A copy of this work was available on the public web and has been preserved in the Wayback Machine. The capture dates from 2016; you can also visit the original URL.
The file type is
snow line" at a few AU and volatile-rich c outside. It will be interesting to see whether the usual migration mechanism that is invoked to alter planetary orbits-tidal interactions with the gaseous protoplanetary disk-could draw together two planets from such different regions of the disk. Or whether the compositions and densities of the planets could have changed with time, for example, because of the preferential erosion of the smaller planet's atmosphere by stellar irradiation (16) (fig. S21doi:10.1126/science.1221206 pmid:22859484 fatcat:o3sb4szbzfa3pepqrfphq7ktwa