Mario van den Ancker – ESO Garching

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Presentation transcript:

Mario van den Ancker – ESO Garching High Angular Resolution Studies of the Structure of Protoplanetary Disks Surrounding Intermediate-Mass Stars Mario van den Ancker – ESO Garching Collaborators: Davide Fedele (MPIA Heidelberg), Gerrit van der Plas (ESO/Univ. Amsterdam), Bram Acke (KU Leuven), Jeroen Bouwman (MPIA Heidelberg), Rens Waters (Univ. Amsterdam), Markus Wittkowski (ESO)

Herbig Ae/Be Stars: A Primer Young (< 10 Myr) intermediate-mass (2-10 solar mass) stars surrounded by protoplanetary disks Observationally advantageous targets as disks are brighter and more extended than around T Tauri stars About 200 known in our galaxy

Meeus et al. (2001) Classification Scheme Herbig Ae/Be Stars ``Group I’’ ``Group II’’

Correlations with Meeus et al. classification scheme Group I (`` flared disks’’) Group II (``self-shadowed disks’’) Strong far-IR excess Weak far-IR excess Strong PAH emission Weak or no PAH emission Strong [O I] emission Weak or no [O I] emission Nearby disks resolved in scattered light Point-sources

A Comparison of the Distribution of Gas and Dust in Protoplanetary Disks Poorly constrained observationally Two tracers sensitive to the 1-10 AU region for systems at 100-200 pc: Gas: [O I] 6300 Å emission line Dust: Mid-IR (8-13 µm) Interferometry

[O I] Emission: VLT/UVES Observations

[O I] emission: Non-thermal

[O I] emission: Due to photo-dissociation of OH by stellar UV photons in upper layers flared disk

HD 179218 Group I = Flared Disk HD 101412 Group II = Self-shadowed Disk

VLTI/MIDI Observations (I) HD 179218 (group I = flared disk)

VLTI/MIDI Observations (II) HD 101412 (group II = self-shadowed disk)

Conclusions HD 179218: Dust seen further out than [O I] emission; little OH in surface layers past 15 AU? HD 101412: Scale height of gas larger than dust; disk self-shadowed in dust, but not in gas! Evolution: from flared disks to self-shadowed disks Driver: loss of gas-dust coupling in disk atmosphere?