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Intro
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Classroom Contents
Uncovering the Origins of Super-Earths and Giant Planets
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- 1 Intro
- 2 Dust growth and transport: key process for planet formation
- 3 Planet formation: Likely a bottom up process
- 4 Formation clues from exoplanet demographics
- 5 Why does dust content matter for gas accretion?
- 6 Dust-to-gas ratio and dust opacity A function of location in the disk, especially if the fragmentation threshold varies with composition
- 7 Disk opacity is starkly different from ISM opacity
- 8 Gas giants at intermediate distances
- 9 Super-Earths are the most common planets in the galaxy. They are even more common around M stars than FGK stars.
- 10 The process of pebble accretion
- 11 Pebble accretion efficiency: key to converting dust to planets
- 12 Pebble accretion efficiency as a function of stellar mass
- 13 Super-Earth formation in actively heated regions of the disk
- 14 Giant planet core formation in the passively heated regions of the disk
- 15 Comparison to observations: We need early-stage disk demographics
- 16 What conditions favor the formation of cold giant planets?
- 17 Placing constraints on Kepler-167's disk properties
- 18 How giant planet hosting disks can form super-Earths
