Analytical model on mass limits of strange stars

In this paper, we present a new kind of stellar model using the Nariai IV metric. This model can be used to study the strange/quark stars (which is our current interest, although it can also be applicable to neutron stars). We present a mass-radius region where all regularity conditions, energy conditions, the TOV equation, and stability conditions are satisfied. According to our model, strange stars with masses up to 1.9165M(circle dot) (= 2.81 km) are stable. A strange star with a mass greater than 1.9165M(circle dot) violates the stability conditions. This model can be very useful to predict the radius of strange stars with a mass greater than 1M(circle dot).