Growth and Evolution of Planets in protoplanetary Disks
Final Report Abstract
Understanding the diversity of extrasolar planets’ mass and orbital distributions is difficult due to incorrect assumptions on the protoplanetary disk structure. In this project, a more realistic model of protoplanetary discs, which accounts both for the vertical shear instability and disks winds, magnetohydrodynamical and self-gravitational effects is developed. By the help of numerical simulations, we can show that gas accretion can proceed in conditions of low turbulent viscosity when the influence of magnetic fields is considered. Magnetic fields operate in the regions of protoplanetary disks, where the degree of ionization was believed to be too low up to now, due to instabilities specific to weakly ionized gas. Additionally, we have studied the process of planet formation by fragmentation in a self-gravitating disk depending on the cooling. Turbulence driven by gravitational instabilities can be modeled as an effective viscosity. We could also clearly separate planet-induced spirals from instabilityinduced spirals; this could help future identifications of embedded exoplanets that are too faint to be observed directly, or help rule out planets as the cause of spirals in other disks.
Publications
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Migration of Jupiter-mass planets in low-viscosity discs. Astronomy & Astrophysics, 646, A166.
Lega, E.; Nelson, R. P.; Morbidelli, A.; Kley, W.; Béthune, W.; Crida, A.; Kloster, D.; Méheut, H.; Rometsch, T. & Ziampras, A.
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Spiral structures in gravito-turbulent gaseous disks. Astronomy & Astrophysics, 650, A49.
Béthune, William; Latter, Henrik & Kley, Wilhelm
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Gravitoturbulent dynamo in global simulations of gaseous disks. Astronomy & Astrophysics, 663, A138.
Béthune, William & Latter, Henrik
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Migration of Jupiter mass planets in discs with laminar accretion flows. Astronomy & Astrophysics, 658 (2022, 1, 27), A32.
Lega, E.; Morbidelli, A.; Nelson, R. P.; Ramos, X. S.; Crida, A.; Béthune, W. & Batygin, K.
