Radiative Transfer in Protoplanetary Disks

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Light scattering: anisotropy 56 2.6.4 Quelques remarques sur la distribution angulaire de rayonnement Polarisability depends on grain size S11 S11 0.012 0.010 0.008 10 +0 10 −2 10 −4 2πa λ 0.012 =0.01 2πa λ =0.1 0 90 180 0.010 0.008 10 −2 10 −4 0 90 180 1.5 10 −2 8.0 6.0 10 +0 10 +0 2πa λ = 10 2πa λ = 100 2πa λ angle de diffusion ( ◦ ) angle de diffusion ( ◦ ) 10 −2 2πa λ =1 = 1000 10 0 90 180 −4 angle de diffusion ( ◦ ) Figure 2.8 – Comparaison entre la fonction de phase calculée par la théorie de Mie (ligne pleine) Mie theory grain size distribution dn(a) α a et la fonction de Henyey-Greenstein (ligne en tirets) de même premier moment g = 〈cos θ〉 -3.5 da
The case of GG Tau •A 0.13M, 180AU-radius circumbinary ring •Clear detection of the ring in scattered light •Morphology extremely similar to visible image ISM dust models match the visible Image with i ! 40 o HST (0.8µm) Krist et al. (2002) Keck AO (3.8µm) Duchêne et al. (2004) 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 24: A first direct evidence Scattered l
Page 27 and 28: G Tau : un anneau stratifié Tau :
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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