Abstract
Some of the observed pulsars can be identified with ordinary neutron stars. If strange matter is stable, the central density of the neutron stars should be lower than the critical density of the quark-hadron phase transition occurring due to the strong interactions only. The quark matter being formed turns to more stable strange matter on a weak interaction time scale, converting neutron stars into strange stars. The requirement of stability of old and newly born hot neutron stars with respect to the phase transition is used to constrain the binding energy of strange matter.
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