  We report the discovery of accretion disks associated with ~ 13 Myr-old
intermediate/low-mass stars in h and chi Persei. Optical spectroscopy of ~ 5000
stars in these clusters and a surrounding halo population reveal 32 A-K stars
with H(alpha) emission. Matching these stars with 2MASS and optical photometry
yields 25 stars with the highest probability of cluster membership and
EW(H(alpha)) > 5 angstroms. Sixteen of these sources have EW(H(alpha)) > 10
angstroms. The population of accreting sources is strongly spectral type
dependent: H(alpha) emission characteristic of accretion, especially strong
accretion (EW(H(alpha)) > 10 angstroms), is much more prevalent around stars
later than G0. Strong H(alpha) emission from accretion is typically associated
with redder Ks-[8] colors. The existence of accreting pre-main sequence stars
in h and chi Persei implies that circumstellar gas in some systems, especially
those with primaries later than G5 spectral type, can last longer than 10-15
Myr.
