  The recent identification of several groups of young stars within 100 parsecs
of the Sun has generated widespread interest. Given their proximity and
possible age differences, these systems are ideally suited for detailed studies
of star and planet formation. Here we report on the first investigation of
protoplanetary disks in one such group, the high-latitude cloud MBM 12 at a
distance of $\sim$65 pc. We present mid-infrared observations of the eight
candidate pre-main-sequence (PMS) members and the two main-sequence (MS) stars
in the same line-of-sight which may or may not be associated with the group. We
have also derived H$\alpha$ and Li line widths from medium-resolution optical
spectra. We report the discovery of significant mid-infrared excess from six
PMS stars --LkH$\alpha$ 262, LkH$\alpha$ 263, LkH$\alpha$ 264, E02553+2018,
RXJ0258.3+1947 and S18 --presumably due to optically thick circumstellar disks.
Our flux measurements for the other two PMS stars and the two MS stars are
consistent with photospheric emission, allowing us to rule out dusty inner
disks. The disks we have found in MBM 12 represent the nearest known sample of
very young protoplanetary systems, and thus are prime targets for
high-resolution imaging at infrared and millimeter wavelengths.
