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Planetary population synthesis
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The planetary population synthesis method aims at comprehensively testing planet formation theories against observational evidence and providing theoretical sets of planets to help interpret observations and inform instrument development. Recent developments on the theoretical and observational sides are reviewed: First, observational constraints are summarized, then, the work flow of population synthesis and its two main components are presented, which are, global end-to-end models of planetary formation and evolution and probability distributions for the disk initial conditions. Next, the output of four recent population synthesis models is compared in detail and differences and similarities are discussed. The goal is to help the reader understand the assumptions that were made and how they impact the results. Furthermore, future directions of research are identified and the impact of current and future observational programs is discussed. With JWST, evidence on disk and planet compositions emerges. Planet formation models need to prepare for these near-future developments by including self-consistent magnetic wind-driven gas and dust disk evolution, planetary migration, as well as employ hybrid pebble and planetesimal accretion, which are identified as dominant modes of accretion in different mass regimes.
Forward citations
Cited by 3 Pith papers
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The importance of the dynamical corotation torque for the migration of low-mass planets -- 1D analytical prescriptions verified by 2D hydrodynamical simulations
A memory-timescale prescription for the dynamical corotation torque lets 1D models reproduce 2D hydrodynamic migration of low-mass planets in low-viscosity discs.
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The New Generation Planetary Population Synthesis (NGPPS) VIII. Impact of host star metallicity on planet occurrence rates, orbital periods, eccentricities, and radius valley morphology
A population synthesis model reproduces several observed metallicity trends in exoplanet demographics, including the deepening radius valley, while underestimating the period and eccentricity dependence.
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On the formation of satellites in dense solid-particle disks
In dense solid-particle disks, the mass of the largest formed satellite scales roughly linearly with disk mass, with a stochastic spread large enough that duplicated initial conditions produce very different moons.
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