Observational Constraints on The Evolution of Dust in ...

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164 From Protoplanetary Disks to Planetary Systems ID Oli/Pyr a % Ens % For % Sil % Oli/Pyr a % Sil % (1.5 µm) (1.5 µm) (1.5 µm) (1.5 µm) (6.0 µm) (6.0 µm) PBB2002 J161420.2 67.7 +7.9 −7.8 0.6 +0.9 −0.0 0.8 +1.2 −0.0 0.0 +0.4 −0.0 15.2 +2.8 −1.5 7.9 +1.3 −1.3 PZ99 J160357.6 6.1 +9.2 −0.0 3.8 +2.9 −0.0 0.2 +2.2 −0.0 0.0 +2.6 −0.0 87.1 +19.9 −46.7 0.0 +5.1 −0.0 PZ99 J161411.0 8.8 +4.7 −0.0 3.9 +3.5 −0.0 0.0 +1.4 −0.0 0.0 +4.1 −0.0 84.8 +8.6 −55.2 0.0 +3.0 −0.0 ScoPMS31 72.4 +39.8 −61.0 4.6 +10.7 −3.7 0.0 +9.0 −1.9 1.9 +9.2 −1.4 6.6 +4.2 −6.2 0.0 +1.5 −0.0 η Chamaeleontis J0843 44.6 +19.9 −21.9 5.9 +7.6 −0.0 0.0 +10.2 −0.0 1.6 +11.6 −0.0 13.6 +19.2 −0.0 0.0 +3.9 −0.0 RECX-5 12.3 +15.6 −3.5 23.9 +13.9 −0.0 0.0 +8.0 −0.0 8.0 +6.9 −3.3 7.1 +18.9 −0.0 0.0 +10.0 −0.0 RECX-9 31.6 +15.8 −24.2 0.9 +7.0 −0.0 5.4 +5.8 −3.2 4.6 +10.8 −2.1 3.3 +3.0 −1.1 0.8 +8.3 −0.0 RECX-11 26.8 +15.7 −14.4 8.0 +10.5 −0.0 0.0 +2.7 −0.0 3.4 +3.7 −1.9 17.6 +8.1 −6.6 0.0 +1.9 −0.0 Table A.2 – Intermediate and large dust composition derived using the “B2C” procedure. b a Amorphous olivine and pyroxene combined. b For each object, the first line corresponds to the warm component abundances, while the second line corresponds to the cold component abundances, when available.
7 Spectral Energy Distributions of the Young Stars with Disks in Serpens We present the spectral energy distributions (SEDs) of the young stars surrounded by disks in the Serpens Molecular Cloud. The SEDs allow a correct separation between the stellar radiation from that re-emitted by the disks. Taking into account the distance of 415 pc, the distribution of ages is shifted to lower values, in the 1 – 3 Myr range, with a tail up to 10 Myr. The mass distribution varies between 0.2 and 1.2 M ⊙, with median mass of 0.7 M ⊙. The distribution of fractional disk luminosities resembles that of the young Taurus Molecular Cloud, with most disks consistent with passively irradiated disks. The actively accreting and non-accreting stars show very similar distributions in fractional disk luminosities, differing in the brighter tail. Comparison with a sample of Herbig Ae/Be stars shows that the T Tauri disks do not show the clear separation in fractional disk luminosities for different geometries as seen for disks around the more massive Herbig Ae/Be. Furthermore, the results for the mineralogy of the dust in the disk surface do not seem to be directly related to either stellar or disk characteristics. Isa Oliveira, Bruno Merín, Ewine F. van Dishoeck, Klaus M. Pontoppidan In preparation
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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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4 Introduction Figure 1.1 - Illustr
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6 Introduction 1.3.1.1 Disk Observa
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8 Introduction 1.3.1.3 Processes Af
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10 Introduction of them (e.g., β P
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12 Introduction responsible for dis
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14 Introduction Figure 1.4 - Eviden
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16 Introduction stars (due to spect
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18 Introduction the potential to ch
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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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52 YSOs in the Lupus Molecular Clou
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4 A Spitzer Survey of Protoplanetar
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A. Background Sources 111 Table 4.3
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216 Curriculum Vitæ omy Center (ES
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218 Publications 8. c2d Spitzer-IRS
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220 Thesis Acknowledgments Liesbeth
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