Dark energy star in gravity's rainbow

Tudeshki, A. Bagheri; Bordbar, G. H.; Panah, B. Eslam

doi:10.1016/j.physletb.2022.137523

Cited by 14 publications

(5 citation statements)

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“…This modification of the relativistic dispersion relation finds motivation in the observation of highenergy cosmic rays [8], TeV photons emitted during gamma ray bursts [14,28,29], and neutrino data from IceCube [30]. The rainbow gravity effects have been studied in various physical aspects reported in [31][32][33][34][35][36][37][38][39][40][41].…”

Section: Introductionmentioning

confidence: 99%

Study of scalar particles through the Klein–Gordon equation under rainbow gravity effects in Bonnor–Melvin-Lambda space-time

Ahmed,

Bouzenada

2024

Commun. Theor. Phys.

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In our investigation, we explore the quantum dynamics of charge-free scalar particles through the Klein-Gordon equation within the framework of rainbow gravity's, considering the Bonnor-Melvin-Lambda (BML) space-time background. The BML solution is characterized by the magnetic field strength along the axis of symmetry direction which is related with the cosmological constant $\Lambda$ and the topological parameter $\alpha$ of the geometry. The behavior of charge-free scalar particles described by the Klein-Gordon equation is investigated, utilizing two sets of rainbow functions: (i) $f(\chi)=\frac{(e^{\beta\,\chi}-1)}{\beta\,\chi}$,\, $h(\chi)=1$ and (ii) $f(\chi)=1$,\, $h(\chi)=1+\frac{\beta\,\chi}{2}$. Here $0 < \Big(\chi=\frac{|E|}{E_p}\Big) \leq 1$ with $E$ represents the particle's energy, $E_p$ is the Planck's energy, and $\beta$ is the rainbow parameter. We obtain the approximate analytical solutions for the scalar particles and conduct a thorough analysis of the obtained results. Afterwards, we study the quantum dynamics of quantum oscillator fields within this BML space-time, employing the Klein-Gordon oscillator. Here also, we choose the same sets of rainbow functions and obtained approximate eigenvalue solution for the oscillator fields. Notably, we demonstrate that the relativistic approximate energy profiles of charge-free scalar particles and oscillator fields get influenced by the topology of the geometry and the cosmological constant. Furthermore, we show that the energy profiles of scalar particles get modifications by the rainbow parameter and the quantum oscillator fields by both the rainbow parameter and the frequency of oscillation.

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Section: Introductionmentioning

confidence: 99%

Study of scalar particles through the Klein–Gordon equation under rainbow gravity effects in Bonnor–Melvin-Lambda space-time

Ahmed,

Bouzenada

2024

Commun. Theor. Phys.

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“…For example, Malaver et al [25] showed that the physical properties of a DES are maintained in Einstein-Gauss-Bonnet gravity. Also, by assuming the dependence of metric potentials on energy, Tudeshki et al [26] demonstrated in addition to satisfying the characteristics of DES, the stability of a star near the surface depends on energy, and the results obtained in gravity's rainbow are improved compared to GR gravity. Secondly, the origin of late acceleration of the universe is not yet precisely known.…”

Section: Introductionmentioning

confidence: 99%

Effect of massive graviton on dark energy star structure

Tudeshki¹,

Bordbar²,

Panah³

2023

Preprint

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The presence of massive gravitons in the field of massive gravity is considered as an important factor in investigating the structure of compact objects. Hence, we are encouraged to study the dark energy star structure in the Vegh's massive gravity. We consider that the equation of state governing the inner spacetime of the star is the extended Chaplygin gas, and then using this equation of state, we numerically solve the Tolman-Oppenheimer-Volkoff (TOV) equation in massive gravity. In the following, assuming different values of free parameters defined in massive gravity, we calculate the properties of dark energy star such as radial pressure, transverse pressure, anisotropy parameter, and other characteristics. Then, after obtaining the maximum mass and its corresponding radius, we compute redshift and compactness. The obtained results show that for this model of dark energy star, the maximum mass and its corresponding radius depend on the massive gravity's free parameters and anisotropy parameter. These results are consistent with the observational data, and cover the lower mass gap. We also demonstrate that all energy conditions are satisfied for this model, and in the presence of anisotropy, the dark energy star is potentially unstable.

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“…Tudeshki et al. [ 48 ] studied the properties of dark energy stars in a modified theory of gravity called gravity's rainbow. To obtain the anisotropic dark energy star, the authors obtained a modified Tolman‐Openheimer‐Volkof (TOV) equation in gravity's rainbow.…”

Section: Introductionmentioning

confidence: 99%

“…By analyzing M − −R curves, the authors found that the coupling of dark energy increases the equilibrium radius to confine the active gravitational mass of the star. Tudeshki et al [48] studied the properties of dark energy stars in a modified theory of gravity called gravity's rainbow. To obtain the anisotropic dark energy star, the authors obtained a modified Tolman-Openheimer-Volkof (TOV) equation in gravity's rainbow.…”

Section: Introductionmentioning

confidence: 99%

Existence of Dark Energy Stars within Lower Mass Gap in the Realm of f(Q)$f(Q)$ Gravity

Bhar

2023

Fortschritte der Physik

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The object of this article is to study a new class of dark energy stars in the background of gravity by using the metric potentials proposed by Krori‐Barua [J. Phys. A, Math. Gen. 8:508 (1975)]. To achieve the goal, a quadratic form of as is taken into account for the static spherically symmetric spacetime,`a' being a coupling parameter of gravity. The maximum allowable masses with corresponding radii have been obtained via plots for and 8. The obtained maximum masses from our analysis are found in the range . For a smaller value of the coupling parameter ‘a’ associated with gravity, more massive stars are found. The radii corresponding to the maximum masses also increase with decreasing ‘a’. In particular, when , the theory can achieve a dark energy star of mass for certain specific combinations of model parameters. This obtained mass is located within a mass in the range of and that can be a lighter object in the GW190814 event detected by LIGO/VIRGO experiments.

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Dark energy star in gravity's rainbow

Cited by 14 publications

References 50 publications

Study of scalar particles through the Klein–Gordon equation under rainbow gravity effects in Bonnor–Melvin-Lambda space-time

Study of scalar particles through the Klein–Gordon equation under rainbow gravity effects in Bonnor–Melvin-Lambda space-time

Effect of massive graviton on dark energy star structure

Existence of Dark Energy Stars within Lower Mass Gap in the Realm of f(Q)$f(Q)$ Gravity

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