eccentric planets

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Mass distribution II: new view (w. low masses) Mayor et al. 2011 uncorrected for obs. bias corrected for obs. bias Mayor et al. 2011 •RV: thanks to 1 m/s precision observations, a new huge population of low mass planets has emerged in the last few years (mostly planets found by HARPS). •bi (tri?) modal distribution: minimum at about 30 Earth masses. Imprint of formation? •neptunian bump: strong increase between 30-15 ME. •overall maximum at small masses •more than 50% of solar-type stars harbor at least one planet of any mass and with period up to 100 days (!)
Grether & Lineweaver 2006 Mass distribution III: upper boundary desert • less than 0.6 % of Sun-like stars have a brown-dwarf companion: so called “Brown dwarf desert” •mass distribution function shows a lack of objects between 25-45 MJ. Upper end of planet mass distribution? •Nothing particular is seen at 13 MJ (Dburning limit). Sahlmann et al. 2010 Segresan et al. A distinction of BD vs. planets based on formation seems advisable, but difficult to realize in practice.
Page 1 and 2: Observational constraints from the
Page 3 and 4: 6. Properties of extrasolar planets
Page 5 and 6: Different techniques - different co
Page 7 and 8: Overview on observed exoplanet prop
Page 9 and 10: 6.1 a-M diagram
Page 11 and 12: Frequency of planet types Bias-corr
Page 13: ∼15 MJup, with an upper mass limi
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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