eccentric planets

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No metallicity effect for low mass planets Mayor et al. 2011 •HARPS high precision sample: [Fe/H] for giant gaseous planets (black), for planets less massive than 30 ME (red), and for the global combined sample stars (blue). •No metallicity effect for low mass planets. •Even absence of low mass planets at high [Fe/H]? •Natural outcome in the core accretion formation model. ? ? Mayor et al. 2011
Sousa et al. 2011 Metallicity effect as function of mass •The division between metalophile and not metalophile planets coincides with a minimum in the planetary mass function. (ca. 30 ME) •Different populations: Giant planets (w. gas runaway accretion) vs. Neptunian planets. •Correlation with other elemental abundances in the stars are less clear (maybe Lithium-planet anticorrelation).
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 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: N. Santos et al. (2005) Metallicity
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

eccentric planets

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