Properties of strange quark matter and strange quark stars

Kumari, Manisha; Kumar, Arvind

doi:10.1140/epjc/s10052-021-09576-w

Cited by 10 publications

(7 citation statements)

References 105 publications

(117 reference statements)

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“…Similar to the trends in strange quark stars, as reported in Ref. [70], the Love number of dark energy stars grows until it reaches a maximum value and then decreases as compactness increases. Note also that the maximum value of k 2 is sensitive to the value of α, indicating that the Love number decreases as the parameter α increases for both models.…”

Section: Tidal Propertiessupporting

confidence: 84%

“…To do so, we follow the procedure carried out by Hinderer et al [64] (see also Refs. [65][66][67][68][69][70] for additional results). The basic idea is as follows: In a binary system, the deformation of a compact star due to the tidal effect created by the companion star is characterized by the tidal deformability parameter λ = −Q i j /E i j , where Q i j is the induced quadrupole moment tensor and E i j is the tidal field tensor [68].…”

Section: Tidal Deformabilitymentioning

confidence: 99%

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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: Tidal Propertiessupporting

confidence: 84%

Section: Tidal Deformabilitymentioning

confidence: 99%

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

Pretel

2023

Eur. Phys. J. C

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“…In theoretical physics, interest in this theory of dilatons [5][6][7][8][9][10] has recently increased. In these works, the manifestations of the dilaton field in astrophysical and laboratory conditions are studied theoretically.…”

Section: Introductionmentioning

confidence: 99%

“…In these works, the manifestations of the dilaton field in astrophysical and laboratory conditions are studied theoretically. In particular, the influence of the dilaton scalar field on the properties of strange quark stars and quantum deformed Schwarzschild black holes was studied in [5,6].…”

Section: Introductionmentioning

confidence: 99%

The investigation of low-frequency dilaton generation

2022

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The electromagnetic source of dilaton radiation is a first invariant of the electromagnetic field tensor. For electromagnetic waves, this invariant can be nonzero only in the near zone. Pulsars and magnetars are natural sources of this type. We calculated the generation of dilatons by a coherent electromagnetic field of rotating magnetic dipole moments of pulsars and magnetars. It was shown that the radiation of dilaton waves occurs at two frequencies: the rotation frequency $$\omega $$ ω of the magnetic dipole moment of the neutron star, and twice that frequency. The generation of dilatons at frequency $$\omega $$ ω is maximal when the angle between the magnetic dipole moment and the axis of its rotation is $$\pi /4.$$ π / 4 . If this angle is $$ \pi /2,$$ π / 2 , then dilaton radiation at frequency $$\omega $$ ω does not occur. The generation of dilatons at frequency $$2\omega $$ 2 ω is maximal when the angle between the magnetic dipole and the axis of its rotation is $$\pi /2.$$ π / 2 . The angular distribution of radiation of dilatons having a frequency of $$\omega $$ ω is maximal along the conic surfaces $$\theta =\pi /4$$ θ = π / 4 and $$\theta =3\pi /4.$$ θ = 3 π / 4 . The angular distribution of radiation of dilatons having a frequency of $$2\omega $$ 2 ω is maximal in the plane perpendicular to the axis of rotation $$(\theta =\pi /2).$$ ( θ = π / 2 ) .

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“…In particular, the influence of the dilaton scalar field on the properties of strange quark stars and quantum a e-mail: vid.msu@yandex.ru b e-mail: denisovaip@mati.ru c e-mail: pm@mati.ru deformed Schwarzschild black holes was studied in [3,4].…”

Section: Introductionmentioning

confidence: 99%

The investigation of low frequency dilaton generation

Denisov,

Denisova,

Einiev

2021

Preprint

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The electromagnetic source of dilaton is a first invariant of the electromagnetic field tensor. For electromagnetic waves, this invariant can be non zero only in the near zone. Pulsars and magnetars are natural sources of this type. We calculated the generation of dilatons by coherent electromagnetic field of rotating magnetic dipole moment of pulsars and magnetars. It is shown that the radiation of dilaton waves occurs at the two frequencies: the rotation frequency ω of the magnetic dipole moment of the neutron star and the twice frequency.The generation of dilaton at frequency ω is maximal in the case when the angle between the magnetic dipole moment and the axis of its rotation is π/4. If this angle is π/2, then dilaton radiation at frequency ω does not occur. The generation of dilaton at frequency 2ω is maximal in the case when the angle between the magnetic dipole and the axis of its rotation is π/2.Angular distribution of radiation of dilatons having a frequency of ω, has a maximum along conic surfaces θ = π/4. Angular distribution of radiation of dilatons having a frequency of 2ω, has a maximum in the plane which is perpendicular to the axis of rotation (θ = π/2).

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Properties of strange quark matter and strange quark stars

Cited by 10 publications

References 105 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

The investigation of low-frequency dilaton generation

The investigation of low frequency dilaton generation

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