Origin of debris disks and the supply of metals in DZ white dwarfs

Details Origin of debris disks and the supply of metals in DZ white dwarfs Origin of debris disks and the supply of metals in DZ white dwarfs

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008iaus..249..389w&link_type=abstract

Exoplanets: Detection, Formation and Dynamics, Proceedings of the International Astronomical Union, IAU Symposium, Volume 249, p

Mathematics

Probability

1

Giant Planet, Debris Disks, Planet Dynamic, N-Body Simulations, White Dwarfs

Scientific paper

We discuss the dynamical evolution of minor planetary bodies in the outer regions of planetary systems around the progenitors of DZ white dwarfs. We show that during the planetary-nebula phase of these stars, mass loss can lead to the expansion of all planetary bodies. The orbital eccentricity of the minor bodies, as relics of planetesimals, may be largely excited by the perturbation due to both gas drag effects and nearby gas giant planets. Some of these bodies migrate toward the host star, while others are scattered out of the planetary system. The former have modest probability of being captured by the sweeping secular resonances of giant planets, and induced to migrate toward the host star. When they venture close to their host stars, their orbits are tidally circularized so that they form compact disks where they may undergo further collisionally driven evolution. During the subsequent post main sequence evolution of their host stars, this process may provide an avenue which continually channels heavy elements onto the surface of the white dwarfs. We suggest that this scenario provides an explanation for the recently discovered Calcium line variation in G29-38.

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