Biology
Scientific paper
Dec 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufm.p31b1530n&link_type=abstract
American Geophysical Union, Fall Meeting 2010, abstract #P31B-1530
Biology
[5205] Planetary Sciences: Astrobiology / Formation Of Stars And Planets
Scientific paper
It has been thought that the Moon is formed by a giant impact in the late stage of the Earth formation. The impact generates a debris disk around the earth, from which the Moon is accreted. This type of satellite formation is believed to be common in the solar and extra solar systems, such as Pluto and its moon, Charon. Recent study has revealed that the initial gas mass fraction in an impact-generated disk can highly affect the satellite formation process. It also means that a satellite mass depends on the initial disk gas ratio. Machida and Abe (2004) have shown that the higher disk gas ratio creates smaller satellite mass. They have also found out that if evaporation rate exceeds 70%, no satellite can be formed from the disk since solid/liquid materials in the disk fall into the Earth or escape before the disk cooling. Wada et al. (2006) have suggested that strong shocks occur in a gas rich disk, which causes most of the disk material falls into the earth within a few days. Thus, initial disk gas ratio must be taken into account in order to understand the satellite formation process, however, its effect has not been considered carefully yet. In our work, we have investigated the disk gas ratio as a function of protoplanet mass and its material, based on the idea that impact energy and the latent heat of disk material basically define the disk gas ratio. We have performed giant impact simulations of water-icy and rocky protoplanets using Smoothed Particle Hydrodynamics (SPH) method. ANEOS and SESAME equation of states are used. As a result, the disk evaporation is negligible in a Pluto-Chaon mass-size impact, but for an Earth-Moon size, the disk evaporation rate of the water-icy protoplanet can exceed 70%, whereas that of rocky one is about 10-30%. For a 5 Earth mass size system, most of the disk material evaporates in both icy and rocky protoplanet impacts. The result suggests that protoplanet mass and its material also affect the satellite mass. In our presentation, we will also discuss the disk evolution after the debris disk formation, taking into account the disk cooling and hydrodynamic escape.
Asphaug Erik Ian
Genda Hidenori
Ida Shigeru
Nakajima Motoki
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