Unstable low-mass planetary systems as drivers of white dwarf pollution

  title={Unstable low-mass planetary systems as drivers of white dwarf pollution},
  author={Alexander J. Mustill and Eva Villaver and Dimitri Veras and Boris T. Gansicke and Amy Bonsor},
  journal={Monthly Notices of the Royal Astronomical Society},
At least 25 percent of white dwarfs show atmospheric pollution by metals, sometimes accompanied by detectable circumstellar dust/gas discs or (in the case of WD 1145+017) transiting disintegrating asteroids. Delivery of planetesimals to the white dwarf by orbiting planets is a leading candidate to explain these phenomena. Here, we study systems of planets and planetesimals undergoing planet–planet scattering triggered by the star's post-main-sequence mass loss, and test whether this can… 
Dynamical evolution of two-planet systems and its connection with white dwarf atmospheric pollution
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
Understanding the origin of white dwarf atmospheric pollution by dynamical simulations based on detected three-planet systems
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.
Short-term stability of particles in the WD J0914+1914 white dwarf planetary system
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
Accretion of a giant planet onto a white dwarf star
Optical spectroscopy of a hot white dwarf, WD J091405.30+191412, reveals that the chemical abundances in its disk are similar to those thought to exist deep in icy giant planets, so the white dwarf must be accreting a giant planet.
Orbital relaxation and excitation of planets tidally interacting with white dwarfs
Observational evidence of white dwarf planetary systems is dominated by the remains of exo-asteroids through accreted metals, debris discs, and orbiting planetesimals. However, exo-planets in these
Do instabilities in high-multiplicity systems explain the existence of close-in white dwarf planets?
We investigate the origin of close-in planets and related phenomena orbiting white dwarfs (WDs), which are thought to originate from orbits more distant from the star. We use the planetary
The dynamical history of the evaporating or disrupted ice giant planet around white dwarf WD J0914+1914
  • D. VerasJ. Fuller
  • Physics, Geology
    Monthly Notices of the Royal Astronomical Society
  • 2020
Robust evidence of an ice giant planet shedding its atmosphere around the white dwarf WD J0914+1914 represents a milestone in exoplanetary science, allowing us to finally supplement our knowledge
Planetary magnetosphere evolution around post-main-sequence stars
Accompanying the mounting detections of planets orbiting white dwarfs and giant stars are questions about their physical history and evolution, particularly regarding detectability of their
Driving white dwarf metal pollution through unstable eccentric periodic orbits
Context. Planetary debris is observed in the atmospheres of over 1000 white dwarfs, and two white dwarfs are now observed to contain orbiting minor planets. Exoasteroids and planetary core fragments
A Jovian analogue orbiting a white dwarf star.
The non-detection of a main-sequence lens star in the microlensing event MOA-2010-BLG-477Lb12 using near-infrared observations from the Keck Observatory is reported, which is evidence that planets around white dwarfs can survive the giant and asymptotic giant phases of their host's evolution, and supports the prediction that more than half ofwhite dwarfs have Jovian planetary companions.


Are There Unstable Planetary Systems around White Dwarfs
The presence of planets around solar-type stars suggests that many white dwarfs should have relic planetary systems. While planets closer than ~5 AU will most likely not survive the
Liberating exomoons in white dwarf planetary systems
Previous studies indicate that more than a quarter of all white dwarf (WD) atmospheres are polluted by remnant planetary material, with some WDs being observed to accrete the mass of Pluto in 106 yr.
A significant fraction of the mature FGK stars have cool dusty disks at least an order of magnitude brighter than the solar system's outer zodiacal light. Since such dusts must be continually
Planetary engulfment as a trigger for white dwarf pollution
The presence of a planetary system can shield a planetesimal disk from the secular gravitational perturbations due to distant outer massive objects (planets or stellar companions). As the host star
It has long been suspected that metal-polluted white dwarfs (types DAZ, DBZ, and DZ) and white dwarfs with dusty disks possess planetary systems, but a specific physical mechanism by which
Simulations of two-planet systems through all phases of stellar evolution: implications for the instability boundary and white dwarf pollution
Exoplanets have been observed at many stages of their host star's life, including the main-sequence (MS), subgiant and red giant branch stages. Also, polluted white dwarfs (WDs) likely represent
Post-main-sequence Evolution of Icy Minor Planets. II. Water Retention and White Dwarf Pollution around Massive Progenitor Stars
Most studies suggest that the pollution of white dwarf (WD) atmospheres arises from the accretion of minor planets, but the exact properties of polluting material, and in particular the evidence for
Debris disks as signposts of terrestrial planet formation
There exists strong circumstantial evidence from their eccentric orbits that most of the known extra-solar planetary systems are the survivors of violent dynamical instabilities. Here we explore the
The frequency of planetary debris around young white dwarfs
Context. Heavy metals in the atmospheres of white dwarfs are thought in many cases to be accreted from a circumstellar debris disk, which was formed by the tidal disruption of a rocky planetary body
Full-lifetime simulations of multiple unequal-mass planets across all phases of stellar evolution
We know that planetary systems are just as common around white dwarfs as around main-sequence stars. However, self-consistently linking a planetary system across these two phases of stellar evolution