The chemical diversity of exo-terrestrial planetary debris around white   dwarfs
  We present HST ultraviolet spectroscopy of the white dwarfs PG0843+516, PG1015+161, SDSS1228+1040, and GALEX1931+0117, which accrete circumstellar planetary debris formed from the destruction of asteroids. Combined with optical data, a minimum of five and a maximum of eleven different metals are detected in their photospheres. With metal sinking time scales of only a few days, these stars are in accretion/diffusion equilibrium, and the photospheric abundances closely reflect those of the circumstellar material. We find C/Si ratios that are consistent with that of the bulk Earth, corroborating the rocky nature of the debris. Their C/O values are also very similar to those of bulk Earth, implying that the planetary debris is dominated by Mg and Fe silicates. The abundances found for the debris at the four white dwarfs show substantial diversity, comparable at least to that seen across different meteorite classes in the solar system. PG0843+516 exhibits significant over-abundances of Fe and Ni, as well as of S and Cr, which suggests the accretion of material that has undergone melting, and possibly differentiation. PG1015+161 stands out by having the lowest Si abundance relative to all other detected elements. The Al/Ca ratio of the planetary debris around different white dwarfs is remarkably similar. This is analogous to the nearly constant abundance ratio of these two refractory lithophile elements found among most bodies in the solar system. Based on the detection of all major elements of the circumstellar debris, we calculate accretion rates of ~1.7e8g/s ~1.5e9g/s. We detect additional circumstellar absorption in the SiIV 1394,1403 doublet in PG0843+516 and SDSS1228+1040, reminiscent to similar high-ionisation lines seen in white dwarfs in cataclysmic variables. We suspect that these lines originate in hot gas close to the white dwarf, well within the sublimation radius. 
B.T. Gaensicke, D. Koester, J. Farihi, J. Girven, S.G. Parsons, E.   Breedt
astro-ph.EP