  We have identified two moderately hot (~18000-22000K) white dwarfs,
SDSSJ1228+1040 and SDSSJ1043+0855, which exhibit double-peaked emission lines
in the CaII 8600A triplet. These line profiles are unambiguous signatures of
gaseous discs with outer radii of ~1Rsun orbiting the two white dwarfs. Both
stars accrete from the circumstellar material, resulting in large photospheric
Mg abundances. The absence of hydrogen emission from the discs, and helium
absorption in the white dwarf photospheres demonstrates that the circumstellar
material is depleted in volatile elements, and the most likely origin of these
gaseous rings are tidally disrupted rocky asteroids. The relatively high mass
of SDSSJ1228+1040 implies that planetary systems can not only form around
4-5Msun stars, but may also survive their post main-sequence evolution.
