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abstract
The effect that the presence of spherically symmetric, isothermal $(\rho \sim r^{-2})$ dark matter halos about members of binary galaxies has on the nature of tidal disruption in these systems is considered for galaxy pairs whose members possess dark matter halos extending anywhere from the edge of their visible disks out to a distance of $1$ Mpc. The frequency of tidal disruption in binary galaxy samples is then predicted and compared to that observed in these samples in an attempt to place constraints on the size of galactic dark matter halos.
