Driving white dwarf metal pollution through unstable eccentric periodic orbits

Antoniadou, Kyriaki I.; Veras, Dimitri

doi:10.1051/0004-6361/201935996

Cited by 24 publications

(7 citation statements)

References 64 publications

(79 reference statements)

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“…5 and 6 could be reflective of unstable periodic orbits. Both Antoniadou & Veras (2016) and Antoniadou & Veras (2019) illustrated that, for both the circular and elliptic restricted three-body problems which include white dwarfs, unstable asteroids at high eccentricities (e 0.95) may reflect the locations of these periodic orbits. Alternatively, some periodic orbits can help to protect asteroids from polluting the white dwarf.…”

Section: Discussionmentioning

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: Discussionmentioning

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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“…Technically, the GALI method is similar to the somewhat less quantitatively definite method of sibling trajectories separation based on the exponential divergence of initially very close chaotic trajectories. This class of techniques has been used to investigate the multi-dimensional parameter space of the Solar system (Hayes 2008(Hayes , 2007, detect chaotic orbits in exoplanet systems (Makarov & Berghea 2014), and to map the stability areas of generally chaotic motion of higheccentricity and high-inclination orbits of exoasteroids orbiting white dwarfs (Antoniadou & Veras 2019). For this paper, we mostly used k = 2 because it seems to be sufficient to capture the fine detail of the chaos/regular transition zones surrounding the islands of stability.…”

Section: Detection Of Chaos By Galimentioning

confidence: 99%

Chaos over order: mapping 3D rotation of triaxial asteroids and minor planets

Макаров

Goldin²,

Tkachenko

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Celestial bodies approximated with rigid triaxial ellipsoids in a two-body system can rotate chaotically due to the time-varying gravitational torque from the central mass. At small orbital eccentricity values, rotation is short-term orderly and predictable within the commensurate spin-orbit resonances, while at eccentricity approaching unity, chaos completely takes over. Here, we present the full 3D rotational equations of motion around all three principle axes for triaxial minor planets and two independent methods of numerical solution based on Euler rotations and quaternion algebra. The domains of chaotic rotation are numerically investigated over the entire range of eccentricity with a combination of trial integrations of Euler’s equations of motion and the GALI(k) method. We quantify the dependence of the order–chaos boundaries on shape by changing a prolateness parameter, and find that the main 1:1 spin-orbit resonance disappears for specific moderately prolate shapes already at eccentricities as low as 0.3. The island of short-term stability around the main 1:1 resonance shrinks with increasing eccentricity at a fixed low degree of prolateness and completely vanishes at approximately 0.8. This island is also encroached by chaos on longer time scales indicating longer Lyapunov exponents. Trajectories in the close vicinity of the 3:2 spin-orbit resonance become chaotic at smaller eccentricities, but separated enclaves of orderly rotation emerge at eccentricities as high as 0.8. Initial perturbations of rotational velocity in latitude away from the exact equilibrium result in a spectrum of free libration, nutation, and polar wander, which is not well matched by the linearized analysis omitting the inertial terms.

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“…Our findings therefore show that a significant fraction of planetary systems around white dwarfs might be shaped by gravitational interactions, in particular resonances, occurring during the evolution of their host stars. Eccentric orbits of planets around white dwarfs generated this way might play a significant role in scattering planetesimals or asteroids (Frewen & Hansen 2014;Smallwood et al 2018;Antoniadou & Veras 2019) and maybe even smaller planets closer to the white dwarf. It could therefore be that the evolutionary scenarios discovered in this letter represent an important ingredient for understanding metal polluted white dwarfs as well as the properties of planetary systems around white dwarfs.…”

Section: Neptune Rgb Survivorsmentioning

confidence: 99%