Observational Constraints on The Evolution of Dust in ...

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66 YSOs in the Lupus Molecular Clouds Figure 3.10 – Continuum subtracted, normalized profiles of the Hα emission lines (black line) overplotted with a Gaussian fit (gray solid line). The red dotted line marks the centre of the Gaussian fit and the horizontal gray line marks the width at 10% intensity.
Evolution of Dust in Protoplanetary Disks 67 Figure 3.11 – Sample of continuum subtracted, normalized profiles of the Hα emission lines overplotted with a Gaussian fit (light gray solid line) and a Voigt fit (dark gray solid line). The red dotted line marks the center of the Gaussian fit. Figure 3.12 – Histogram of the mass accretion rates derived from the Hα[10%] value. The shaded area are objects out of the range for which the relationship of Natta et al. (2004) was calibrated. Those objects are generally classified as non-accreters.
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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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118 Discovery of a Dusty Planetary
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128 From Protoplanetary Disks to Pl
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Nederlandse Samenvatting Inleiding
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193 Figuur 1 - Het ontstaan van een
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195 kunnen worden om de verschillen
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197 Figuur 3 - Het planeetvormingsp
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199 parameter is. Na 6 tot 8 miljoe
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201 van de X-shooter in het ultravi
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Resumo em Português Restrições O
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205 Figura 1 - Ilustração do cen
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207 Figura 2 - O Telescópio Espaci
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209 interagem gravitacionalmente, a
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211 e discos são conectados, é ba
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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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