Observing inner discs where planets formFrom discs to planets: New observations, models, and theoriesPasadena, California, USARégis Lachaume1, Fabien Malbet2, & Jean-Louis Monin21Max-Planck-Institut für Radioastronomie2Laboratoire d’Astrophysique de GrenobleMarch 8th 2005IntroductionScales in protoplanetary discs0.10.00110.01100.11001AU’’distance to the star@ TaurusKuchner 2004, ApJ 612, 1147Earth Plutoopticalradiogiant planet formationlarge column density:→ Optical interferometry & radiative transferScales in protoplanetary discs0.10.00110.01100.11001AU’’distance to the star@ Taurus1001000 101000 100 m (N band)m (K band)baseline lengthEarth Plutoopticalradio→ Optical interferometry & radiative transferBut visibilities are are not enough! (1)Irradiated & visous disc model for T Tauri: visibility fit.Lachaume, Malbet, & Monin 2003, A&A 379, 515 0 50 100 1500.00.51.0 B (m)|V2| (norm.)˙M = 8.0 × 10−7M/yr rmin= 18.0 R→ Combine observables, e.g. SED + visibilitiesBut visibilities are are not enough! (1)Irradiated & visous disc model for T Tauri: visibility fit.Lachaume, Malbet, & Monin 2003, A&A 379, 515 0 50 100 1500.00.51.0 B (m)|V2| (norm.)1.0 10.0 100.010−1310−1210−11 λ (µm)λFλ (W.m−2)˙M = 8.0 × 10−7M/yr rmin= 18.0 R→ Combine observables, e.g. SED + visibilitiesBut visibilities are are not enough! (2)The large-scale diffuse emission problemLachaume, 2003, A&A 400, 795diffuse emissioncompact objectvisibilitybaselinewrong diameter→ Adaptive optics & speckle interferometryBut visibilities are are not enough! (2)The large-scale diffuse emission problemLachaume, 2003, A&A 400, 795diffuse emissioncompact objectvisibilitybaselinewrong diameter→ Adaptive optics & speckle interferometryAd hoc modellingAMBER observation of MWC 297Herbig Be starResolved in K, Tatulli 2005, Ph.D. thesis 2.14 2.16 2.180.00.51.0 2 4 6 8Wavelength (micron)VisibiliyFlux (kADU/ch/s)continuum Br γdiscenvelopeØdisc= 5.8 ± 0.6 mas → 2.6 ± 0.3 AUØenv= 10.6 ± 0.8 mas → 4.8 ± 0.4 AUAMBER observation of MWC 297Herbig Be starResolved in K, Tatulli 2005, Ph.D. thesis 2.14 2.16 2.180.00.51.0 2 4 6 8Wavelength (micron)VisibiliyFlux (kADU/ch/s)continuum Br γdiscenvelopeØdisc= 5.8 ± 0.6 mas → 2.6 ± 0.3 AUØenv= 10.6 ± 0.8 mas → 4.8 ± 0.4 AUPTI, IOTA, & VLTI observation of FU Ori (1)FU Ori: YSO with accretion outburstMarginally resolved in H & K, Malbet et al. 2005, submitted−100 0 100−100 0 100−100 0 100 IOTA/S15N15IOTA/S15N35PTI/NSPTI/NWPTI/SWVLTI/U1−U3λ = 1.63 µm λ = 2.15 µmu (m)v (m)1.0 10.010−1310−1210−1110−10 λ (µm)λ Fλ (W m−2)IOTA/S15N15IOTA/S15N35PTI/NSPTI/NWPTI/SWVLTI/U1−U3 0 50 1000.00.51.0 0 50 100 λ = 1.63 µm λ = 2.15 µmB (m)|V|2˙M = (6.1 ± 2.5)× 10−5M/yri = 55 ± 7oθ = 47 ± 10ormin= 5.5 ± 2.5 RPTI, IOTA, & VLTI observation of FU Ori (1)FU Ori: YSO with accretion outburstMarginally resolved in H & K, Malbet et al. 2005, submitted−100 0 100−100 0 100−100 0 100 IOTA/S15N15IOTA/S15N35PTI/NSPTI/NWPTI/SWVLTI/U1−U3λ = 1.63 µm λ = 2.15 µmu (m)v (m)1.0 10.010−1310−1210−1110−10 λ (µm)λ Fλ (W