Issue |
A&A
Volume 694, February 2025
|
|
---|---|---|
Article Number | A236 | |
Number of page(s) | 8 | |
Section | Planets, planetary systems, and small bodies | |
DOI | https://doi.org/10.1051/0004-6361/202452632 | |
Published online | 18 February 2025 |
Dynamics of the β Pictoris planetary system and possibility of an additional planet
1
Univ. Grenoble Alpes, CNRS, IPAG,
38000
Grenoble,
France
2
Department of Astronomy and Steward Observatory, University of Arizona,
933 N Cherry Ave.,
Tucson,
AZ
85719,
USA
3
Department of Astronomy, University of California,
Berkeley,
CA
94720,
USA
★ Corresponding author; antoine.lacquement@univ-grenoble-alpes.fr
Received:
16
October
2024
Accepted:
27
December
2024
Context. The β Pictoris system is a well-known young planetary system, extensively studied for more than 40 years. It is characterized by a dusty debris disk, in addition to the presence of two already known planets. This makes it a particularly interesting case for studying the formation and evolution of planetary systems at a stage where giant planets have already formed, most of the protoplanetary gas has dissipated, and terrestrial planets could emerge.
Aims. Our goal here is to explore the possibility of additional planets orbiting beyond the outermost known one, β Pictoris b. More specifically, we aim to assess whether additional planets in the system could explain the discrepancy between the predicted cutoff of the disk inner cavity at ~28 au with only two planets, and the observed one at ~50 au.
Methods. We performed an exhaustive dynamical modeling of the debris disk and the carving of its inner edge, by introducing one or two additional planets beyond β Pictoris b, coplanar with the disk. Guided by theoretical predictions for the parameter space – mass, semi-major axis, eccentricity – allowed for additional planets, we further carried out a set of N-body simulations, using the symplectic integrator RMVS3.
Results. Our simulations indicate that an additional planet with a low eccentricity of 0.05, a mass between 0.15 and 1 MJup, and a semi-major axis between 30 and 36 au would be consistent with the observations of an inner debris disk edge at 50 au. We also explored the hypotheses of a higher eccentricity and the presence of two additional lower-mass planets instead of one, which could also account for these observations.
Conclusions. While we find that one or even two additional planets could explain the observed location of the disk inner edge, these hypothetical planets remain in most cases below the current observational limits of high-contrast imaging. Future observational campaigns with improved sensitivity will help to lower these limits and perhaps detect that planet.
Key words: methods: numerical / celestial mechanics / planets and satellites: dynamical evolution and stability / planet–disk interactions / planetary systems / stars: individual: β Pictoris
© The Authors 2025
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
This article is published in open access under the Subscribe to Open model. Subscribe to A&A to support open access publication.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.