Close Encounters of Planetary Embryos in Single and Binary Star Systems
- Author(s)
- Elke Pilat-Lohinger, Thomas I. Maindl, David Bancelin, Christoph M. Schäfer, Ákos Bazso
- Abstract
In numerical simulations for terrestrial planet formation one usually traces the orbital evolution of numerous protoplanetary embryos over a timespan up to 100 Myrs. When collisional fragmentation is excluded, two embryos merge completely once their mutual distance becomes smaller than a pre-defined collision threshold. It is well known that this assumption is a weak point of such studies which needs to be improved. A more sophisticated model will consider fragmentation in different collision outcome regimes (see Leinhardt and Stewart, 2012). In this study, we suggest a more realistic formation scenario that includes SPH (SmoothParticle Hydrodynamics) simulations of colliding embryos in the N-body computations. Since the SPH simulations provide the necessary information about volatile and material loss during impact this N-body-SPH combination yields a more realistic result for the growth of bodies and the water transport via collisions on terrestrial planets in the habitable zone. We show the results for collisions of Moon and Mars sized objects moving in the habitable zone of a sun-like star (i.e. between 0.9 and 1.7 au) perturbed by a Jupiter-mass planet at 3 au and a secondary star at distances of 25/50/75/100 au. Besides the comparison of the different binary-star-planet configurations we also provide a study for a similar planetary system orbiting a single star. In this context, we show the mass-loss during collision depending on the impact velocity and angle. This might modify the result of perfect merging-based N-body simulations of terrestrial planet formation.
- Organisation(s)
- Department of Astrophysics
- Publication date
- 07-2018
- Austrian Fields of Science 2012
- 103003 Astronomy, 103004 Astrophysics
- Portal url
- https://ucrisportal.univie.ac.at/en/publications/03366068-d585-4c09-86e8-092eb60dd091