eccentric planets

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A quickly progressing field •Incredible wealth of data provided by already flying space mission (e.g. CoRoT and Kepler). More to come. •Field observationally driven. Formation theory struggles to keep up... Observation and theory often don’t match well. •Common characteristic: provide observations of a large number of exoplanets. This data should therefore be treated as a statistical ensemble. This could help. Venus Earth Mars Jupiter Saturn Uranus Neptune
Overview on observed exoplanet properties • Extrasolar planets exhibit a very large diversity (all techniques). • Frequencies -Low mass close-in planets: approx. 50 % (radial velocity) -Jovian planets inside a few AU: approx. 10-15 % (rv) -Hot Jupiters: 0.5-1% (rv, transits) -Cold Neptunes are common (microlensing) -Overall (FGK stars): any mass, P
Page 1 and 2: Observational constraints from the
Page 3 and 4: 6. Properties of extrasolar planets
Page 5: Different techniques - different co
Page 9 and 10: 6.1 a-M diagram
Page 11 and 12: Frequency of planet types Bias-corr
Page 13 and 14: ∼15 MJup, with an upper mass limi
Page 15 and 16: Grether & Lineweaver 2006 Mass dist
Page 17 and 18: ative points of view invoke in situ
Page 19 and 20: 6.4 Eccentricity distribution
Page 21 and 22: 6.5 Metallicity
Page 23 and 24: N. Santos et al. (2005) Metallicity
Page 25 and 26: Sousa et al. 2011 Metallicity effec
Page 27 and 28: Influence of the host star mass •
Page 29 and 30: Multiplicity •Fraction of giant p
Page 31 and 32: Kepler multiple systems •Kepler h
Page 33 and 34: or stems directly from 35% rms unce
Page 35 and 36: M-R: Giant planets •During evolut
Page 37 and 38: Additional observations
Page 39 and 40: Transits: correlation planetary cor

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