2006/09/07 by Sean N. Raymond, Avi M. Mandell, Steinn Sigurdsson +1 · 5 citations
Physics and Astronomy · #Astro and Planetary Science #Astrobiology #Astronomy #Astrophysics and Star Formation Studies #Physics #Planet #Planetary habitability #Stellar, planetary, and galactic studies #Terrestrial planet #astro-ph
paper · pdf · doi:10.1126/science.1130461
published as Science 313 (2006) 1413 · 13 pages, 3 figures, 1 table. Resolution of one figure has been degraded. For full-resolution images, see http://lasp.colorado.edu/~raymond/RMS-pre.pdf
openalex publication_date 2006/09/07 · arxiv created 2006/09/08 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Close-in giant planets (e.g., "hot Jupiters") are thought to form far from their host stars and migrate inward, through the terrestrial planet zone, via torques with a massive gaseous disk. Here we simulate terrestrial planet growth during and after giant planet migration. Several-Earth-mass planets also form interior to the migrating jovian planet, analogous to recently discovered "hot Earths." Very-water-rich, Earth-mass planets form from surviving material outside the giant planet's orbit, often in the habitable zone and with low orbital eccentricities. More than a third of the known systems of giant planets may harbor Earth-like planets.