Summary
Exoplanets are frequent around Solar-like stars, as shown by Large Surveys. They are formed by the growth of dust and accumulation of gas contained in protoplanetary disks surrounding young stars. To form planets, the classic Core-Accretion scenario is the main framework today, but it appears to be too slow given the short lifetimes of disks. Theoretical additions to Core-Accretion exist to speed it up. They all hypothesize that disks contain a massive, dense, and flat layer of pebbles in the midplane. The validation of these scenarios will be impossible as long as the disk properties remain uncertain. The first objective of this project is to provide the first direct observational constraints (mass, vertical extent, radius) for this midplane pebble layer. Specifically, an original imaging programme for Edge-On disks will be combined with dedicated hydrodynamical models of vertical dust settling, taking into account dust evolution and dust-gas dynamics. This is very demanding. The second objective is to identify the shape of dust in young disks and pin down their growth mechanisms. This major advance is also crucial because the structure of dust governs the dust-gas dynamics (via collision and drag cross-sections) as well as the scattering properties needed to compare data and models. To meet this goal, we will extract the scattering properties (phase function, polarisation) from high resolution images and use a unique micro-wave analogy experiment. Complex analog particles will be fabricated, measured, and compared with data to ultimately reveal the structure of dust in disks. All these results, combined in the final objective, will lead to a major leap towards a deep understanding of dust growth and early planet assembly in protoplanetary disks. Dust2Planets has the potential to overcome two long-standing obstacles in early planetesimal assembly: how dust overcomes the radial-drift and fragmentation barriers to form planetesimals.
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| Web resources: | https://cordis.europa.eu/project/id/101053020 |
| Start date: | 01-09-2022 |
| End date: | 31-08-2027 |
| Total budget - Public funding: | 2 487 721,00 Euro - 2 487 721,00 Euro |
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Original description
Exoplanets are frequent around Solar-like stars, as shown by Large Surveys. They are formed by the growth of dust and accumulation of gas contained in protoplanetary disks surrounding young stars. To form planets, the classic Core-Accretion scenario is the main framework today, but it appears to be too slow given the short lifetimes of disks. Theoretical additions to Core-Accretion exist to speed it up. They all hypothesize that disks contain a massive, dense, and flat layer of pebbles in the midplane. The validation of these scenarios will be impossible as long as the disk properties remain uncertain. The first objective of this project is to provide the first direct observational constraints (mass, vertical extent, radius) for this midplane pebble layer. Specifically, an original imaging programme for Edge-On disks will be combined with dedicated hydrodynamical models of vertical dust settling, taking into account dust evolution and dust-gas dynamics. This is very demanding. The second objective is to identify the shape of dust in young disks and pin down their growth mechanisms. This major advance is also crucial because the structure of dust governs the dust-gas dynamics (via collision and drag cross-sections) as well as the scattering properties needed to compare data and models. To meet this goal, we will extract the scattering properties (phase function, polarisation) from high resolution images and use a unique micro-wave analogy experiment. Complex analog particles will be fabricated, measured, and compared with data to ultimately reveal the structure of dust in disks. All these results, combined in the final objective, will lead to a major leap towards a deep understanding of dust growth and early planet assembly in protoplanetary disks. Dust2Planets has the potential to overcome two long-standing obstacles in early planetesimal assembly: how dust overcomes the radial-drift and fragmentation barriers to form planetesimals.Status
SIGNEDCall topic
ERC-2021-ADGUpdate Date
09-02-2023
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