Join a comprehensive lecture exploring the formation mechanisms of super-Earths and giant planets, delivered by McGill University's Yayaati Chachan. Delve into crucial planetary formation processes including dust growth, transport, and pebble accretion, while examining how these mechanisms vary across different stellar environments. Learn about the relationship between dust-to-gas ratios and disk opacity, and understand why super-Earths are particularly abundant around M-type stars compared to FGK stars. Explore the conditions necessary for giant planet formation, including core development in passively heated disk regions, and investigate specific case studies like the Kepler-167 system. Discover how disk demographics in early stellar system development influence planetary formation, and understand the complex interplay between super-Earth and giant planet formation within the same stellar system.
Overview
Syllabus
Intro
Dust growth and transport: key process for planet formation
Planet formation: Likely a bottom up process
Formation clues from exoplanet demographics
Why does dust content matter for gas accretion?
Dust-to-gas ratio and dust opacity A function of location in the disk, especially if the fragmentation threshold varies with composition
Disk opacity is starkly different from ISM opacity
Gas giants at intermediate distances
Super-Earths are the most common planets in the galaxy. They are even more common around M stars than FGK stars.
The process of pebble accretion
Pebble accretion efficiency: key to converting dust to planets
Pebble accretion efficiency as a function of stellar mass
Super-Earth formation in actively heated regions of the disk
Giant planet core formation in the passively heated regions of the disk
Comparison to observations: We need early-stage disk demographics
What conditions favor the formation of cold giant planets?
Placing constraints on Kepler-167's disk properties
How giant planet hosting disks can form super-Earths
Taught by
CITA Presentations
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