Presentation Information
[PPS04-P12]Crater and droplet formation by impact into liquid targets
*Toshihiko Kadono1, Sota Arakawa2, Hiroshi Kobayashi3, Takayuki Ushikubo2, Makiko Nagasawa4, Hidekazu Tanaka5 (1.University of Occupational and Environmental Health, 2.JAMSTEC, 3.Nagoya University, 4.Kurume University, 5.Tohoku University)
Keywords:
impact cratering,liquid target,droplet,chondrule
Arakawa et al. (2024 Fall Meeting of the Japanese society for planetary sciences; 2025 JpGU) propose a new chondrule formation mechanism during the evolution of the protoplanetary disk after Jupiter formation. In this mechanism, planetesimals penetrate dust layers at high velocities in the protoplanetary disk, generating large amounts of silicate melt on their surfaces. The molten particles are ejected into the dust layer, where they solidify to become chondrules.
When an impact occurs on a liquid target, the ejecta curtain breakup occurs, forming droplets (2025 Fall Meeting of the Japanese society for planetary sciences). The characteristic size of the droplets depends on the ejection velocity and the surface tension coefficient of the liquid. The ejection velocity is a function of the ejection location and is directly related to the crater formation process. On planetesimal surfaces, gravity is so small that the crater formation process is likely dominated by surface tension. Here, we conducted some experiments to investigate the crater formation process dominated by surface tension. We examined the crater size as a function of impact velocity and discussed the differences compared to the crater formation process dominated by gravity.
When an impact occurs on a liquid target, the ejecta curtain breakup occurs, forming droplets (2025 Fall Meeting of the Japanese society for planetary sciences). The characteristic size of the droplets depends on the ejection velocity and the surface tension coefficient of the liquid. The ejection velocity is a function of the ejection location and is directly related to the crater formation process. On planetesimal surfaces, gravity is so small that the crater formation process is likely dominated by surface tension. Here, we conducted some experiments to investigate the crater formation process dominated by surface tension. We examined the crater size as a function of impact velocity and discussed the differences compared to the crater formation process dominated by gravity.