Periodic Reporting for period 3 - MHDiscs (From non-ideal magnetohydrodynamics to the structure and evolution of protoplanetary discs)
Reporting period: 2022-09-01 to 2024-02-29
The project main objective is to model protoplanetary disc (then gas and dust around a newly formed star that harbour planet formation) using state of the art, first principle, magnetohydrodynamical simulations.
Our main objectives are to identify the physical processes responsinble for the structures observed in many protoplanetary discs, like concentric rings, spiral waves and crescents, and to be able to tell whether these structures are due to embedded planets formed early in the system, or are due to gas processes, that are responsible for planet formation.
The key working hypothesis of the project is that magnetohydrodynamical disc winds are one of the key to protoplanetary disc evolution, which could explain simultaneously the accretion rates and the structure we observe. If confirmed, this scenario could also explain the enrichment in reprocessed elements in the outer solar system (in particular in comets) and the origin of our own solar system.
Our main objectives are to identify the physical processes responsinble for the structures observed in many protoplanetary discs, like concentric rings, spiral waves and crescents, and to be able to tell whether these structures are due to embedded planets formed early in the system, or are due to gas processes, that are responsible for planet formation.
The key working hypothesis of the project is that magnetohydrodynamical disc winds are one of the key to protoplanetary disc evolution, which could explain simultaneously the accretion rates and the structure we observe. If confirmed, this scenario could also explain the enrichment in reprocessed elements in the outer solar system (in particular in comets) and the origin of our own solar system.
Since the beginning of the project we have performed the following tasks:
- compute a set of semi-anayltical MHD wind models to be used in the project for testing and initial exploration
- computed the first global non-ideal MHD simulations of protoplanetary disc with dust, demonstrating that MHD wind can indeed shape the dust disk in lead to observational signatures similar to the ones observed
- written a complete MHD numerical code portable on new hybrid architectures. The code is now being used to compute our numerical models.
- computed the first global non-ideal MHD simulation of planet-disc interraction
- compute a set of semi-anayltical MHD wind models to be used in the project for testing and initial exploration
- computed the first global non-ideal MHD simulations of protoplanetary disc with dust, demonstrating that MHD wind can indeed shape the dust disk in lead to observational signatures similar to the ones observed
- written a complete MHD numerical code portable on new hybrid architectures. The code is now being used to compute our numerical models.
- computed the first global non-ideal MHD simulation of planet-disc interraction
The project has already delivered its first results with the first global models including detailed first principle physics (non-ideal MHD+grains). As a side product, it has also led to a new performance-portable numerical code which will be opened to the community as an open-source code.
By the end of the project, we expect to have the full kinematic and radiative signature of embedded planets and wind-driven structures, and a direct confrontation to observations thanks to our participation to a large ALMA survey targeting disc kinematics.
By the end of the project, we expect to have the full kinematic and radiative signature of embedded planets and wind-driven structures, and a direct confrontation to observations thanks to our participation to a large ALMA survey targeting disc kinematics.