Newtonian Cosmology and Evolution of κ-Deformed Universe

Harikumar, E.; Sreekumar, Harsha; Panja, Suman Kumar

doi:10.3390/universe9070343

Cited by 2 publications

(3 citation statements)

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“…Here, we consider the interior of the star to be a static perfect fluid, and hence, we take ûµ = (ce −ν(r)/2 , 0, 0, 0). Thus, only diagonal components of Equation (35) will survive and these are T00 = c 2 e ν(r) ρ…”

Section: Einstein's Field Equation In the κ-Deformed Space-timementioning

confidence: 99%

“…Recently, various aspects of non-commutative gravity and corresponding physics have been investigated. The effects of the κ-deformed non-commutativity in cosmology and astrophysics have been analyzed in [32][33][34][35]. In [32], κ-deformed corrections to Hawking radiation are derived using the method of Bogoliubov coefficients.…”

Section: Introductionmentioning

confidence: 99%

“…From the κ-deformed strong energy condition, a bound on the deformation parameter has been obtained. In [35], considering space-time to be non-commutative, a detailed investigation of the evolution of the universe within the Newtonian cosmology framework has been discussed. The physics of black holes in non-commutative space-time was analyzed in [36,37].…”

Section: Introductionmentioning

confidence: 99%

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Neutron Star in Quantized Space-Time

Parai,

Harikumar

et al. 2024

Universe

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We construct and analyze a model of a neutron star in a κ-deformed space-time. This is conducted by first deriving the κ-deformed generalization of the Einstein tensor, starting from the non-commutative generalization of the metric tensor. By generalizing the energy-momentum tensor to the non-commutative space-time and exploiting the κ-deformed dispersion relation, we then set up Einstein’s field equations in the κ-deformed space-time. As we adopt a realization of the non-commutative coordinates in terms of the commutative coordinates and their derivatives, our model is constructed in terms of commutative variables. Using this, we derive the κ-deformed generalization of the Tolman–Oppenheimer–Volkoff equation. Now, by treating the interior of the star as a perfect fluid as in the commutative space-time, we investigate the modification of the neutron star’s mass due to the non-commutativity of space-time, valid up to first order in the deformation parameter. We show that the non-commutativity of space-time enhances the mass limit of the neutron star. We show that the radius and maximum mass of the neutron star depend on the deformation parameter. Further, our study shows that the mass increases as the radius increases for fixed values of the deformation parameter. We show that maximum mass and radius increase as the deformation parameter increases. We find that the mass varies from 0.26M⊙ to 3.68M⊙ as the radius changes from 8.45 km to 18.66 km. Using the recent observational limits on the upper bound of the mass of a neutron star, we find the deformation parameter to be |a|∼10−44 m. We also show that the compactness and surface redshift of the neutron star increase with its mass.

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Section: Einstein's Field Equation In the κ-Deformed Space-timementioning

confidence: 99%