Survival and Detectability of Exoplanets Beyond 100 AU

Details Survival and Detectability of Exoplanets Beyond 100 AU Survival and Detectability of Exoplanets Beyond 100 AU

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dda....39.0603v&link_type=abstract

American Astronomical Society, DDA meeting #39, #6.03

Astronomy and Astrophysics

Astronomy

Scientific paper

Direct imaging searches have begun to achieve significant sensitivity to giant planets at large separations (> 100 AU) from their host stars. Such searches motivate the exploration of planetary formation and evolution models that predict the number, masses, and orbital properties of planets which may reside in wide orbits. The standard formation models of core accretion and direct gravitational collapse are not expected to form such planets in situ. We explore the possibility of giant planets forming at conventional distances before migrating to much larger separations via gravitational scattering (Debes and Sigurdsson 2006). We present simulations of dynamically unstable multiple planet systems in order to determine the efficiency of placing planets on detectably wide orbits. We also investigate how long planets can remain in such "extreme" orbits and consider the effects of galactic tides and stellar encounters. We find that planet scattering could lead to a population of highly eccentric (e > 0.8) planets with planet-star separations of hundreds to thousands of AU and contrast ratios suitable for detection via direct imaging in nearby star forming regions. If most stars form multiple giant planets that will eventually undergo a dynamical instability, then the frequency of such planets could be measured via ground-based direct imaging campaigns and place constraints on planet formation models.

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