Towards a noncommutative astrophysics

Bertolami, Orfeu; Zarro, C. A. D.

doi:10.1103/physrevd.81.025005

Cited by 69 publications

(142 citation statements)

References 45 publications

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“…Since pressure and density of matter are effected by the non-commutative factor Θ, so equation of state is also effected by this factor. Recently, Bertolami and Zarro 25) have pointed out this effect by studying the astrophysical objects in the context of non-commutativity. For non-commutative energy density, ρ Θ and pressure, p ⊥ , Eq.…”

Section: Non-commutative Correction To Thin Shell Collapsementioning

confidence: 99%

“…The left graph in Fig. 2 indicates the behavior of effective potential (25) for the perfect fluid shell depending on the EoS parameter and shell initial data. All these graphs show that V ef f 0, thus Eq.…”

Section: Thin Shell Collapsementioning

confidence: 99%

“…Bastos et al 23),24) explored the non-canonical phase space, singularity problem and black hole in the context of non-commutativity. Recently, Bartolami and Zarro 25) investigated the non-commutative correction to pressure, particle numbers and energy density for fermion gas and radiations. The non-commutative correction to these quantities lead to the fact that non-commutativity affects the matter dispersion relation and equation of state.…”

Section: )mentioning

confidence: 99%

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Non-Commutative Correction to Thin Shell Collapse in Reissner–Nordström Geometry

Sharif

Abbas

2012

J. Phys. Soc. Jpn.

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This paper investigates the polytropic matter shell collapse in the non-commutative Reissner-Nordström geometry. Using the Israel criteria, equation of motion for the polytropic matter shell is derived. In order to explore the physical aspects of this equation, the most general equation of state, p = kρ (1+ 1 n ) , has been used for finite and infinite values of n. The effective potentials corresponding to the equation of motion have been used to explain different states of the matter shell collapse. The numerical solution of the equation of motion predicts collapse as well as expansion depending on the choice of initial data. Further, in order to include the non-commutative correction, we modify the matter components and re-formulate the equation of motion as well as the corresponding effective potentials by including non-commutative factor and charge parameter. It is concluded that charge reduces the velocity of the expanding or collapsing matter shell but does not bring the shell to static position. While the noncommutative factor with generic matter favors the formation of black hole.

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Section: Non-commutative Correction To Thin Shell Collapsementioning

confidence: 99%

Section: Thin Shell Collapsementioning

confidence: 99%

Section: )mentioning

confidence: 99%

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Non-Commutative Correction to Thin Shell Collapse in Reissner–Nordström Geometry

Sharif

Abbas

2012

J. Phys. Soc. Jpn.

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“…Neutronization and the effects of general relativity would still occur at much lower momenta. Recently there has been work on the impact of MDRs on the structure of astrophysical objets [17].…”

Section: Discussionmentioning

confidence: 99%

On Modified Dispersion Relations and the Chandrasekhar Mass Limit

Gregg

Major

2009

Int. J. Mod. Phys. D

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Modified dispersion relations from effective field theory are shown to alter the Chandrasekhar mass limit. At exceptionally high densities, the modifications affect the pressure of a degenerate electron gas and can increase or decrease the mass limit, depending on the sign of the modifications. These changes to the mass limit are unlikely to be relevant for the astrophysics of white dwarf or neutron stars due to well-known dynamical instabilities that occur at lower densities.Generalizations to frameworks other than effective field theory are discussed.

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“…The first one has the space-time commutators described by [x i , t] = iλx i and [x i , x j ] = 0, whose astrophysics properties were studied in [108]. The second and the third model are described by the modified Heisenberg relation…”

Section: Introductionmentioning

confidence: 99%

Loop quantum cosmology with a non-commutative quantum deformed photon gas

Harkó

Liang

2018

Eur. Phys. J. C

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The non-commutativity of the space-time had important implications for the very early Universe, when its size was of the order of the Planck length. An important implication of this effect is the deformation of the standard dispersion relation of special relativity. Moreover, in the Planck regime gravity itself must be described by a quantum theory. We consider the implications of the modified dispersion relations for a photon gas, filling the early Universe, in the framework of loop quantum cosmology, a theoretical approach to quantum gravity. We consider three types of deformations of the dispersion relations of the photon gas, from which we obtain the Planck scale corrections to the energy density and pressure. The cosmological implications of the modified equations of state are explored in detail for all radiation models in the framework of the modified Friedmann equation of loop quantum cosmology. By numerically integrating the evolution equations we investigate the evolution of the basic cosmological parameters (scale factor, Hubble function, radiation temperature, and deceleration parameter) for a deformed photon gas filled Universe. In all models the evolution of the Universe shows the presence of a (nonsingular) bounce, corresponding to the transition from a contracting to an expanding phase.

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Towards a noncommutative astrophysics

Cited by 69 publications

References 45 publications

Non-Commutative Correction to Thin Shell Collapse in Reissner–Nordström Geometry

Non-Commutative Correction to Thin Shell Collapse in Reissner–Nordström Geometry

On Modified Dispersion Relations and the Chandrasekhar Mass Limit

Loop quantum cosmology with a non-commutative quantum deformed photon gas

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