Superdense star in a spacetime with minimal length

Kiran, S. Bhanu; Harikumar, E.; Rajagopal, Vishnu

doi:10.1142/s0217732319501165

Cited by 4 publications

(4 citation statements)

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“…In our calculations, we use the mass of the sun (M ⊙ ) to be 1475 m (in natural units). The compactness of an object is defined as the ratio of its mass to radius [34,53,54]…”

Section: The Solution Of the Field Equationsmentioning

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%

“…Using κ-deformed degenerate pressure, compact stars have been studied [33]. In [34], the core-envelope model describing superdense stars is constructed using Einstein's field equation in κ-deformed space-time. From the κ-deformed strong energy condition, a bound on the deformation parameter has been obtained.…”

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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“…In our calculations, we use the mass of the sun (M ⊙ ) to be 1475 m (in natural units). The compactness of an object is defined as the ratio of its mass to radius [34,53,54]…”

Section: The Solution Of the Field Equationsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Neutron Star in Quantized Space-Time

Parai,

Harikumar

et al. 2024

Universe

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“…Field theory models on such space-times have been constructed and studied with various motivations [9,10,12]. Various models on different non-commutative space-times have been studied extensively to analyze the effect of the fundamental length scale and its possible signals [23][24][25][26][27][28][29][30][31]. Thus, it is of intrinsic interest to study the implications of a minimal length (introduced through the spacetime non-commutativity) in physical phenomena.…”

Section: Introductionmentioning

confidence: 99%

How does Casimir energy fall in $$\kappa $$-deformed space-time?

Harikumar,

Shajesh,

Panja

2024

Eur. Phys. J. C

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We investigate the response of Casimir energies to fluctuations in a scalar field in the background of a weak gravitational field in $$\kappa $$ κ -deformed space-time. We model the Casimir plates in a gravitational field by $$\kappa $$ κ -deformed Rindler coordinates and calculate the Casimir energy using the $$\kappa $$ κ -deformed scalar field. We show that the Casimir energy accelerates in a weak gravitational field like a mass. Thus, our calculations show that the mass–energy equivalence principle holds in $$\kappa $$ κ -deformed space-time even though a length scale is introduced through space-time non-commutativity.

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