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Hybrid star model with quark matter and baryonic matter in minimally coupled f(R) gravity
Annals of Physics ( IF 3 ) Pub Date : 2021-01-01 , DOI: 10.1016/j.aop.2020.168336
G. Abbas , H. Nazar

Abstract The present article deals with some new features of static anisotropic relativistic compact object with two fluids distribution (strange quark matter ( S Q M ) and normal baryonic matter) along with Karori-Barua ( K B ) type metric within the framework of so called f ( R ) theory of gravity. We have considered the M I T bag model equation of state (EoS) to describe the relationship between pressure and matter density for the quark matter distribution inside the celestial object. For this investigation, we have formulated the field equations in f ( R ) theory with M I T bag EoS together with K B ansatz in the background of two specific viable f ( R ) models ( f ( R ) = R + α R 2 and f ( R ) = R + α ( R 2 + ζ R 3 ) ), respectively. Further, the physical credibility of the obtained solutions have been analyzed in the form of matter variables, energy conditions, hydrostatic equilibrium equation and stability criterion by using the graphical representation for different choices of free parameter α . Moreover, we have evaluated that the matter density and radial pressure are central singularity free and remain finite throughout the interior of the fluid sphere. The numerical values of such parameters and bag constant have been calculated corresponding to different compact star candidates ( S A X J 1808 . 4 -3658 ( x = 7 . 07 K m ), 4 U 1820 -30 ( x = 10 K m ) and P S R J 1614 -2230 ( x = 10 . 3 K m )). Finally, we have observed that our proposed compact star candidate with two viable f ( R ) models, satisfies all the necessary and sufficient conditions for potentially stable configuration, which are quite suitable to test the strange star candidates.

中文翻译:

夸克物质和重子物质在最小耦合 f(R) 引力下的混合星模型

摘要 本文讨论了具有两种流体分布(奇异夸克物质 ( SQM ) 和正常重子物质)以及 Karori-Barua ( KB ) 型度量的静态各向异性相对论致密物体的一些新特征,即所谓的 f ( R ) 引力理论。我们已经考虑了 MIT 袋模型状态方程 (EoS) 来描述天体内部夸克物质分布的压力和物质密度之间的关系。对于这项研究,我们在两个特定可行的 f ( R ) 模型 ( f ( R ) = R + α R 2 和 f ( R ) = R + α ( R 2 + ζ R 3 ) )。进一步,以物质变量的形式分析了所得解的物理可信度,通过使用自由参数 α 的不同选择的图形表示,可以得到能量条件、流体静力平衡方程和稳定性准则。此外,我们已经评估了物质密度和径向压力是无中心奇点的,并且在整个流体球内部保持有限。这些参数和袋常数的数值已经根据不同的候选致密星(SAXJ 1808 . 4 -3658 ( x = 7 . 07 K m )、4 U 1820 -30 ( x = 10 K m ) 和 PSRJ 1614 进行计算-2230 ( x = 10 . 3 K m ))。最后,我们观察到我们提出的具有两个可行 f ( R ) 模型的致密恒星候选者满足潜在稳定配置的所有必要和充分条件,非常适合测试奇异恒星候选者。通过使用自由参数α的不同选择的图形表示,流体静力平衡方程和稳定性准则。此外,我们已经评估了物质密度和径向压力是无中心奇点的,并且在整个流体球内部保持有限。这些参数和袋常数的数值已经根据不同的候选致密星(SAXJ 1808 . 4 -3658 ( x = 7 . 07 K m )、4 U 1820 -30 ( x = 10 K m ) 和 PSRJ 1614 进行了计算) -2230 ( x = 10 . 3 K m ))。最后,我们观察到我们提出的具有两个可行 f ( R ) 模型的致密恒星候选者满足潜在稳定配置的所有必要和充分条件,非常适合测试奇异恒星候选者。通过使用自由参数α的不同选择的图形表示,流体静力平衡方程和稳定性准则。此外,我们已经评估了物质密度和径向压力是无中心奇点的,并且在整个流体球内部保持有限。这些参数和袋常数的数值已经根据不同的候选致密星(SAXJ 1808 . 4 -3658 ( x = 7 . 07 K m )、4 U 1820 -30 ( x = 10 K m ) 和 PSRJ 1614 进行了计算) -2230 ( x = 10 . 3 K m ))。最后,我们观察到我们提出的具有两个可行 f ( R ) 模型的致密恒星候选者满足潜在稳定配置的所有必要和充分条件,非常适合测试奇异恒星候选者。
更新日期:2021-01-01
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