Presentation on theme: "Courtney Dressing Advisor: David Charbonneau All Souls College, Oxford July 4, 2011."— Presentation transcript:
Courtney Dressing Advisor: David Charbonneau All Souls College, Oxford July 4, 2011
Number of target stars: 156,453 (58,041) Number of candidates: 1,235 (438) ◦ Orbiting 997 (375) stars Solar Subset: T eff = 4100-6100 K log g = 4.0-4.9 Kepmag < 15 Bright Dwarf Sample: T eff = 3600-7100 K
Random errors? ◦ Trend preserved for T eff = 4100-6100 K ◦ Trend preserved after Monte Carlo applying gaussian random deviates to T eff and log g Systematic stellar radius bias? ◦ Would require log g error of 1.6 dex ◦ Errors in KIC are ~0.25 dex Systematic metallicity bias? ◦ Errors on [Fe/H] in KIC are ≳0.2 dex (rms) ◦ Cannot be ruled out
More massive planets have more H/He gas Change at 4.5 M E ? Models from Fortney et al. 2007 Solar system Kepler Other surveys
Assume planets with densities above 4 g/cm 3 are primarily composed of refractory elements
Toy density models ◦ Constant density ◦ Piece-wise constant density Compared to Eta-Earth Survey ◦ Volume-limited survey of 166 GK dwarfs ◦ 35 planets detected around 24 stars ◦ Keck-HIRES ◦ See Howard et al. 2010
Planet occurrence increases with decreasing radius and increasing orbital period Smaller planets (2-4 R E ) are more common around cooler stars (metallicity effect?) Larger planets have steeper cutoffs at shorter periods than smaller planets There is a ridge of high planet occurrence from 3 days and 2 R E to 50 days and 4 R E.
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