Abstract
The Rastall gravity is the modified Einstein general relativity, in which the energy-momentum conservation law is generalized to T^{mu nu }_{~~;mu }=lambda R^{,nu }. In this work, we derive the Kerr–Newman-AdS (KN-AdS) black hole solutions surrounded by the perfect fluid matter in the Rastall gravity using the Newman–Janis method and Mathematica package. We then discuss the black hole properties surrounded by two kinds of specific perfect fluid matter, the dark energy (omega =-,2/3) and the perfect fluid dark matter (omega =-,1/3). Firstly, the Rastall parameter kappa lambda could be constrained by the weak energy condition and strong energy condition. Secondly, by analyzing the number of roots in the horizon equation, we get the range of the perfect fluid matter intensity alpha , which depends on the black hole mass M and the Rastall parameter kappa lambda . Thirdly, we study the influence of the perfect fluid dark matter and dark energy on the ergosphere. We find that the perfect fluid dark matter has significant effects on the ergosphere size, while the dark energy has smaller effects. Finally, we find that the perfect fluid matter does not change the singularity of the black hole. Furthermore, we investigate the rotation velocity in the equatorial plane for the KN-AdS black hole with dark energy and perfect fluid dark matter. We propose that the rotation curve diversity in Low Surface Brightness galaxies could be explained in the framework of the Rastall gravity when both the perfect fluid dark matter halo and the baryon disk are taken into account.
Highlights
The dark matter and dark energy are two unsolved problems in cosmology and particle physics
From Eq (31), we find that ρ + Pr + Pθ + Pφ = 0 has one zero point, Y = ρ + Pr + Pθ + Pφ is in the range [r1, ∞) in the KN-AdS spacetime with perfect fluid matter in the Rastall gravity
We find following properties of the ergosphere: (1) its size decreases with the increasing α, indicating that dark energy and perfect fluid dark matter reduce the rotational energy of the black hole; (2) its size increases with the increasing κλ in the effective range
Summary
The dark matter and dark energy are two unsolved problems in cosmology and particle physics. Today many observations, including Type Ia supernovae, cosmic microwave background (CMB), baryon acoustic oscillations (BAO), weak lensing, rotation curve and larger scale structure, etc., have revealed that the dark energy accounts for 73%, the dark matter for 23% and ordinary baryonic matter only for 4% of the total mass-energy of the universe (e.g., [1,2]) Following these observations, many theoretical models have been proposed (e.g., [3,4,5,6]). In the case of spherical symmetry, the Reissner–Nordstrom black hole space-time surrounded by perfect fluid matter in the Rastall gravity has been obtained by Heydarzade and Darabi [34]. 4, we analyze the properties of the KN-AdS black hole surrounded by perfect fluid matter in the Rastall gravity, including the energy condition, horizon structure, ergosphere and singularity.
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