An isotropic compact stellar model in curvature coordinate system consistent with observational data. (arXiv:2102.12754v2 [astro-ph.GA] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Kumar_J/0/1/0/all/0/1">Jitendra Kumar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bharti_P/0/1/0/all/0/1">Puja Bharti</a>
This paper investigates a spherically symmetric compact relativistic body
with isotropic pressure profiles within the framework of general relativity. In
order to solve the Einstein’s field equations, we have considered the
Vaidya-Tikekar type metric potential, which depends upon parameter K. We have
presented a perfect fluid model, considering K<0 or K>1, which represent
compact stars like SMC X-1, Her X-1, 4U 1538-52, SAX J1808.4-3658, LMC X-4, EXO
1785-248 and 4U1820-30, to an excellent degree of accuracy. We have
investigated the physical features such as the energy conditions, velocity of
sound, surface redshift, adiabatic index of the model in detail and shown that
our model obeys all the physical requirements for a realistic stellar model.
Using the Tolman-Oppenheimer-Volkoff equations, we have explored the
hydrostatic equilibrium and the stability of the compact objects. This model
also fulfils the Harrison-Zeldovich-Novikov stability criterion. The results
obtained in this paper can be used in analyzing other isotropic compact
objects.
This paper investigates a spherically symmetric compact relativistic body
with isotropic pressure profiles within the framework of general relativity. In
order to solve the Einstein’s field equations, we have considered the
Vaidya-Tikekar type metric potential, which depends upon parameter K. We have
presented a perfect fluid model, considering K<0 or K>1, which represent
compact stars like SMC X-1, Her X-1, 4U 1538-52, SAX J1808.4-3658, LMC X-4, EXO
1785-248 and 4U1820-30, to an excellent degree of accuracy. We have
investigated the physical features such as the energy conditions, velocity of
sound, surface redshift, adiabatic index of the model in detail and shown that
our model obeys all the physical requirements for a realistic stellar model.
Using the Tolman-Oppenheimer-Volkoff equations, we have explored the
hydrostatic equilibrium and the stability of the compact objects. This model
also fulfils the Harrison-Zeldovich-Novikov stability criterion. The results
obtained in this paper can be used in analyzing other isotropic compact
objects.
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