  Whether the higher occurrence of giant planets being hosted by metal-rich
versus metal-poor stars results from formation or from "pollution" has been a
question of intense debate. We present new patterns that emerge when
planet/star systems are separated by stellar [Fe/H], and when systems with
stellar companions are separated out. These differences can best be explained
if the onset of high eccentricity planet migration is also a time when planet
are sent into merge with the star. Planet migration into the star is likely a
complementary explanation to the view that systems with higher initial iron
abundance form more planets, and that more crowded planets are more likely to
scatter into eccentric orbits. Planets of iron-rich single stars have
eccentricity distributions that are higher than planets of iron-poor single
stars (where "rich" and "poor" are stars whose [Fe/H] is above and below solar,
respectively). Stars with planets that have a stellar companion comprise a
third population of systems in which the stars are preferentially iron-rich. We
describe new patterns that are best explained by eccentric planet migration
being associated with other planets migrating into the star. Though medium
planets are more numerous than giant planets at periods greater than three
days, giant planets are more numerous than medium planets at the shortest
periods. Since giant planets migrate into the star faster, we show this as
evidence of giant planet migration. Planet migration into the star is certain
to be an important part of planetary system evolution.
