Planetary Formation Scenarios Revisited: Core-Accretion versus Disk Instability

@inproceedings{Matsuo2007PlanetaryFS,
  title={Planetary Formation Scenarios Revisited: Core-Accretion versus Disk Instability},
  author={T. Matsuo and H. Shibai and T. Ootsubo and M. Tamura},
  year={2007}
}
  • T. Matsuo, H. Shibai, +1 author M. Tamura
  • Published 2007
  • Physics
  • The core-accretion and disk instability models have so far been used to explain planetary formation. These models have different conditions, such as planet mass, disk mass, and metallicity for formation of gas giants. The core-accretion model has a metallicity condition ([Fe/H] > -1.17 in the case of G-type stars), and the mass of planets formed is less than 6 times that of the Jupiter mass MJ. On the other hand, the disk instability model does not have the metallicity condition, but requires… CONTINUE READING

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