LUMINOSITY EVOLUTION OF STRANGE DWARF STARS

We study the evolution of strange dwarf stars of 0.4, 0.55, and 0.8 M. in the range of luminosities attributed to white dwarf stars. It is s hown that, if the density at the base of the normal matter envelope is slightly lower than the density at which the onset of neutron drip oc curs, these objects will have an evolution observationally indistingui shable from that corresponding to normal white dwarfs. This result is independent of the chemical composition of the high density, normal ma tter layers. However, strange dwarfs should behave very differently fr om white dwarfs in mass exchanging close binary systems.