  We investigate the long-term evolution and observability of remnants
originating from the merger of compact binary systems and discuss the
differences to supernova remnants. Compact binary mergers expel much smaller
amounts of mass at much higher velocities, as compared to supernovae, which
will affect the dynamical evolution of their remnants. The ejecta of mergers
consist of very neutron rich nuclei. Some of these neutron rich nuclei will
produce observational signatures in form of gamma ray lines during their decay.
The composition of the ejecta might even give interesting constraints about the
internal structure of the neutron star. We further discuss the possibility that
merger remnants appear as recently discovered 'dark accelerators' which are
extended TeV sources which lack emission in other bands.
