Location
Havener Center, St. Pat's Ballroom C
Presentation Date
April 21, 2023, 3:15pm-4:15pm
Session
Session 4
Description
We investigated the formation of planets near resonances in the context of histories in which systems contain an outer giant planet that forms early, and inner planets form via oligarchic growth in situ. We conducted N-body dynamical simulations with a Jupiter-like planet and initial inner planet planetesimal conditions that led to the establishment of chains of resonant and near-resonant planets in situ if the giant planet were not present. Systems with the giant planet tended to produce lower mass and more numerous planets than systems without the giant planet. The systems with the giant planet tended to be more compact and closer to first order mean motion resonances than the systems without giant planets. In both scenarios, period ratios between planet pairs in the resulting systems were most commonly near the 4:3 and 3:2 resonances out of the first order mean motion resonances. We conducted and are analyzing a larger number of simulations with a broader set of initial inner planetesimal conditions.
Meeting Name
32nd Annual Spring Meeting of the NASA-Mo Space Grant Consortium
Document Type
Presentation
Document Version
Final Version
File Type
text
Language(s)
English
Rights
© 2023 The Authors, all rights reserved.
The Influence of an Outer Jupiter-like Planet on the In Situ Formation of Near Resonant Inner Super Earths
Havener Center, St. Pat's Ballroom C
We investigated the formation of planets near resonances in the context of histories in which systems contain an outer giant planet that forms early, and inner planets form via oligarchic growth in situ. We conducted N-body dynamical simulations with a Jupiter-like planet and initial inner planet planetesimal conditions that led to the establishment of chains of resonant and near-resonant planets in situ if the giant planet were not present. Systems with the giant planet tended to produce lower mass and more numerous planets than systems without the giant planet. The systems with the giant planet tended to be more compact and closer to first order mean motion resonances than the systems without giant planets. In both scenarios, period ratios between planet pairs in the resulting systems were most commonly near the 4:3 and 3:2 resonances out of the first order mean motion resonances. We conducted and are analyzing a larger number of simulations with a broader set of initial inner planetesimal conditions.
