Radiative Transfer in Protoplanetary Disks

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- Timescale for gas dispersal and planet formation? - Grain growth and settling ? - Relative evolution of dust and gas ? Text From clouds to envelopes, to disks, to planets ?
Processes in Protoplanetary disks Processes in Protoplanetary Disks © Peter Woitke
Page 1 and 2: Radiative Transfer in Protoplanetar
Page 3: Text From clouds to envelopes, to d
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 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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