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Fig. 1


Stable and unstable regions on the baryon mass–equatorial radius MbReq plane. The lowest (red) line denotes the nonrotating configurations. The wavy pattern region denotes a region in which the back-bending phenomenon does not occur, whereas dashed lines are constant frequency tracks in a region in which back-bending occurs (lines every 100 Hz, in the range 100–1000 Hz). The solid green lines denote sequences of configurations with constant angular momentum J (1, 1.5, ..., 3, in units of ). The thick solid blue line on the left side marks the boundary of the region in which rotating axisymmetric stars are unstable with respect to axisymmetric perturbations. The red strip on the right is the instability induced by the EOS, dividing the MbReq plane into two disjoint families of solutions. Finally, the green region is the allowed twin branch part of the MbReq plane to where NSs collapse after entering the instability strip (assuming Mb = const. and J = const.).

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