Galactic stellar mass binaries have been suggested as both unresolved (WD-WD) and resolved (NS-NS,BH-BH)
LISA sources.  Such binaries, particularly BH-BH, may be rare due to mergers during mass transfer or
disruption during supernovae.  They are often assumed to be circular due to tidal effects and 
gravitational wave radiation.  I have studied BH-BH binaries in star clusters where dynamics may both
form new BH-BH binaries and impart significant eccentricity in binaries already in the LISA frequency 
regime.  I will report on the results of several simulations I have performed investigating the number
and parameters of BH-BH binaries in the LISA band.  I consider binaries that remain within clusters
and those that have escaped clusters and now reside in the galactic field.