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

Discovery of Gas Accretion Onto Stars in 13 Myr old h and chi Persei