Astronomy and Astrophysics – Astronomy
Scientific paper
May 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21011003r&link_type=abstract
American Astronomical Society Meeting 210, #110.03; Bulletin of the American Astronomical Society, Vol. 39, p.234
Astronomy and Astrophysics
Astronomy
Scientific paper
Close-in planets with masses less than one Neptune mass have been detected around roughly ten stars to date. In addition to these so-called "Hot Neptunes" or "Hot Super-Earths", upcoming missions such as CoRot and Kepler expect to find a large number of smaller, close-in "Hot Earths". Most disk models do not contain a large amount of mass in their innermost regions. So, how do Hot Earths form? There are several candidate mechanisms: 1) A "type 2" migrating giant planet can shepherd material interior to strong mean motion resonances. More than half of the solid component of the disk inside the giant planet's starting orbit can be displaced to the region interior to the giant planet's final orbit. So, many close-in giant planets may be accompanied by "hot Earths"; 2) Terrestrial cores, interacting tidally with the gaseous disk, can "type 1" migrate into the very inner disk. Interactions between cores may result in near-resonant configurations; and 3) In a system with two or more giant planets with non-zero eccentricities, dispersal of the gaseous disk can cause secular resonances to sweep through the system, and can moderately enhance the amount of material in the inner regions. Each of these mechanisms makes predictions that should be testable in the near future.
References: Fogg & Nelson (2005, 2007), Zhou et al (2005), Raymond, Mandell & Sigurdsson (2006), Mandell, Raymond & Sigurdsson (2007), Terquem & Papaloizou (2007)
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