  Abridged: We report the discovery of two, new, rare, wide, double-degenerate
binaries that each contain a magnetic and a non-magnetic star. The components
of SDSSJ092646.88+132134.5 + J092647.00+132138.4 and SDSSJ150746.48+521002.1 +
J150746.80+520958.0 have angular separations of only 4.6 arcsec (a~650AU) and
5.1 arcsec (a~750AU), respectively. They also appear to share common proper
motions. Follow-up optical spectroscopy reveals each system to consist of a DA
and a H-rich high-field magnetic white dwarf (HFMWD). Our measurements of the
effective temperatures and the surface gravities of the DA components reveal
both to have larger masses than are typical of field white dwarfs. By assuming
that these degenerates have evolved essentially as single stars, due to their
wide orbital separations, we use them to place limits on the total ages of our
stellar systems. These argue that in each case the HFMWD is probably associated
with an early type progenitor (M_init > 2M_solar). We find that the cooling
time of SDSSJ150746.80+520958.0 (DAH) is somewhat lower than might be expected
had it followed the evolutionary path of a typical single star. This mild
discord is in the same sense as that observed for two of the small number of
other HFMWDs for which progenitor mass estimates have been made, REJ0317-853
and EG59. The mass of the other DAH, SDSSJ092646.88+132134.5, appears to be
smaller than expected on the basis of single star evolution. If this object
was/is a member of a hierarchical triple system it may have experienced greater
mass loss during an earlier phase of its life as a result of it having a close
companion. The large uncertainties on our estimates of the parameters of the
HFMWDs suggest a larger sample of these objects is required to firmly identify
any trends in their inferred cooling times and progenitor masses.
