Radiative Transfer in Protoplanetary Disks

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≈ 400 000 models Some parameters fixed from data (amax, Mdust, Rout) →Fitting for 6 parameters IM Lupi: quantitative constraints Bayesian method to estimate model parameters: for SED + mm visibilities + scattered light images Pinte et al 2008 Probability Probability Probability Probability Probability Probability 1.0 0.5 0.0 1.0 0.6 0.4 0.2 0.5 cos(i) 0.0 0.05 0.1 0.2 0.5 1.0 rin 1.0 0.5 0.0 0.0 1.0 0.5 0.0 0 −1 −2 5 10 15 1.0 0.5 0.0 0.6 0.4 0.2 1.0 1.1 1.2 surface density flaring 0.0 0.00 0.05 0.10 0.15 0.20 H stratification See also Glauser et al 2008, Bouy et al 2008, Duchêne et al 2010
• Gas represents 99% of the disk mass • Difficult to observe but Herschel is opening the far-IR window • Gas & dust evolution strongly coupled Gas and Dust Evolution Gas & Dust evolution VIMOS Multi-object Spectroscopy and Spitzer/IRA Fedele et al. 2009 Fedele et al. (2009, Poster A 31)
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Radiative Transfer in Protoplanetar
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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 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: ≈ 400 000 models Some parameters
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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