Noncommutativity and logarithmic correction to the black hole entropy

Gupta, Kumar S.; Jurić, Tajron; Samsarov, Andjelo; Smolić, Ivica

doi:10.1007/jhep02(2023)060

Cited by 6 publications

(3 citation statements)

References 62 publications

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“…Taking the derivative with respect to r of Equation (38) and with the help of Equation ( 34) we obtain…”

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

confidence: 99%

“…κ-deformed corrections to the entropy of the BTZ black hole have been calculated using the brick wall method as well as using the quasinormal mode frequency of the κ-scalar field (in the background of BTZ black hole) [36,37]. Non-commutative correction to Bekenstein-Hawking entropy is obtained in [38]. Using a squashed fuzzy sphere, the super Chandrasekhar limit was calculated in [39].…”

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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“…Taking the derivative with respect to r of Equation (38) and with the help of Equation ( 34) we obtain…”

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

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Neutron Star in Quantized Space-Time

Parai,

Harikumar

et al. 2024

Universe

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“…Different aspects of black hole physics in non-commutative spacetime were analyzed in [37][38][39][40]. The correction to Bekenstein-Hawking entropy in noncommutative space-time was studied in [41]. Different features of non-commutative field theoretical models in FLRW space-time were investigated in [42,43].…”

Section: Introductionmentioning

confidence: 99%

Newtonian Cosmology and Evolution of κ-Deformed Universe

Harikumar,

Sreekumar,

Panja

2023

Universe

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Considering space-time to be non-commutative, we study the evolution of the universe employing the approach of Newtonian cosmology. Generalizing the conservation of energy and the first law of thermodynamics to κ-deformed space-time, we derive the modified Friedmann equations, valid up to the first order, in the deformation parameter. Analyzing these deformed equations, we derive the time evolution of the scale factor in cases of radiation-dominated, matter-dominated, and vacuum (energy)-dominated universes. We show that the rate of change of the scale factor in all three situations is modified by the non-commutativity of space-time, and this rate depends on the sign of the deformation parameter, indicating a possible explanation for the observed Hubble tension. We undertake this investigation for two different realizations of non-commutative space-time coordinates. In both cases, we also argue for the existence of bounce in the evolution of the universe.

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