How the presence of a giant planet affects the outcome of terrestrial planet formation simulations
(2024) In Astronomy and Astrophysics 687.- Abstract
The architecture and masses of planetary systems in the habitable zone could be strongly influenced by the presence of outer giant planets. Here, we investigate the impact of outer giants on terrestrial planet formation, under the assumption that the final assembly of the planetary system is set by a giant impact phase. Utilizing a state-of-the-art N-body simulation software, GENGA, we interpret how the late stage of terrestrial planet formation contributes to diversity among planetary systems. We designed two global model setups: 1) we placed a gas giant on the outer side of planetesimals and embryo disk and 2) we only included planetesimals and embryos, but no giant. For the model including the outer giant, we studied the effect of... (More)
The architecture and masses of planetary systems in the habitable zone could be strongly influenced by the presence of outer giant planets. Here, we investigate the impact of outer giants on terrestrial planet formation, under the assumption that the final assembly of the planetary system is set by a giant impact phase. Utilizing a state-of-the-art N-body simulation software, GENGA, we interpret how the late stage of terrestrial planet formation contributes to diversity among planetary systems. We designed two global model setups: 1) we placed a gas giant on the outer side of planetesimals and embryo disk and 2) we only included planetesimals and embryos, but no giant. For the model including the outer giant, we studied the effect of different giant initial masses in the range of 1.0–3.0 Jupiter masses, as well as a range of orbital radii from 2.0–5.8 AU. We also studied the influence of different initial positions of planetesimals and embryos on the results. Our N-body simulation time is approximately 50 Myr. The results show that the existence of an outer giant will promote the interaction between planetesimals and embryos, making the orbits of the formed terrestrial planets more compact. However, placing the giant planet too close to the planetesimals and embryo disk suppresses the formation of massive rocky planets. In addition, under the classical theory, where planetary embryos and planetesimals collide to form terrestrial planets, our results show that the presence of a giant planet actually decreases the gap complexity of the inner planetary system.
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- author
- Kong, Zhihui ; Johansen, Anders LU ; Lambrechts, Michiel LU ; Jiang, Jonathan H. and Zhu, Zong Hong
- organization
- publishing date
- 2024-07
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- planetary systems, planets and satellites: dynamical evolution and stability, planets and satellites: formation, planets and satellites: terrestrial planets, protoplanetary disks
- in
- Astronomy and Astrophysics
- volume
- 687
- article number
- A121
- publisher
- EDP Sciences
- external identifiers
-
- scopus:85197652191
- ISSN
- 0004-6361
- DOI
- 10.1051/0004-6361/202349043
- language
- English
- LU publication?
- yes
- id
- f484bbe7-4af6-41ce-b55d-d1dc243a8c22
- date added to LUP
- 2024-09-30 14:01:34
- date last changed
- 2024-09-30 14:02:01
@article{f484bbe7-4af6-41ce-b55d-d1dc243a8c22,
abstract = {{<p>The architecture and masses of planetary systems in the habitable zone could be strongly influenced by the presence of outer giant planets. Here, we investigate the impact of outer giants on terrestrial planet formation, under the assumption that the final assembly of the planetary system is set by a giant impact phase. Utilizing a state-of-the-art N-body simulation software, GENGA, we interpret how the late stage of terrestrial planet formation contributes to diversity among planetary systems. We designed two global model setups: 1) we placed a gas giant on the outer side of planetesimals and embryo disk and 2) we only included planetesimals and embryos, but no giant. For the model including the outer giant, we studied the effect of different giant initial masses in the range of 1.0–3.0 Jupiter masses, as well as a range of orbital radii from 2.0–5.8 AU. We also studied the influence of different initial positions of planetesimals and embryos on the results. Our N-body simulation time is approximately 50 Myr. The results show that the existence of an outer giant will promote the interaction between planetesimals and embryos, making the orbits of the formed terrestrial planets more compact. However, placing the giant planet too close to the planetesimals and embryo disk suppresses the formation of massive rocky planets. In addition, under the classical theory, where planetary embryos and planetesimals collide to form terrestrial planets, our results show that the presence of a giant planet actually decreases the gap complexity of the inner planetary system.</p>}},
author = {{Kong, Zhihui and Johansen, Anders and Lambrechts, Michiel and Jiang, Jonathan H. and Zhu, Zong Hong}},
issn = {{0004-6361}},
keywords = {{planetary systems; planets and satellites: dynamical evolution and stability; planets and satellites: formation; planets and satellites: terrestrial planets; protoplanetary disks}},
language = {{eng}},
publisher = {{EDP Sciences}},
series = {{Astronomy and Astrophysics}},
title = {{How the presence of a giant planet affects the outcome of terrestrial planet formation simulations}},
url = {{http://dx.doi.org/10.1051/0004-6361/202349043}},
doi = {{10.1051/0004-6361/202349043}},
volume = {{687}},
year = {{2024}},
}