Location
Toomey Hall, Room 199
Presentation Date
April 22, 2023, 8:30am-10:00am
Session
Session 5s
Description
The most common planets within 1 AU of a star are a few Earth radii in size, dubbed ‘super-Earths.’ Yet the Solar system lacks a super-Earth, and potentially the presence of Jupiter played a role. For this project, the outcomes of in situ inner planet formation under the influence of a massive outer planet were analyzed. Ninety-two N-body dynamical simulations were conducted of the in-situ formation process with a Jupiter-mass planet at a distance of five astronomical units from a host star. These simulations were then compared with the same inner planet conditions without a massive outer planet. The simulations were conducted in two stages: 1) during the residual protoplanetary disk phase with damped orbit eccentricities and 2) post-disk dispersal with subsequent dynamical evolution. It was found that systems produced more planets at lower surface densities. The average mass and eccentricity in the cases with no Jupiter were higher in stage two compared to the massive planet present. There was a tendency for the average number of planets produced to be higher in simulations with Jupiter, especially at different solid surface density ranges.
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.
Investigating Outcomes of Inner Planet Formation Influenced by a Jupiter-like Perturber
Toomey Hall, Room 199
The most common planets within 1 AU of a star are a few Earth radii in size, dubbed ‘super-Earths.’ Yet the Solar system lacks a super-Earth, and potentially the presence of Jupiter played a role. For this project, the outcomes of in situ inner planet formation under the influence of a massive outer planet were analyzed. Ninety-two N-body dynamical simulations were conducted of the in-situ formation process with a Jupiter-mass planet at a distance of five astronomical units from a host star. These simulations were then compared with the same inner planet conditions without a massive outer planet. The simulations were conducted in two stages: 1) during the residual protoplanetary disk phase with damped orbit eccentricities and 2) post-disk dispersal with subsequent dynamical evolution. It was found that systems produced more planets at lower surface densities. The average mass and eccentricity in the cases with no Jupiter were higher in stage two compared to the massive planet present. There was a tendency for the average number of planets produced to be higher in simulations with Jupiter, especially at different solid surface density ranges.
