Abstract
It is reported (Estevez-Delgado and Estevez-Delgado in Eur Phys J C 78:673, 2018) recently, that the absence of anisotropic in compact object pressure leads to a solution which is not physically acceptable due to the energy density and speed of sound can not be positive at the origin at the same time. Here, we calculate the pressure and energy density of NSs using realistic EOS predicted by a relativistic mean-field model including hyperons for isotropic and three different anisotropic pressure models such as the one of Doneva and Yazadjiev (Phys Rev D 85:124023, 2012), the one of Herrera and Barreto (Phys Rev D 88:084022, 2013), and the one of Bowers and Liang (Astrophys J 188:657, 1974). We obtain that the all of energy conditions of perfect fluid are satisfied not only by anisotropic NSs profiles but also the one of isotropic NSs.
Highlights
neutron stars (NSs) are one of the possible end-points of evolutionary high mass stars, and they are one of the densest objects in the universe
We will show that the perfect fluids energy conditions is satisfied by isotropic and anisotropic NSs profiles using realistic equation of state (EOS) predicted by relativistic mean-field (RMF) model including hyperons for three different anisotropic pressure models
Before we show that the radial and tangential pressure profiles as well as the energy density profile of static and spherically symmetric NSs within DY, HB, and BL anisotropic models and the isotropic model, we show in Fig. 1 the massradius relation of NSs predicted by the DY, HB, and BL models using NSs EOS discussed in Sect
Summary
NSs are one of the possible end-points of evolutionary high mass stars, and they are one of the densest objects in the universe. Even though significant progress in constraining EOS of NSs from maximum masses and radii that extracted from NS property observations have been made up to now, the EOS of NSs, especially in the inner core is still unknown properly We need to note that the possibility of “hyperionization puzzle” in the inner core of NSs can be solved by considering anisotropic pressure. In this present work, we will show that the perfect fluids energy conditions is satisfied by isotropic and anisotropic NSs profiles using realistic EOS predicted by relativistic mean-field (RMF) model including hyperons for three different anisotropic pressure models.
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