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• W3104394897 endingPage "1276" @default.
• W3104394897 startingPage "1264" @default.
• W3104394897 abstract "We consider trends resulting from two formation mechanisms for short-period super-Earths: planet-planet scattering and migration. We model scenarios where these planets originate near the snow line in ``cold finger'' circumstellar disks. Low-mass planet-planet scattering excites planets to low periastron orbits only for lower mass stars. With long circularisation times, these planets reside on long-period eccentric orbits. Closer formation regions mean planets that reach short-period orbits by migration are most common around low-mass stars. Above ~1 Solar mass, planets massive enough to migrate to close-in orbits before the gas disk dissipates are above the critical mass for gas giant formation. Thus, there is an upper stellar mass limit for short-period super-Earths that form by migration. If disk masses are distributed as a power law, planet frequency increases with metallicity because most disks have low masses. For disk masses distributed around a relatively high mass, planet frequency decreases with increasing metallicity. As icy planets migrate, they shepherd interior objects toward the star, which grow to ~1 Earth mass. In contrast to icy migrators, surviving shepherded planets are rocky. Upon reaching short-period orbits, planets are subject to evaporation processes. The closest planets may be reduced to rocky or icy cores. Low-mass stars have lower EUV luminosities, so the level of evaporation decreases with decreasing stellar mass." @default.
• W3104394897 created "2020-11-23" @default.
• W3104394897 creator A5015993983 @default.
• W3104394897 creator A5036275243 @default.
• W3104394897 date "2008-08-01" @default.
• W3104394897 modified "2023-09-27" @default.
• W3104394897 title "Planet Formation around Stars of Various Masses: Hot Super‐Earths" @default.
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• W3104394897 doi "https://doi.org/10.1086/589436" @default.
• W3104394897 hasPublicationYear "2008" @default.
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