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An Increase in Planet Formation Efficiency around Low-Mass Stars Gijs Mulders, Ilaria Pascucci, Daniel Apai University of Arizona EOS (PI: Daniel Apai) a NASA NexSS program Mulders et al. 2015b. Disk mass: Andrews et al. 2013 Planet Formation Efficiency Low-Mass Stars have more planets? Howard et al. 2012 Johnson et al. 2007 K2: talk by Ian Crossfield Huber et al. 2014, Dressing & Charbonneau 2013 Stellar Mass vs. Effective Temperature Planet Candidates: Q1-Q16 KOIs from Mullally et al. 2014 3. Detection efficiency Detection efficiency (S/N) (Christiansen et al. 2015) Transit Probability Planet Occurrence Planet Period Distribution Mulders et al. 2015a,b Planet Radius Distribution Mulders et al. 2015a Planet Period Distribution (Q1-Q8) See Mulders et al. 2015a for details Mulders et al. 2015b Planet Radius Distribution (Q1-Q16) Mulders et al. 2015b Planet Radius Distribution (Q1-Q16) Planet Radius Distribution (Q1-Q16) 2x Mulders et al. 2015b 4x Estimating Planet Heavy Element Mass Weiss & Marcy 2014 Heavy element mass from Miller & Fortney 2011 Mulders et al. 2015b Heavy Elements Mass in Planets P<50 days Mulders et al. 2015b. Disk mass: Andrews et al. 2013 Heavy Elements <150 days More Efficient Migration of Disk Material? ? The Planet Population around Low-Mass Stars from Kepler Prime
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