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- W2187145812 abstract "−3.2 0 + 0.7 12.9 ± 1.4 HD 69830 16.8 ± 3.7 20.0 ± 0.9 0 + 0.7 1.9 +9.0 −1.9 20.9 ± 5.1 4.6 ± 0.7 8.1 ± 1.9 7.0 ± 4.2 20.8 ± 4.1 BD+20 307 48.2 ± 1.0 10.5 ± 0.9 0 + 0.7 8.7 ± 0.7 14.0 ± 1.6 2.7 ± 1.0 15.9 ± 0.7 0 + 0.7 0 + 0.7 HD 15407 A 0 + 0.7 13.5 ± 5.8 14.7 ± 5.0 0 + 0.7 0 + 0.7 0 + 0.9 0 + 0.8 51.9 ± 1.6 19.8 ± 10.2 HD 169666 0 + 0.8 0 + 0.7 0 + 0.7 35.8 ± 0.9 0 + 0.9 20.0 ± 7.9 22.2 ± 0.9 10.3 ± 0.7 11.6 ± 4.6 HD 98800 B 15.3 ± 0.7 43.0 ± 0.7 0 + 0.7 7.4 ± 1.2 0 + 0.8 0.8 ± 0.7 15.7 ± 5.2 0 + 0.7 17.8 ± 5.3 ID 8 27.8 ± 8.2 0 + 0.7 0 + 0.7 51.2 ± 11.7 7.5 ± 2.7 1.7 +1.8 −1.7 0 + 0.7 0 + 0.7 11.8 ± 2.0 is propagated only to the relative abundances. We used smax of 1 μm and 1 mm for crystalline and amorphous grains, respectively. Therefore, Δlogs (and thusn) being smaller for crystalline species, their relative abundances increase with respect to amorphous grains. The trends between different crystalline (or amorphous) grains however remain the same (e.g., Fe-rich versus Mgrich crystalline olivine grains), since they have the same Δlogs. Consequently, the best fit parameters remain the same, as well as the best fit models, only the final relative abundances of the dust species required to fit the observed spectrum are modified. Table 1 shows the correct abundances as well as the newly estimated uncertainties for the dust composition. The crystallinity fractions with respect to the amorphous phases are different (higher crystallinity fractions), but the observed trends between crystalline (or amorphous) grains are still valid. All the results and conclusions discussed in the rest of the study therefore remain unchanged." @default.
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- W2187145812 date "2012-01-01" @default.
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- W2187145812 title "Transient dust in warm debris disks Detection of Fe-rich olivine grains (Corrigendum)" @default.
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