New parameterizations of generalized Chaplygin gas model constrained at background and perturbation levels

Salahedin, S. F.; Malekjani, M.; Roobiat, K. Y.; Pazhouhesh, R.

doi:10.1007/s12036-022-09797-9

Cited by 1 publication

(1 citation statement)

References 29 publications

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“…In fact, it was argued that such gas could provide a solution to unify the effects of dark matter in the early times and dark energy in late times [4,11]. Although the literature provides a more generalized version for such EoS in the context of the Friedmann-Lemaître-Robertson-Walker Universe [5][6][7][73][74][75][76][77], here we will use the simplest form plus a linear term corresponding to a barotropic fluid, namely…”

Section: Equation Of State and Anisotropy Modelmentioning

confidence: 99%

Radial pulsations, moment of inertia and tidal deformability of dark energy stars

Pretel

2023

Eur. Phys. J. C

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We construct dark energy stars with Chaplygin-type equation of state (EoS) in the presence of anisotropic pressure within the framework of Einstein gravity. From the classification established by Iyer et al. (Class Quantum Grav 2:219, 1985), we discuss the possible existence of isotropic dark energy stars as compact objects. However, there is the possibility of constructing ultra-compact stars for sufficiently large anisotropies. We investigate the stellar stability against radial oscillations, and we also determine the moment of inertia and tidal deformability of these stars. We find that the usual static criterion for radial stability $$dM/d\rho _c >0$$ d M / d ρ c > 0 still holds for dark energy stars since the squared frequency of the fundamental pulsation mode vanishes at the critical central density corresponding to the maximum-mass configuration. The dependence of the tidal Love number on the anisotropy parameter $$\alpha $$ α is also examined. We show that the surface gravitational redshift, moment of inertia and dimensionless tidal deformability undergo significant changes due to anisotropic pressure, primarily in the high-mass region. Furthermore, in light of the detection of gravitational waves GW190814, we explore the possibility of describing the secondary component of such event as a stable dark energy star in the presence of anisotropy.

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Section: Equation Of State and Anisotropy Modelmentioning

confidence: 99%

Radial pulsations, moment of inertia and tidal deformability of dark energy stars

Pretel

2023

Eur. Phys. J. C

View full text Add to dashboard Cite

show abstract

New parameterizations of generalized Chaplygin gas model constrained at background and perturbation levels

Cited by 1 publication

References 29 publications

Radial pulsations, moment of inertia and tidal deformability of dark energy stars

Radial pulsations, moment of inertia and tidal deformability of dark energy stars

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