  I examine the hypothesis that many of the high velocity white dwarfs observed
by Oppenheimer et al. (2001) are the remnants of donor stars from binaries that
produced type Ia supernovae via the `single degenerate' channel. If this
channel is a significant contributor to the Galactic SN Ia supernova rate, then
the local density of such remnants with V>100 km/s could be as high as 2.e-4
per cubic parsec, comparable to the densities found by Oppenheimer et al. This
white dwarf population differs from others in that it is composed exclusively
of single stars.
