Effects of non-Kozai mutual inclinations on two-planet system stability through all phases of stellar evolution

Veras, Dimitri; Georgakarakos, Nikolaos; Gänsicke, B. T.; Dobbs-Dixon, Ian

doi:10.1093/mnras/sty2409

Cited by 34 publications

(27 citation statements)

References 129 publications

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“…This au-scale assumption about where major planets should orbit a white dwarf is well-founded because planets on tight orbits are engulfed by the star during the giant branch phases (Kunitomo et al 2011 Gallet et al 2017;Rao et al 2018;Sun et al 2018). No major planets should exist within about 1-2 au of a white dwarf unless they are perturbed there by other major planets (Debes & Sigurdsson 2002;Veras et al 2013Veras et al , 2016Veras et al , 2018Voyatzis et al 2013;Mustill et al 2014;Veras & Gänsicke 2015;Ronco et al 2020). Indeed, until 2019, no major planets in such tight orbits were detected, despite the discoveries of several minor planets (Vanderburg et al 2015;Manser et al 2019;Vanderbosch et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Short-term stability of particles in the WD J0914+1914 white dwarf planetary system

Zotos

Veras

Saeed

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Nearly all known white dwarf planetary systems contain detectable rocky debris in the stellar photosphere. A glaring exception is the young and still evolving white dwarf WD J0914+1914, which instead harbours a giant planet and a disc of pure gas. The stability boundaries of this disc and the future prospects for this white dwarf to be polluted with rocks depend upon the mass and orbit of the planet, which are only weakly constrained. Here we combine an ensemble of plausible planet orbits and masses to determine where observers should currently expect to find the outer boundary of the gas disc. We do so by performing a sweep of the entire plausible phase space with short-term numerical integrations. We also demonstrate that particle-star collisional trajectories, which would lead to the (unseen) signature of rocky metal pollution, occupy only a small fraction of the phase space, mostly limited to particle eccentricities above 0.75. Our analysis reveals that a highly inflated planet on a near-circular orbit is the type of planet which is most consistent with the current observations.

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Section: Introductionmentioning

confidence: 99%

Short-term stability of particles in the WD J0914+1914 white dwarf planetary system

Zotos

Veras

Saeed

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…The inclinations are also randomly selected from a Rayleigh distribution with σ = 1.12 • (Xie et al 2016). Choosing small but non-zero inclination angles is adequate for global stability studies (Veras et al 2018).…”

Section: Initial Orbitsmentioning

confidence: 99%

Understanding the origin of white dwarf atmospheric pollution by dynamical simulations based on detected three-planet systems

Maldonado,

Villaver,

Mustill

et al. 2020

Preprint

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Between 25 -50 % of white dwarfs (WD) present atmospheric pollution by metals, mainly by rocky material, which has been detected as gas/dust discs, or in the form of photometric transits in some WDs. Planets might be responsible for scattering minor bodies that can reach stargazing orbits, where the tidal forces of the WD can disrupt them and enhance the chances of debris to fall onto the WD surface. The planet-planet scattering process can be triggered by the stellar mass-loss during the post main-sequence evolution of planetary systems. In this work, we continue the exploration of the dynamical instabilities that can lead to WD pollution. In a previous work we explored two-planet systems found around main-sequence (MS) stars and here we extend the study to three-planet system architectures. We evolved 135 detected three-planet systems orbiting MS stars to the WD phase by scaling their orbital architectures in a way that their dynamical properties are preserved by using the N-body integrator package Mercury. We find that 100 simulations (8.6 %) are dynamically active (having planet losses, orbit crossing and scattering) on the WD phase, where low mass planets (1-100 M ⊕ ) tend to have instabilities in Gyr timescales while high mass planets (> 100 M ⊕ ) decrease the dynamical events more rapidly as the WD ages. Besides, 19 simulations (1.6 %) were found to have planets crossing the Roche radius of the WD, where 9 of them had planet-star collisions. Our three-planet simulations have an slight increase percentage of simulations that may contribute to the WD pollution than the previous study involving two-planet systems and have shown that planetplanet scattering is responsible of sending planets close to the WD, where they may collide directly to the WD, become tidally disrupted or circularize their orbits, hence producing pollution on the WD atmosphere.

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“…Regarding the inclination of the planet orbits, we have also randomly selected them from a Rayleigh distribution with σ = 1.12 • (Xie et al 2016). The choice of using small inclination angles is justified in this work since Veras et al (2018) concluded that near co-planar angles are adequate for global stability studies.…”

Section: Initial Orbitsmentioning

confidence: 99%

Dynamical evolution of two-planet systems and its connection with white dwarf atmospheric pollution

Maldonado,

Villaver,

Mustill

et al. 2020

Preprint

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Asteroid material is detected in white dwarfs (WDs) as atmospheric pollution by metals, in the form of gas/dust discs, or in photometric transits. Within the current paradigm, minor bodies need to be scattered, most likely by planets, into highly eccentric orbits where the material gets disrupted by tidal forces and then accreted onto the star. This can occur through a planet-planet scattering process triggered by the stellar mass loss during the post main-sequence evolution of planetary systems. So far, studies of the N-body dynamics of this process have used artificial planetary system architectures built ad hoc. In this work, we attempt to go a step further and study the dynamical instability provided by more restrictive systems, that, at the same time allow us an exploration of a wider parameter space: the hundreds of multiple planetary systems found around main-sequence (MS) stars. We find that most of our simulated systems remain stable during the MS, Red and Asymptotic Giant Branch and for several Gyr into the WD phases of the host star. Overall, only ≈ 2.3 % of the simulated systems lose a planet on the WD as a result of dynamical instability. If the instabilities take place during the WD phase most of them result in planet ejections with just 5 planetary configurations ending as a collision of a planet with the WD. Finally 3.2 % of the simulated systems experience some form of orbital scattering or orbit crossing that could contribute to the pollution at a sustained rate if planetesimals are present in the same system.

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Effects of non-Kozai mutual inclinations on two-planet system stability through all phases of stellar evolution

Cited by 34 publications

References 129 publications

Short-term stability of particles in the WD J0914+1914 white dwarf planetary system

Short-term stability of particles in the WD J0914+1914 white dwarf planetary system

Understanding the origin of white dwarf atmospheric pollution by dynamical simulations based on detected three-planet systems

Dynamical evolution of two-planet systems and its connection with white dwarf atmospheric pollution

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