Radiative Transfer in Protoplanetary Disks

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Ring Radius (AU) 100.00 10.00 1.00 0.10 0.01 Inner radius ot T Tauri stars Radii inferred from interferometry larger than predicted HAe Objects HBe Objects TTS Objects Sublimation radius: direct dust heating, backwarming Sublimation radius: direct dust heating, no backwarming Sublimation radius: standard model CTTS 10 0 10 0 10 0 Sublimation radius Herbig Ae 10 2 10 2 10 2 Lstar + Laccretion (Lsolar) 10 4 10 4 10 4 1000K 1000K 1000K 1000K 1000K 1500K 1500K 1500K 1500K 1500K 1500K 1000K 1000K 1000K 1500K 1500K 1500K 10 6 10 6 10 6 Direct heating of inner dust disk Star (magnetospheric accretion?) optically!thin gas (puffed!up inner wall?) Dust Sublimation Radius R s "Standard" Disk Model ! oblique disk heating Star (magnetospheric accretion?) optically!thick gas Dust Sublimation Radius R s Fig. 2.— Measured sizes of HAeBe and T Tauri objects vs. central luminosity (stellar + accretion shock); and com sublimation Millan-Gabet radii for dust directly et heated heatedal by by2006 the central luminosity (solid and dashed lines) and for the oblique heating i classical models (dotted line). A schematic representation ofthekeyfeaturesofinnerdiskstructureinthesetwoclasses f flared flared flared disk disk disk
Ring Radius (AU) 100.00 10.00 1.00 0.10 0.01 Inner radius ot T Tauri stars Radii inferred from interferometry larger than predicted HAe Objects HBe Objects TTS Objects Sublimation radius: direct dust heating, backwarming Sublimation radius: direct dust heating, no backwarming Sublimation radius: standard model CTTS 10 0 10 0 10 0 Sublimation radius Herbig Ae 10 2 10 2 10 2 Lstar + Laccretion (Lsolar) 10 4 10 4 10 4 1000K 1000K 1000K 1000K 1000K 1500K 1500K 1500K 1500K 1500K 1500K 1000K 1000K 1000K 1500K 1500K 1500K 10 6 10 6 10 6 Star accretional Direct heating of inner dust disk heating? lower sublimation optically!thin gas temperature? (magnetospheric accretion?) smaller dust grains? photoevaporation? optically!thick gas magnetospheric Dust Sublimation truncation? (puffed!up inner wall?) Dust Sublimation Radius R s "Standard" Disk Model ! oblique disk heating Star (magnetospheric accretion?) Radius R s scattered light? Fig. 2.— Measured sizes of HAeBe and T Tauri objects vs. central luminosity (stellar + accretion shock); and com sublimation Millan-Gabet radii for dust directly et heated heatedal by by2006 the central luminosity (solid and dashed lines) and for the oblique heating i classical models (dotted line). A schematic representation ofthekeyfeaturesofinnerdiskstructureinthesetwoclasses f flared flared flared disk disk disk
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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 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 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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