PHYVE codeProtoplanetary disk HYdrodynamical Viscous Evolution

Author

Kévin BAILLIÉ (IMCCE/Observatoire de Paris/CNES)

Presentation

The PHYVE code is one of the only hydrodynamical numerical codes that allows to follow the entire lifetime of the protoplanetary disk from its formation by the collapse of the molecular cloud to its end by the photoevaporation, upon radial distances up to 1000 AU. It derives the disk viscous evolution: not only the surface mass density distribution but also the midplane temperature and dust composition profiles for instance.

Physics

This code is based on the α-disk model (α, the turbulent viscosity defined by Shakura & Sunyaev 1973) and accounts for a full coupling between:

• The disk dynamics and thermodynamics (through the viscosity)
• The disk temperature and geometry (through an irradiation and shadowing model)
• The disk temperature and its dust composition (through the opacity model)

Initial conditions

PHYVE can not only consider an initial condition such as the Minimum Mass Solar Nebula, but also push that initial condition back to the primordial molecular cloud and build the star and the disk at the same time. The stellar evolution is taken into account by interpolating the star mass accretion rate over pre-calculated stellar evolution tables.

The PHYVE code was initially developed in IDL before being adapted in Python.

Example of application

These evolved disk profiles allow to understand the positions of the ice lines and derive the migration directions and rates of potential planets in such disks. PHYVE was used to show that hot Neptunes and Super-Earths can be saved by being trapped at the icelines in the disk, therefore applying a natural selection process to planetary embryos based on their mass, radial location and composition

References for the code details

• Baillié, K., Marques, J., Piau, L., 2019. Building protoplanetary disks from the molecular cloud: redefining the disk timeline. Accepted in Astronomy & Astrophysics
• Baillié, K., Charnoz, S., Pantin, E., 2016. Trapping planets in an evolving protoplanetary disk: preferred time, locations and planet mass. Astronomy & Astrophysics 590, A60
• Baillié, K., Charnoz, S., Pantin, E., 2015. Time Evolution of Snow Regions and Planet Traps in an Evolving Protoplanetary Disk. Astronomy & Astrophysics 577, A65. [Press Release]
• Charnoz, S., Aléon, J., Chaumard, N., Baillié, K., Taillifet, E., 2015. Growth of Calcium-Aluminum-rich inclusions by coagulation and fragmentation in a turbulent protoplanetary disk. Icarus 252, 440-453
• Baillié, K., Charnoz, S., 2014. Time evolution of a viscous protoplanetary disk with a free geometry: toward a more self-consistent picture. Astrophysical Journal 786, 35