Ricci Inverse Anisotropic Stellar Structures

Abstract

This paper offers novel quintessence compact relativistic spherically symmetrical anisotropic solutions under the recently developed Ricci inverse gravity Amendola et al., 2020), by employing Krori and Barua gravitational potentials, $A{r}^2=\nu (r),\&B{r}^2+C=\mu (r)$ (with A, B, and C being real constants). For this objective, a specific explicit equation of state, connecting energy density and radial pressure, i.e., $p_r=\omega \rho$, such that $0<\omega <1$, has been utilized with an anisotripic fluid source. Ricci inverse field equations are used to find the exclusive expressions of the energy density, radial and tangential stresses, and the quintessence energy density, the critical physical attributes reflecting the exceptional conduct of extremely dense matter configuration. For the observatory source stars $HerX-1$, $SAXJ1808.4-3658$ and $4U1820-30$, all the important physical quantities like energy densities, tangential and radial pressures, energy conditions, gradients, anisotropy, redshift and mass-radius functions, and stellar compactness have been worked out and analyzed graphically. It has been concluded that all of the stellar formations under consideration remain free from any undesirable central singularity and are stable.

arXiv comment14 pages, 19 figures

References in corpus (38)

• f(R) theories
• Cosmological Imprint of an Energy Component with General Equation of State
• The Case for a Positive Cosmological Lambda-term
• Modified Gravity Theories on a Nutshell: Inflation, Bounce and Late-time Evolution
• Cosmology and the Fate of Dilatation Symmetry
• Quintessence, Cosmic Coincidence, and the Cosmological Constant
• The Cosmological Constant
• k-Inflation
• Essentials of k-essence
• Strange Quark Matter and Compact Stars
• Quintessence arising from exponential potentials
• Structure formation with a self-tuning scalar field
• Nonlocal Cosmology
• The Cosmological Constant is Back
• Further stable neutron star models from f(R) gravity
• Modified non-local-F(R) gravity as the key for the inflation and dark energy
• The Robustness of Quintessence
• Curing singularities in cosmological evolution of F(R) gravity
• General relativistic polytropes for anisotropic matter: The general formalism and applications
• Cosmological perturbations and structure formation in nonlocal infrared modifications of general relativity
• Non-local gravity and dark energy
• Neutron Stars in f(R) Gravity with Perturbative Constraints
• Collapsing spherical stars in f(R) gravity
• Minimum mass-radius ratio for charged gravitational objects
• The Force of Gravity from a Lagrangian containing Inverse Powers of the Ricci Scalar
• Physically viable solutions of anisotropic spheres in $f(\mathcal{R},\mathcal{G})$ gravity satisfying the Karmarkar condition
• Neutron stars in Starobinsky model
• Cold Dark Matter Models with a Cosmological Constant
• A New Model of Quintessence Compact Stars in Rastall Theory of Gravity
• Anisotropic Quintessence stars
• Dark energy and dark matter from nonlocal ghost-free gravity theory
• Anisotropic Strange Quintessence Stars in $f(R)$ Gravity
• Initial conditions for Inflation in an FRW Universe
• Study of Anisotropic Compact Stars with Quintessence Field and Modified Chaplygin Gas in f(T) Gravity
• Ricci-inverse gravity: a novel alternative gravity, its flaws, and how to cure them
• Tolman-Oppenheimer-Volkoff Equations in Modified Gauss-Bonnet Gravity
• Observational Constraints in Nonlocal Gravity: the Deser-Woodard Case
• Charged Anisotropic Finch-Skea-Bardeen Spheres

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• Time-Machines Construct in $f(\mathcal{R},\mathcal{A},A^{\mu \nu }{A}_{\mu \nu })$ and $f(\mathcal{R})$ Modified Gravity Theories
• Cylindrical black hole solutions in $f(\mathcal{R})$ and $f(\mathcal{R},\mathcal{A},A^{\mu \nu }{A}_{\mu \nu })$ modified gravity