Planetary migration | Wikipedia audio article
Channel: wikipedia tts
Date: 2019-05-29

This is an audio version of the Wikipedia Article:
https://en.wikipedia.org/wiki/Planetary_migration


00:01:17 1 Types of disk
00:01:27 1.1 Gas disk
00:02:16 1.2 Planetesimal disk
00:03:05 2 Types of migration
00:03:16 2.1 Disk migration
00:04:24 2.1.1 Type I migration
00:07:35 2.1.2 Type II migration
00:10:47 2.1.3 Type III migration
00:12:25 2.2 Gravitational scattering
00:14:29 2.3 Tidal migration
00:16:02 2.4 Kozai cycles and tidal friction
00:17:42 2.5 Planetesimal-driven migration
00:21:17 3 Resonance capture
00:23:39 4 In the Solar System
00:27:02 5 See also



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SUMMARY
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Planetary migration occurs when a planet or other stellar satellite interacts with a disk of gas or planetesimals, resulting in the alteration of the satellite's orbital parameters, especially its semi-major axis.  Planetary migration is the most likely explanation for hot Jupiters: exoplanets with jovian masses but orbits of only a few days.  The generally accepted theory of planet formation from a protoplanetary disk predicts such planets cannot form so close to their stars, as there is insufficient mass at such small radii and the temperature is too high to allow the formation of rocky or icy planetesimals.  
It has also become clear that terrestrial-mass planets may be subject to rapid inward migration if they form while the gas disk is still present. This may affect the formation of the cores of the giant planets (which have masses of the order of 10 Earth masses), if those planets form via the core-accretion mechanism.