Rocky planetesimals as the origin of metals in DZ stars
Article first published online: 18 MAR 2010
© 2010 The Authors. Journal compilation © 2010 RAS
Monthly Notices of the Royal Astronomical Society
Volume 404, Issue 4, pages 2123–2135, June 2010
How to Cite
Farihi, J., Barstow, M. A., Redfield, S., Dufour, P. and Hambly, N. C. (2010), Rocky planetesimals as the origin of metals in DZ stars. Monthly Notices of the Royal Astronomical Society, 404: 2123–2135. doi: 10.1111/j.1365-2966.2010.16426.x
- Issue published online: 21 MAY 2010
- Article first published online: 18 MAR 2010
- Accepted 2010 January 26. Received 2010 January 24; in original form 2009 December 3
- minor planets, asteroids;
- circumstellar matter;
- stars: abundances;
- stars: chemically peculiar;
- planetary systems;
- white dwarfs
The calcium and hydrogen abundances, Galactic positions and kinematics of 146 DZ white dwarfs from the Sloan Digital Sky Survey are analysed to constrain the possible origin of their externally polluted atmospheres. There are no correlations found between their accreted calcium abundances and spatial–kinematical distributions relative to interstellar material. Furthermore, two thirds of the stars are currently located above the Galactic gas and dust layer, and their kinematics indicate multi-Myr residences in this region where interstellar material is virtually absent.
Where detected, the hydrogen abundances for 37 DZA stars show little or no correlation with accreted calcium or spatial–kinematical distributions, though there is a general trend with cooling age. It is found that Eddington-type accretion of interstellar hydrogen can reproduce the observed hydrogen abundances, yet simultaneously fails to account for calcium. The calcium-to-hydrogen ratios for the DZA stars are dominated by supersolar values, as are the lower limits for the remaining 109 DZ stars. All together, these polluted white dwarfs currently contain 1020±2 g of calcium in their convective envelopes, commensurate with the masses of calcium inferred for large asteroids.
A census of current Teff≲ 12 000 K, helium-rich stars from the Sloan Digital Sky Survey suggests the DZ and DC white dwarfs belong to the same stellar population, with similar basic atmospheric compositions, effective temperatures, spatial distributions and Galactic space velocities. Based on this result, pollution by the interstellar medium cannot simultaneously account for both the polluted and non-polluted subpopulations. Rather, it is probable that these white dwarfs are contaminated by circumstellar matter; the rocky remains of terrestrial planetary systems.
In this picture, two predictions emerge. First, at least 3.5 per cent of all white dwarfs harbour the remnants of terrestrial planetary systems; this is a concrete lower limit and the true fraction is almost certainly, and perhaps significantly, higher. Therefore, one can infer that at least 3.5 per cent of main-sequence A- and F-type stars build terrestrial planets. Secondly, the DZA stars are externally polluted by both metals and hydrogen, and hence constrain the frequency and mass of water rich, extrasolar planetesimals.