Radiative Transfer in Protoplanetary Disks

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atified model can reproduce all observations at once GG Tau: models with dust stratification ts Models with Observations Models without dust settling Observations Models without dust settling with dust dust settling > 5µm Pinte et al. (2007) Christophe Pinte An in-depth look at protoplanetary disks
G Tau : un anneau stratifié Tau : un anneau stratifié Pinte et al, 2007, Pinte et al, 2007, A&A G Tau : un anneau stratifié Pinte et al, 2007, A&A GG Tau: a stratified ring Images en lumière diffusée entre 0.5 et 3.8 µm mages en lumière diffusée entre 0.5 et 3.8 µm Images Stratification en lumière permet diffusée de entre les reproduire 0.5 et 3.8 µm simultanément Model with stratification reproduces images from 0.5 to 3.8μm Stratification permet de les reproduire simultanément Obs Models Modèles tratification permet de les reproduire simultanément Obs Modèles Obs Modèles paramétrique paramétrique paramétrique Lyon (Gonzalez) & Lyon Lyon (Gonzalez) (Gonzalez) & & Berne (Fouchet) Berne Berne (Fouchet) (Fouchet) hydro modélisation hydrodynamique hydr hydro modélisation modélisation hydrodynamique hydrodynamique +transfertradiatif +transfertradiatif +transfertradiatif SPH simulations (Fouchet, Gonzalez, Lyon) + radiative transfer Pinte et al 2007 Christophe Pinte Formation et évolution des systèmes planétaires 8/14 Christophe Pinte Formation et évolution des systèmes planétaires Christophe Pinte Formation et évolution des systèmes planétaires 8/1
Page 1 and 2: Radiative Transfer in Protoplanetar
Page 3 and 4: Text From clouds to envelopes, to d
Page 5 and 6: Processes in Protoplanetary disks P
Page 12: Why the need for Monte Carlo? • m
Page 16: Small grains IR spectroscopy with S
Page 22 and 23: Light scattering: anisotropy 56 2.6
Page 24: A first direct evidence Scattered l
Page 29 and 30: Evidence of non spherical grains
Page 32 and 33: Polarisability of dust grains Unres
Page 34: ect of chemical composition / poros
Page 40 and 41: odeling of disks . polarisation can
Page 42 and 43: Another example: AU Mic HST 0.606
Page 44: Unresolved polarimetry: tomography
Page 47: i mary: Tomography of the inner dis
Page 54 and 55: Ring Radius (AU) 100.00 10.00 1.00
Page 56 and 57: Ring Radius (AU) 100.00 10.00 1.00
Page 59 and 60: !.F! (W.m ) hy should should we we
Page 61 and 62: Introduction MCFOST IM Lup GG Tau I
Page 63 and 64: ≈ 400 000 models Some parameters
Page 65 and 66: ≈ 400 000 models Some parameters
Page 67 and 68: • Gas represents 99% of the disk
Page 69 and 70: Modelling tools: MCFOST + ProDiMo I
Page 71: Modelling tools: the DENT grid Grid
Page 77 and 78:
Spatial origin of the lines HD 1691
Page 79 and 80:
[OI] 63 µm [W.m −2 ] Effect of X
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Radiative Transfer in Protoplanetary Disks

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