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Radiative Transfer in Protoplanetary Disks

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Introduction Activités Activités de de recherche recherche Projet Projet de de recherche recherche Résumé Résumé<br />

Un Un exemple exemple : IM : IMLup, Lup, une une CTTS CTTStypique typique<br />

Multi-λ modell<strong>in</strong>g of IM Lupi<br />

Modélisation du dudisque disque d’IM Lup P<strong>in</strong>te et etal, al, 2008b, A&A<br />

!.F! (W.m−2 !.F! (W.m<br />

)<br />

−2 )<br />

A s<strong>in</strong>gle model with mild stratification remarkably reproduces<br />

all Un Un observations: unique modèle H(1mm) avec une une ≈ 0.5 faible H(1μm) stratification<br />

reproduit remarquablement bien l’ensemble des données<br />

WFPC2 bien l’ensemble 0.6 μm des données<br />

1’’<br />

E<br />

N<br />

1.0<br />

WFPC2 0.6 0.6 µm µm<br />

SMA SMA1.3 1.3mm mm<br />

10−12 10−12 10−14 10−14 2<br />

2<br />

10−16 10−13 10−16 10−13 5.<br />

5.<br />

10.0<br />

10.0<br />

20.<br />

20.<br />

1.0<br />

1.0<br />

10.0<br />

10.0<br />

100.0<br />

100.0<br />

1000.<br />

1000.<br />

! (µm) ! (µm)<br />

⇓⇓<br />

Mdisque, croissanceet<br />

Mdust,<br />

croissanceet<br />

gra<strong>in</strong> growth<br />

sédimentation<br />

& settl<strong>in</strong>g<br />

➜<br />

10 C. P<strong>in</strong>te et al.: Prob<strong>in</strong>g dust gra<strong>in</strong> evolution <strong>in</strong> IM<br />

1’’<br />

1’’<br />

E<br />

E<br />

N<br />

Nicmos<br />

Nicmos 1.6<br />

1.6<br />

Nicmos 1.6 µm µm<br />

μm<br />

Obs Modèles<br />

Model<br />

⇓<br />

F" (Jy)<br />

F" (Jy)<br />

F" (Jy)<br />

F" (Jy)<br />

0.2<br />

0.2<br />

0.1<br />

0.1<br />

0.05<br />

0.05<br />

0.02<br />

0.02<br />

0.01<br />

0.01<br />

0.005<br />

0.005<br />

p=0 p=0 p=1 p=1<br />

ATCA 3.3 3.3 mm mm<br />

p=2 p=2<br />

p=0 p=0<br />

0 50 100<br />

0 50 100<br />

Basel<strong>in</strong>e<br />

Basel<strong>in</strong>e<br />

(k!)<br />

(k!)<br />

p=2 p=2<br />

p=1 p=1<br />

⇓<br />

Densité de surface<br />

Σ(r) ∝ r −p<br />

⇓<br />

Densité de surface<br />

Σ(r) ∝ r −p<br />

Surface density<br />

Σ(r) α r-p Coll. Coll. Grenoble (Ménard, Augereau, Duchêne), JPL/Caltech (Padgett,Stapelfeldt),<br />

P<strong>in</strong>te et al 2008<br />

Arizona (Schneider), Leiden Leiden (Panić, van vanDishoeck), Dishoeck), Spitzer Legacy Team Teamc2d c2d<br />

N<br />

Brightness profile<br />

0.5<br />

0.0<br />

0 90 180 270<br />

Azimuthal angle ( o )<br />

Fig. 8. Scattered light images of the best models compared to observations. L<br />

at 0.606 µm andthelowerrowtothoseat1.6µm. Synthetic maps (right) w<br />

from theRext, peak). Rext, Central i, i, H0<br />

H0panel:<br />

0.6 µm azimuthalbrightnessprofile.Right<br />

central Rout, and right i, Ho, panels, gra<strong>in</strong> the red dashed l<strong>in</strong>e correspond to the best fit of the<br />

of all observations simultaneously and the blue dotted to the scatteredlight<br />

<strong>in</strong> the front side of the disc, i.e. towards bottom <strong>in</strong> the first panel.<br />

➜<br />

size, composition<br />

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