Radii, Masses, Densities, and Occurrence for Planets within 0.25 AU

Details Radii, Masses, Densities, and Occurrence for Planets within 0.25 AU Radii, Masses, Densities, and Occurrence for Planets within 0.25 AU

May 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21811202m&link_type=abstract

American Astronomical Society, AAS Meeting #218, #112.02; Bulletin of the American Astronomical Society, Vol. 43, 2011

Astronomy and Astrophysics

Astronomy

Scientific paper

We report the observed distribution of planet radii, masses, and orbital distances for orbital periods less than 50 days around Solar-type (GK) stars. We draw from extensive Doppler and Kepler measurements that offer good completeness for planets with radii as small as 2.0 Earth-radii. We include the photometric signal-to-noise ratio for all 156,000 target stars to determine planet detectability as a function of planet radius and orbital period for each target. We consider Kepler target stars within the ``Solar subset'' having Teff = 4100--6100 K, logg = 4.0--4.9, and stars brighter than Kepler magnitude 15. The resulting occurrence of planets as a function of planet radius and orbital period increases strongly toward the smallest radii (2 Earth-radii) and toward longer orbital periods ( up to 50 days, 0.25 AU). Summing over all orbital periods (P<50 d), the distribution of planet radii increases rapidly with smaller planet size. This high occurrence of smaller planets supports core-accretion theory but disagrees with the theory of migration in a gaseous disk that predicts a desert at Super-Earth and Neptune sizes for close-in orbits, which is not seen. Planets with orbital periods less than 2 days are extremely rare. We explore the densities of exoplanets by finding self-consistent mappings from the distributions of planet radius (from Kepler) to mass (from Doppler).

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