Programme

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A day will typically start with breakfast, then there is a morning session and discussion until lunchtime. In the afternoon there will be a second session with discussion, and in the evening we will have dinner together. Each session will start with a ~1 hour talk, summarising the state-of-the-art and the main open problems related to the corresponding topic. The rest of the session will be devoted to discuss the questions that occurred during the talk and those prepared earlier by the participants. Some questions identified so far are listed below. Participants are encouraged to let us know in advance the topics they want to discuss, or to bring their own questions to create an active debate. Coffee breaks will be offered within each session.

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Tuesday, June 26th

    

Noon: Welcome and lunch

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Afternoon: Session 1. General layout of the problem. 

Discussion opener: Aurora Sicilia-Aguilar.

PDF slides here

Why is there a huge discrepancy between number of exoplanets (>3000) and the number of young planets detected? Why are there so few/none planets detected around PMS stars? Do we have reliable direct detections of young planets, either in formation (accreting) or already formed- in discs around young stars (<10Myr), how many? Which candidates from the list of young planets are the most reliable? Why is it so hard to detect them? ...

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Wednesday, June 27th

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Morning: Session 2. Theoretical expectations and problems. 

Discussion opener: Kaitlin Kratter.

How do planets form, what accretion rates do we expect? Do planets form on a very short timescale or are current detection limits for planetary accretion rates still above the real ones? What is the origin of the planet-metallicity correlation (primordial cloud, pollution,...)? Would it be possible to check that correlation in the pre-main sequence phase?...

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Afternoon: Session 3. Direct observational detections. 

Discussion opener: Sean Brittain & Alice Zurlo.

PDF slides Brittain here

Which is (are) the best observational approach(es) to make direct detections of young (proto)planets? What techniques would improve current detection limits? What are the protoplanet accretion signatures? Could protoplanet outflows be detected better? What can we learn from the exoplanet community? Other techniques?

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Thursday, June 28th

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Morning: Session 4. Indirect observational detections. 

Discussion opener: Zhaohuan Zhu.

PDF slides here

Inner holes, spiral arms, dust traps, radial, non-keplerian streams...Which are the planetary signatures in the disc?what are the problems in these scenarios? To what extent are these observables the direct result of (only) planet formation? What can we really infer about the number of planets and their properties from such indirect observations? Do transient events - red and blue absorptions - constitute a signpost of planetesimals in pre-main sequence stars?

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Afternoon: Session 5. Planet formation vs other processes. 

Discussion opener: Richard Alexander.

PDF slides here

The impact that photoevaporation can have on planet formation, thus the stellar properties on the disc. Is the Mdisc-Macc plane useful to disentangle between the different scenarios driving disc evolution (i.e to identify sub-samples of stars with ongoing planet formation vs e.g. photo-evaporated discs).

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Friday, June 29th

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Morning: Session 6. Planet formation and transition discs

Discussion opener: François Ménard

Are protoplanetary discs with large inner cavities a representative sample? Or perhaps they represent the (small) group of large, massive discs? What causes the phenomenon of a transition disc, how to distinguish between the different scenarios, what are the open problems? Can a planet that carves out a gap cause the disc to spread out and become more luminous if at first some of the material is optically thick?

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Afterwards: Lunch and farewell

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