Effects of Self-gravity on Mass-loss of the Post-impact Super-Earths

Abstract

Kepler's observations show most of the exoplanets are super-Earths. The formation of super-Earth is generally related to the atmospheric mass loss that is crucial in the planetary structure and evolution. The shock driven by the giant impact will heat the planet, resulting in the atmosphere escape. We focus on whether self-gravity changes the efficiency of mass loss. Without self-gravity, if the impactor mass is comparable to the envelope mass, there is a significant mass-loss. The radiative-convective boundary will shift inward by self-gravity. As the temperature and envelope mass increase, the situation becomes more prominent, resulting in a heavier envelope. Therefore, the impactor mass will increase to motivate the significant mass loss, as the self-gravity is included. With the increase of envelope mass, the self-gravity is particularly important.

References in corpus (17)

• The Occurrence and Mass Distribution of Close-in Super-Earths, Neptunes, and Jupiters
• Line and Mean Opacities for Ultracool Dwarfs and Extrasolar Planets
• Migration and the formation of systems of hot super-Earths and Neptunes
• Planetary population synthesis coupled with atmospheric escape: a statistical view of evaporation
• Kepler-62: A five-planet system with planets of 1.4 and 1.6 Earth radii in the Habitable Zone
• Ocean Planet or Thick Atmosphere: On the Mass-Radius Relationship for Solid Exoplanets with Massive Atmospheres
• Atmospheric Mass Loss During Planet Formation: The Importance of Planetesimal Impacts
• Observable Consequences of Planet Formation Models in Systems with Close-in Terrestrial Planets
• Superabundance of Exoplanet Sub-Neptunes Explained by Fugacity Crisis
• A Tale of Planet Formation: From Dust to Planets
• To cool is to keep: Residual H/He atmospheres of super-Earths and sub-Neptunes
• The Preservation of Super Earths and the Emergence of Gas Giants after Their Progenitor Cores have Entered the Pebble Isolation Phase
• The traditional approximation of rotation for rapidly rotating stars and planets. I. The impact of strong deformation
• Envelopes of embedded super-Earths I. Two-dimensional simulations
• Formation of Super-Earths by Tidally-Forced Turbulence
• Self-gravitating planetary envelopes and the core-nucleated instability
• Thermal Tides in Rotating Hot Jupiters