Observational Constraints on The Evolution of Dust in ...

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126 Discovery of a Dusty Planetary Nebula Table 5.1 – Emission lines identified in the IRS spectrum of OL17 (Figure 5.1). λ Line EW Flux (µm) (µm) (erg/s/cm 2 ) 8.99 [Ar iii] 0.08 6.15 × 10 −15 10.51 [S iv] 2.91 1.26 × 10 −13 13.07 [Ar v] 0.14 6.89 × 10 −15 14.32 [Ne v] 3.23 1.88 × 10 −13 15.56 [Ne iii] 1.11 8.30 × 10 −14 18.71 [S iii] 0.23 2.03 × 10 −14 24.32 [Ne v] 1.45 1.92 × 10 −13 25.89 [O iv] 13.64 2.81 × 10 −12 33.48 [S iii] 0.31 3.80 × 10 −14 Table 5.2 – Optical R-band magnitude and Spitzer IRAC/MIPS fluxes of OL17 (see also Figure 5.2). R † 3.6 µm 4.5 µm 5.8 µm 8.0 µm 24.0 µm (mag) (mJy) (mJy) (mJy) (mJy) (mJy) 22.8 0.28 0.64 0.80 2.29 69.60 † From Spezzi et al. 2010. Table 5.3 – Major emission lines identified in the X-shooter spectra (Figure 5.3). Equivalent widths (EW) given indicate (3σ) lower limits, due to the faintness of the continuum. λ Line EW λ Line EW (Å) (Å) (Å) (Å) 4959 [O iii] 1.4 10831 He i 196.1 5007 [O iii] 5.1 10938 H i 125.7 6563 Hα 47.1 11627 He ii 100.4 7135 [Ar iii] 2.6 12818 H i 290.5 8236 He ii 2.9 16112 O i 21.9 9014 H i 2.4 16918 Al ii 25.6 9069 [S iii] 18.8 17364 Ne ii 66.0 9229 H i 5.5 18176 Ne ii 88.1 9531 [S iii] 43.4 18638 Ne ii 183.4 9546 H i 22.2 18754 N ii 564.4 10049 H i 5.4 21657 Br γ 597.1 10123 He ii 228.5
6 On the Evolution of Dust Mineralogy: from Protoplanetary Disks to Planetary Systems Mineralogical studies of silicate features emitted by dust grains in protoplanetary disks and Solar System bodies can shed light on the progress of planet formation. The significant fraction of crystalline material in comets, chondritic meteorites and interplanetary dust particles indicates a modification of the almost completely amorphous interstellar medium (ISM) dust from which they formed. The production of crystalline silicates, thus, must happen in protoplanetary disks, where dust evolves to build planets and planetesimals. Different scenarios have been proposed, but it is still unclear how and when this happens. This paper presents dust grain mineralogy (composition, crystallinity and grain size distribution) of a complete sample of protoplanetary disks in the young Serpens cluster. These results are compared to those in the young Taurus region and to sources that have retained their protoplanetary disks in the older Upper Scorpius and η Chamaeleontis stellar clusters, using the same analysis technique for all samples. This comparison allows an investigation of the grain mineralogy evolution with time for a total sample of 139 disks. The mean cluster age and disk fraction are used as indicators of the evolutionary stage of the different populations. Our results show that the disks in the different regions have similar distributions of mean grain sizes and crystallinity fractions (∼10 – 20%) despite the spread in mean ages. Furthermore, there is no evidence of preferential grain sizes for any given disk geometry, nor for the mean cluster crystallinity fraction to increase with mean age in the 1 – 8 Myr range. The main implication is that a modest level of crystallinity is established in the disk surface early on (≤ 1 Myr), reaching an equilibrium that is independent of what may be happening in the disk midplane. These results are discussed in the context of planet formation, in comparison with mineralogical results from small bodies in our own Solar System. Isa Oliveira, Johan Olofsson, Klaus M. Pontoppidan, Ewine F. van Dishoeck, Jean-Charles Augereau & Bruno Merín The Astrophysical Journal, 2011, in press
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Observational <str
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Promotiecommissie Promotor: Co-Prom
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Cover Artwork: Roderik Overzier
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viii Chapter 3. YSOs in the Lupus M
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x Publications 217 Acknowledgments
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2 Introduction planets may eventual
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20 Introduction Gorti, U., Dullemon
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2 Optical Characterization of a New
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Evolution of Dust in Protoplanetary
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