Maxwell wave packets in de Sitter expanding universe

Cotăescu, Ion I.

doi:10.1140/epjc/s10052-021-09462-5

Cited by 7 publications

(9 citation statements)

References 69 publications

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“…Thus we revisited the redshift in the particular case when O ′ does not have a peculiar velocity. The general result for arbitrary peculiar velocity of O ′ was derived recently [8,9]. These results that hold at the level of the geometric optics in de Sitter background are incomplete since at this level we neglect the wave behaviour and polarization that may be studied considering the classical and quantum theory of the Maxwell field.…”

Section: Null Geodesics and Redshiftmentioning

confidence: 99%

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Quantum theory of redshift in de Sitter expanding universe

Cotaescu

2021

Preprint

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The quantum theory of the Maxwell free field in Coulomb gauge on the de Sitter expanding universe is completed with the technical elements needed for building a coherent quantum theory of redshift. Paying a special attention to the conserved observables and defining the projection operator selecting the detected momenta it is shown that the expectation values of the energies of the emitted and detected photons comply with the Lemaître rule of Hubble's law. Moreover, the quantum corrections to the dispersions of the principal observables and new uncertainty relations are derived.Pacs: 04.62.+v

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Section: Null Geodesics and Redshiftmentioning

confidence: 99%

“…We obtained thus a rdshift formula having a new term combining the cosmological and kinetic contributions in a non-trivial manner [8]. Moreover, we related the black hole shadow and redshift for the Schwarzschild [9] and Reissner-Nordstrom [10] black holes moving freely in the de Sitter expanding universe.…”

Section: Introductionmentioning

confidence: 99%

Quantum theory of redshift in de Sitter expanding universe

Cotaescu

2021

Preprint

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“…2, it is easy to see how we may combine the EUP metric function to the dark matter mass. Thus, the static and spherically symmetric spacetime metric (10) can have the metric function f (r) as…”

Section: Metric Of Eup Black Hole Surrounded By Dark Mattermentioning

confidence: 99%

“…Several researchers theorized various black hole models to study its shadow, such as Schwarzschild black holes [4], Kerr black holes [5,6], Kerr-like black holes [7], Kaluza Klein black holes [8], naked singularities [9], Reissner-Nordstrom-de Sitter black holes [10], Weyl black holes [11], and much more. Interest in black hole research has increased more than ever when Event Horizon Telescope (EHT) captured the first image of the shadow of the supermassive black hole (SMBH) at the center of the M87 galaxy last April 10, 2019 [12].…”

Section: Introductionmentioning

confidence: 99%

Shadow and weak deflection angle of extended uncertainty principle black hole surrounded with dark matter

Pantig,

Yu,

Rodulfo

et al. 2021

Preprint

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In this paper, we discussed the possible effects of dark matter on a Schwarzschild black hole with EUP correction such as the parameter α and the large fundamental length scale L * . In particular, we surrounded the EUP black hole of mass m with a static spherical shell of dark matter described the parameters mass M , inner radius rs, and thickness ∆rs. Considering only the case where the EUP event horizon coincides rs, the study finds that there is no deviation in the event horizon, which readily implies that the black hole temperature due to the Hawking radiation is independent any dark matter concentration. In addition, we explored the deviations in the ISCO radius of time-like particles, photonsphere, shadow radius, and weak deflection angle. While the ISCO radius increases with decreasing value of L * , dark matter further enhances the increase in the ISCO radius. The ISCO radius is also sensitive to deviation even at very low dark matter concentration. The photonsphere is found to decrease in radius, while the reverse behavior happens to the shadow radius. Using the analytic expression for the shadow radius and the approximation ∆rs >> rs, it is revealed that L * should not be any lower than 2m. To broaden the scope of this study, we also calculated the analytic expression for the weak deflection angle using the Ishihara et al. method [1] to improve the dark matter estimate found via shadow radius. As a result, the estimate improved by a factor of (1 + 4αm 2 /L 2 * ) due to the EUP correction parameters. The estimates for the shadow radius and weak deflection angle are compared using the estimated values of galactic mass, and the mass of the SMBH at the center of Sgr A* and M87 galaxies. The study found out that the analytical estimates are not satisfied in these galaxies, which indicates that the notable deviation due to dark matter is only evident and considerable if the dark matter distribution is near the supermassive black hole.

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“…( 44) and (46) for x 0 = d(t 0 ), verifying that P • Q = p(t f ) 2 for closing again the identity (40). Note that the relation among the conserved quantities E, P, ... and E ′ , P ′ , ... can be derived directly according to the transformation rule under isometries we have discussed recently [19,20].…”

Section: Time-like Geodesicsmentioning

confidence: 99%

Kinematics in spatially flat FLRW space-time

Cotaescu

2021

Preprint

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The kinematics on spatially flat FLRW space-times is presented for the first time in co-moving local charts with physical coordinates, i. e. the cosmic time and Painlevé-type Cartesian space coordinates. It is shown that there exists a conserved momentum which determines the form of the covariant four-momentum on geodesics in terms of physical coordinates. Moreover, with the help of the conserved momentum one identifies the peculiar momentum separating the peculiar and recessional motions without ambiguities. It is shown that the energy and peculiar momentum satisfy the mass-shell condition of special relativity while the recessional momentum does not produce energy. In this framework, the measurements of the kinetic quantities along geodesic performed by different observers are analysed pointing out an energy loss of the massive particles similar to that giving the photon redshift. The examples of the kinematics on the de Sitter expanding universe and a new Milne-type space-time are extensively analysed.Pacs: 04.62.+v

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Maxwell wave packets in de Sitter expanding universe

Cited by 7 publications

References 69 publications

Quantum theory of redshift in de Sitter expanding universe

Quantum theory of redshift in de Sitter expanding universe

Shadow and weak deflection angle of extended uncertainty principle black hole surrounded with dark matter

Kinematics in spatially flat FLRW space-time

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