Eccentric planets and stellar evolution as a cause of polluted white dwarfs

@article{Frewen2014EccentricPA,
  title={Eccentric planets and stellar evolution as a cause of polluted white dwarfs},
  author={S. F. N. Frewen and Brad Hansen},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2014},
  volume={439},
  pages={2442-2458}
}
  • S. Frewen, B. Hansen
  • Published 21 January 2014
  • Geology, Physics
  • Monthly Notices of the Royal Astronomical Society
A significant fraction of white dwarfs (WDs) are observed to be polluted with metals despite high surface gravities and short settling times. The current theoretical model for this pollution is accretion of rocky bodies delivered to the WD through perturbations by orbiting planets. Using N-body simulations, we examine the possibility of a single planet as the source of pollution. We determine the stability of test particles on circular orbits in systems with a single planet located at 4 au for… 
Unstable low-mass planetary systems as drivers of white dwarf pollution
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
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
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
High-eccentricity migration of planetesimals around polluted white dwarfs
Several white dwarfs with atmospheric metal pollution have been found to host small planetary bodies (planetesimals) orbiting near the tidal disruption radius. We study the physical properties and
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
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
Formation of planetary debris discs around white dwarfs – I. Tidal disruption of an extremely eccentric asteroid
25–50 per cent of all white dwarfs (WDs) host observable and dynamically active remnant planetary systems based on the presence of close-in circumstellar dust and gas and photospheric metal
Accretion of a giant planet onto a white dwarf star
TLDR
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.
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.
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
...
...

References

SHOWING 1-10 OF 60 REFERENCES
Dynamical effects of stellar mass-loss on a Kuiper-like belt
A quarter of DA white dwarfs are metal polluted, yet elements heavier than helium sink down through the stellar atmosphere on time-scales of days. Hence, these white dwarfs must be the currently
ANCIENT PLANETARY SYSTEMS ARE ORBITING A LARGE FRACTION OF WHITE DWARF STARS
Infrared studies have revealed debris likely related to planet formation in orbit around ∼30% of youthful, intermediate mass, main-sequence stars. We present evidence, based on atmospheric pollution
THE LINK BETWEEN PLANETARY SYSTEMS, DUSTY WHITE DWARFS, AND METAL-POLLUTED WHITE DWARFS
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
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
DUSTY DISKS AROUND WHITE DWARFS. I. ORIGIN OF DEBRIS DISKS
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
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
COLLISIONAL CASCADES IN PLANETESIMAL DISKS. II. EMBEDDED PLANETS
We use a multiannulus planetesimal accretion code to investigate the growth of icy planets in the outer regions of a planetesimal disk. In a quiescent minimum-mass solar nebula, icy planets grow to
INFRARED SIGNATURES OF DISRUPTED MINOR PLANETS AT WHITE DWARFS
Spitzer Space Observatory IRAC and MIPS photometric observations are presented for 20 white dwarfs with Teff ≲ 20, 000 K and metal-contaminated photospheres. A warm circumstellar disk is detected at
Can Planets Survive Stellar Evolution
We study the survival of gas planets around stars with masses in the range 1-5 M☉, as these stars evolve off the main sequence. We show that planets with masses smaller than one Jupiter mass do not
Evolution of Debris Disks
Circumstellar dust exists around several hundred main sequence stars. For the youngest stars, that dust could be a remnant of the protoplanetary disk. Mostly it is inferred to be continuously
...
...