A new Bessel kernel for 2D disc gravity fixes convergence in GI simulations and reveals that softening prescriptions overestimate formed planet masses by a factor of 2-3.
Title resolution pending
6 Pith papers cite this work. Polarity classification is still indexing.
6
Pith papers citing it
verdicts
UNVERDICTED 6representative citing papers
High-resolution molecular gas observations show that spiral arms and bars in z~1.5 disk galaxies drive substantial radial inflows at rates matching star formation, linking morphology directly to gas transport.
Resolving the inner few AU in protostellar disk simulations yields complete tidal disruption of migrating fragments and shorter, sharper accretion outbursts than coarser 30 AU models.
Live halos with sufficient mass resolution enable cascading multi-mode spirals in galactic disks through swing amplification and mode interference, absent in fixed-potential or coarsely resolved models.
Radiative cooling thins hot accretion disks around black holes, reduces wind power, and makes inflow-rate decrease depend more on MRI-driven turbulence than on winds as cooling strengthens.
Statistical analysis of 1155 protoplanetary disks shows only 1.2% are formally gravitationally unstable, likely because observations underestimate their masses.
citing papers explorer
-
Self-gravity in thin protoplanetary discs: 2. Numerical convergence solved and revealing the overestimation in mass of formed planets with softening
A new Bessel kernel for 2D disc gravity fixes convergence in GI simulations and reveals that softening prescriptions overestimate formed planet masses by a factor of 2-3.
-
NOEMA3D: Resolving radial gas flows in disk galaxies at z~1.1-1.6 with high-resolution CO observations
High-resolution molecular gas observations show that spiral arms and bars in z~1.5 disk galaxies drive substantial radial inflows at rates matching star formation, linking morphology directly to gas transport.
-
From Fragments to Flares: Migration, Tidal Disruption, and Observable Bursts in Massive Protostellar Disks
Resolving the inner few AU in protostellar disk simulations yields complete tidal disruption of migrating fragments and shorter, sharper accretion outbursts than coarser 30 AU models.
-
Effects of Resolution and Local Stability on Galactic Disks: I. Multiple Spiral Mode Formation via Swing Amplification
Live halos with sufficient mass resolution enable cascading multi-mode spirals in galactic disks through swing amplification and mode interference, absent in fixed-potential or coarsely resolved models.
-
Radiative cooling effects on black hole hot accretion flows around the sub-Bondi radius
Radiative cooling thins hot accretion disks around black holes, reduces wind power, and makes inflow-rate decrease depend more on MRI-driven turbulence than on winds as cooling strengthens.
-
Investigation of gravitational stability of protoplanetary disks based on statistical analysis of their masses
Statistical analysis of 1155 protoplanetary disks shows only 1.2% are formally gravitationally unstable, likely because observations underestimate their masses.