Water transport and loss in planet formation: a collision outcome parameter study
- Autor(en)
- Thomas I. Maindl, Philip M. Winter, Elke Pilat-Lohinger, Nader Haghighipour, Christoph Schäfer, Christoph Burger, Rudolf Dvorak
- Abstrakt
As it is well established, the formation of terrestrial planets involves a long sequence of collisions of protoplanetary bodies. Water in particular may have been brought to the accretion zone of Earth by water-carrying planetesimals and planetary embryos from outer regions of the asteroid belt. In most simulations of planet formation, these collisions are treated as perfect inelastic merging events andconsequently ignore fragmentation and the loss of volatiles such as water. Compared to the actual out come of realistic, physical collisions, the masses as well as the water contents of the final terrestrial planets are significantly overestimated. In order to arrive at a more realistic estimate of the amount of water transported to Earth's accretion zone, we performed a suite of several hundred collisions imulations with our 3D smooth particle hydrodynamics (SPH) code. We discuss the outcome of our simulations in terms of mass and water content of final bodies and for different parameters of the system including collision velocity, impact angle, and the masses and water-mass fractions of the projectile and target. Our results present a more realistic estimate of water transport rates in dynamical studies of planet formation.
- Organisation(en)
- Institut für Astrophysik
- Externe Organisation(en)
- University of Hawaii at Manoa, Eberhard Karls Universität Tübingen
- Publikationsdatum
- 08-2018
- ÖFOS 2012
- 103003 Astronomie, 103004 Astrophysik
- Schlagwörter
- Link zum Portal
- https://ucrisportal.univie.ac.at/de/publications/ac136408-b80b-4883-a6bf-377821cf3628