m−2)IOTA/S15N15IOTA/S15N35PTI/NSPTI/NWPTI/SWVLTI/U1−U3 0 50 1000.00.51.0 0 50 100 λ = 1.63 µm λ = 2.15 µmB (m)|V|2˙M = (6.1 ± 2.5)× 10−5M/yri = 55 ± 7oθ = 47 ± 10ormin= 5.5 ± 2.5 RPTI, IOTA, & VLTI observation of FU Ori (2)FU Ori: hot spot in the disc?0.60.81.01.2−4 −2 0 2 40.60.81.01.2−4 −2 0 2 4 PTI/NSPTI/NWλ = 1.63 µm λ = 2.15 µmhour angle (hr)|V|2∆K = 4.2 ± 1.1 magrspot= 10.1 ± 0.4 AUθspot= 130 ± 1oEN−10 0 10−10 0 10 λ = 2.19 µmα offset (AU)δ offset (AU)PTI, IOTA, & VLTI observation of FU Ori (2)FU Ori: hot spot in the disc?0.60.81.01.2−4 −2 0 2 40.60.81.01.2−4 −2 0 2 4 PTI/NSPTI/NWλ = 1.63 µm λ = 2.15 µmhour angle (hr)|V|2∆K = 4.2 ± 1.1 magrspot= 10.1 ± 0.4 AUθspot= 130 ± 1oEN−10 0 10−10 0 10 λ = 2.19 µmα offset (AU)δ offset (AU)MIDI observation of Hen 3 1191 (1)B[e] star: either YSO or proto-PN.Resolved in N, Lachaume et al. 2005, in prep 8 10 120.00.51.0 B = 41.2 m θ = 54 oB = 45.6 m θ = 33 oB = 46.3 m θ = 22 oλ (µm)|V|staractive discinner rimMIDI observation of Hen 3 1191 (1)B[e] star: either YSO or proto-PN.Resolved in N, Lachaume et al. 2005, in prep 8 10 120.00.51.0 B = 41.2 m θ = 54 oB = 45.6 m θ = 33 oB = 46.3 m θ = 22 oλ (µm)|V|staractive discinner rimMIDI observation of Hen 3 1191 (2) 8 10 12 0 10 20 30 40 λ (µm)θud (mas)λ (µm)θud (mas)λ (µm)θud (mas)λ (µm)θud (mas)1.0 10.0 100.0 1000.10−1410−1310−1210−11 λ (µm)λ Fλ (W/m2)star = B1.5 star˙M/M?= 1.5 × 10−3yr−1!rrim= 30 AU (Trim= 1000 K)Radiative transfer modellingUsing two-layer disc modelsGeneralised Chiang & Goldreich (1997) two-layer models.τiτeτTeTiopticalviscous heatingIR/sub mmheating by the starISimple implementationIAnalytical dependenciesUsing two-layer disc modelsGeneralised Chiang & Goldreich (1997) two-layer models.τiτeτoptical IR/sub mmviscous heatingbackwarmingISimple implementationIAnalytical dependenciesPTI observation of SU AurIrradiation by the star and accretionLachaume et al. 2003, A&A 400, 795 0 50 100 1500.00.51.0 B (m)|V2| (norm.)1.0 10.0 100.0 1000.10−1410−1310−1210−11 (µm)λFλ (W.m−2)star = G2 star˙M = 2–10 × 10−8M/yrThe mid-IR SED of FU Ori starsBackwarming of the disc and accretionLachaume 2004, A&A, 422, 171backwarmingstellar heating10−610−510−410−1410−1310−1210−1110−10 λ (m)λFλ (W.m−2)V1057 Cyg550 pcH/r (10 AU) = 0.35V1057 Cyg550 pcH/r (10 AU) = 0.35backwarmingstellar heating10−610−510−410−1410−1310−1210−1110−10 λ (m)λFλ (W.m−2)V1515 Cyg1000 pcH/r (10 AU) = 0.35V1515 Cyg1000 pcH/r (10 AU) = 0.35→ N-band interferometryConclusionMain pointsIIn absence of image reconstruction, be careful:Icount with extended contribution;Icombine with other observables.Still new constraints on the physics of the first AUsIForthcoming large data sets with the VLTI needI“toy models” for a first interpretation;Inew, detailed simulationsIAccretion and irradiation often occur together,which no current model self-consistently describes.IOptically thick inner parts are not directly seen,though their physics condition planet formation.Main pointsIIn absence of image reconstruction, be careful:Icount with extended