Abstract
The solution of equation of state corresponding to equality Γ=Γ3 gives non-terminating solutions for isothermal neutron star cores. Hence, for this equality, core-envelope models have been developed by taking another equation of state, corresponding to the condition Γ3, in the envelope. Various static, pulsational, and rotational parameters pertaining to neutron star models are calculated. These models are gravitationally bound and stable for radial perturbations and slow rotations.
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Fuloria, R.S., Pandey, S.C. & Durgapal, M.C. Core-envelope models for massive fluid spheres. Astrophys Space Sci 151, 255–264 (1989). https://doi.org/10.1007/BF00648383
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DOI: https://doi.org/10.1007/BF00648383