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Planet formation theory: an overview
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Planet formation theory: an overview
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The standard model for planet formation is a bottom-up process in which the origin of rocky and gaseous planets can be traced back to the collision of micron-sized dust grains within the gas-rich environment of protoplanetary disks. Key milestones along the way include disk formation, grain growth, planetesimal formation, core growth, gas accretion, and planetary system evolution. I provide an introductory overview of planet formation, emphasizing the main ideas and reviewing current theoretical understanding. Many of the phases of planet formation have a well-developed physical understanding, though the complexity of the problem means that few can be quantitatively modeled with complete confidence. Transformative advances in disk imaging provide the first direct information on the initial conditions for planet formation, while exoplanet data has motivated new formation models that are faster, more efficient, and lead to a more diverse set of architectures than their Solar System inspired forebears. Much remains to be learned, and I close with a personal, incomplete list, of open problems.
Forward citations
Cited by 8 Pith papers
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The multi-planet system TOI-5624: Four transiting sub-Neptunes with an outer companion revealed by transit-timing variations
Four transiting sub-Neptunes with radii measured to <1.7% precision and masses >3 sigma for three planets, plus an outer non-transiting companion, discovered around TOI-5624 via TESS, CHEOPS photometry, and ground-bas...
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Sub-Snowline Formation of Gas-Giant Planets in Binary Systems
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Dust and Gas Transport in Substructured Nonideal MHD Wind-Launching Disks with Embedded Planets
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Extreme debris disks are a distinct subclass produced by large (Moon- to Mars-sized) collisions, with silica-rich mineralogy tracing energetic embryo impacts during terrestrial planet formation and high-W10 silica-poo...
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The Longest-period Young Transiting Exoplanets. A Duo of Puffy Giants inside a Debris Disk
HD 114082 hosts two puffy, moderate-to-low-mass giants on nearly circular, coplanar, near-resonant orbits of 225.55 and ~314 days, the longest-period young transiting exoplanets known.
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GPU-accelerated N-body simulations show that the common acceleration factor f distorts planetary chemical compositions and that terrestrial planets can form resonant chains without gas-driven orbital migration.
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