porous and composite grains |
| Stognienko (1993) | with inclusions | shortwards and | do not fit the observed | |
| indicated | broadens with | IR emission from AFGL 2591 | ||
| amorphous carbon | or BN objects | |||
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| O’Donnell | No shift in this | No shift in | R = 0.51 for prolates | The silicate grains which give rise |
| (1994) | feature with | this feature | R = 0.42 for oblates | to the 10 μm & 18 μm features do not |
| inclusions indicated | with inclusions | Observed R value | posses any coatings of | |
| is indicated | is between 0.3–0.6 | amorphous or glassy carbon | ||
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| Min et al. | Feature shifts shortwards | No shift in | R not determined | GRF, DHS and irregularly |
| (2007) | (~0.5 μm) & broadens | this feature | shaped particles fit | |
| (FWHM 2–2.5 μm) | the interstellar spectrum | |||
| in the region 5–25 μm | ||||
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| Voshchinnikov | The strength of this | This feature | R not determined | Porous and fluffy grain |
| & Henning (2008) | feature decreases with | was not | models fit the observed | |
| the porosity and the | studied | 10 μm feature in | ||
| feature also broadens | T-Tauri & Herbig Ae/Be stars | |||
| (FWHM 2.1–2.7 μm) | ||||
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| Li et al. | This feature shifts to longer | This feature | R not determined | Observed 10 μm feature |
| (2008) | wavelengths (~10.6 μm) | was not | can be explained in | |
| & the profile broadens | studied | terms of porous composite | ||
| (FWHM 2.1–2.8 μm) | dust consisting of | |||
| with porosity | amorphous Si and C & vacuum | |||
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