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Observing inner discs where planets form



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Observing inner discs where planets form From discs to planets New observations models and theories Pasadena California USA R gis Lachaume1 Fabien Malbet2 Jean Louis Monin2 1 2 Max Planck Institut f r Radioastronomie Laboratoire d Astrophysique de Grenoble March 8th 2005 Introduction Scales in protoplanetary discs Taurus 0 1 0 001 1 0 01 optical distance to the star 10 100 AU 0 1 1 radio Earth large column density giant planet formation Kuchner 2004 ApJ 612 1147 Pluto Scales in protoplanetary discs Taurus 0 1 0 001 distance to the star 10 100 AU 0 1 1 radio 1 0 01 optical Earth 1000 1000 100 Pluto 100 10 m N band m K band baseline length Optical interferometry radiative transfer But visibilities are are not enough 1 Irradiated visous disc model for T Tauri visibility fit Lachaume Malbet Monin 2003 A A 379 515 V2 norm 1 0 0 5 0 0 0 50 100 150 B m M 8 0 10 7 M yr rmin 18 0 R But visibilities are are not enough 1 Irradiated visous disc model for T Tauri visibility fit Lachaume Malbet Monin 2003 A A 379 515 10 11 F W m 2 V2 norm 1 0 0 5 0 0 0 50 100 150 10 12 10 13 1 0 10 0 m B m M 8 0 10 7 M yr rmin 18 0 R Combine observables e g SED visibilities 100 0 But visibilities are are not enough 2 The large scale diffuse emission problem Lachaume 2003 A A 400 795 compact object diffuse emission But visibilities are are not enough 2 compact object visibility The large scale diffuse emission problem Lachaume 2003 A A 400 795 wrong diameter diffuse emission baseline Adaptive optics speckle interferometry Ad hoc modelling AMBER observation of MWC 297 Herbig Be star Resolved in K Tatulli 2005 Ph D thesis 1 0 6 0 5 4 2 0 0 2 14 2 16 2 18 Wavelength micron Flux kADU ch s Visibiliy 8 AMBER observation of MWC 297 Herbig Be star Resolved in K Tatulli 2005 Ph D thesis 1 0 continuum 6 0 5 4 2 0 0 Br Flux kADU ch s Visibiliy 8 disc envelope 2 14 2 16 2 18 Wavelength micron disc 5 8 0 6 mas 2 6 0 3 AU env 10 6 0 8 mas 4 8 0 4 AU PTI IOTA VLTI observation of FU Ori 1 FU Ori YSO with



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