AGN dust tori can form tens of millions of planetesimals from Earth to super-Jupiter masses via streaming instability, with continued growth to stellar masses through pebble and gas accretion.
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MHD collapse simulations define an Envelope-Disk Transition Zone (ENDTRANZ) where a jump in the j-r profile occurs due to positive gravitational torques, with a corresponding jump detected in ALMA observations of L1527 IRS.
Non-ideal MHD shearing-box simulations with a new damping scheme yield power-law scalings for wind-driven accretion rates based on midplane plasma beta, ambipolar Elsasser number, and active layer thickness that match results within a factor of 2-3.
Simulations require 2000 Earth masses of pebbles to match observed disc gaps, but this produces mostly gas giants and few super-Earths, contradicting exoplanet data.
An upgraded planet population synthesis model incorporates post-disc dynamical evolution and atmospheric enrichment to generate synthetic exoplanet populations with improved fidelity to N-body results and observations.
citing papers explorer
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Active Galactic Nucleus Tori: Potential Birthplace to Millions of Planets
AGN dust tori can form tens of millions of planetesimals from Earth to super-Jupiter masses via streaming instability, with continued growth to stellar masses through pebble and gas accretion.
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Modelling the Break in the Specific Angular Momentum within the Envelope-Disk Transition Zone
MHD collapse simulations define an Envelope-Disk Transition Zone (ENDTRANZ) where a jump in the j-r profile occurs due to positive gravitational torques, with a corresponding jump detected in ALMA observations of L1527 IRS.
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Beyond the $\alpha$ model: scaling the wind-driven accretion rate in protoplanetary disks using systematic non-ideal magnetohydrodynamical simulations
Non-ideal MHD shearing-box simulations with a new damping scheme yield power-law scalings for wind-driven accretion rates based on midplane plasma beta, ambipolar Elsasser number, and active layer thickness that match results within a factor of 2-3.
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Rapid and Predictive Planet Population Synthesis Model (RAPPS) I. Upgraded model and resulting synthetic populations
An upgraded planet population synthesis model incorporates post-disc dynamical evolution and atmospheric enrichment to generate synthetic exoplanet populations with improved fidelity to N-body results and observations.