A mixed stirring mechanism for debris discs with giant and dwarf planetary perturbations

Article

Munoz-Gutierrez, Marco A., Marshall, Jonathan P. and Peimbert, Antonio. 2023. "A mixed stirring mechanism for debris discs with giant and dwarf planetary perturbations." Monthly Notices of the Royal Astronomical Society. 520 (3), pp. 3218-3228. https://doi.org/10.1093/mnras/stad218
Article Title

A mixed stirring mechanism for debris discs with giant and dwarf planetary perturbations

ERA Journal ID1074
Article CategoryArticle
AuthorsMunoz-Gutierrez, Marco A., Marshall, Jonathan P. and Peimbert, Antonio
Journal TitleMonthly Notices of the Royal Astronomical Society
Journal Citation520 (3), pp. 3218-3228
Number of Pages11
Year2023
PublisherOxford University Press
Place of PublicationUnited Kingdom
ISSN0035-8711
1365-2966
Digital Object Identifier (DOI)https://doi.org/10.1093/mnras/stad218
Web Address (URL)https://academic.oup.com/mnras/article/520/3/3218/6994535
AbstractDebris discs consist of belts of bodies ranging in size from dust grains to planetesimals; these belts are visible markers of planetary systems around other stars that can reveal the influence of extrasolar planets through their shape and structure. Two key stirring mechanisms – self-stirring by planetesimals and secular perturbation by an external giant planet – have been identified to explain the dynamics of planetesimal belts; their relative importance has been studied independently, but are yet to be considered in combination. In this work, we perform a suite of 286 N-body simulations exploring the evolution of debris discs over 1 Gyr, combining the gravitational perturbations of both dwarf planets embedded in the discs, and an interior giant planet. Our systems were somewhat modelled after the architecture of the outer Solar system: a Solar mass star, a single massive giant planet at 30 au (MGP = 10 to 316 M?), and a debris disc formed by 100 massive dwarf planets and 1000 massless particles (MDD = 3.16 to 31.6 M?). We present the evolution of both the disc and the giant planet after 1 Gyr. The time evolution of the average eccentricity and inclination of the disc is strongly dependent on the giant planet mass as well as on the remaining disc mass. We also found that efficient stirring is achieved even with small disc masses. In general, we find that a mixed mechanism is more efficient in the stirring of cold debris discs than either mechanism acting in isolation.
Keywordsmethods: numerical; software: simulations; planets and satellites: dynamical evolution and stability; planet-disc interactions
ANZSRC Field of Research 2020510107. Planetary science (excl. solar system and planetary geology)
Public Notes

This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2023 The authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.

Byline AffiliationsAcademia Sinica Institute of Astronomy and Astrophysics, Taiwan
Centre for Astrophysics
National Autonomous University of Mexico, Mexico
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