Anisotropic compact stars: Constraining model parameters to account for physical features of tidal Love numbers

Das, Shyam; Ray, Saibal; Khlopov, Maxim Yu.; Nandi, K. K.; Parida, Bikram Keshari

doi:10.1016/j.aop.2021.168597

Cited by 24 publications

(12 citation statements)

References 54 publications

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“…Nonetheless, there are solid arguments that the impact of anisotropy (unequal radial and tangential pressures) cannot be overlooked when dealing with nuclear matter at extremely high densities and pressures(see, e.g., Herrera & Santos 1997;Isayev 2017;Ivanov 2017;Maurya et al 2018;Biswas & Bose 2019;Pretel 2020;Bordbar & Karami 2022 and the references therein). It has been demonstrated that the presence of anisotropy can cause significant changes in the main characteristics of compact stars (Maurya et al 2018;Biswas & Bose 2019;Pretel 2020;Horvat et al 2010;Rahmansyah et al 2020;Roupas & Nashed 2020;Das et al 2021aDas et al , 2021bDas et al , 2022Roupas 2021). It is also worth mentioning that non-rotating anisotropic compact stars have recently been studied within the framework of extended theories of gravity (Shamir et al 2017;Folomeev 2018;Mustafa et al 2020;Nashed & Capozziello 2021;Deb et al 2019b;Maurya et al 2019;Biswas et al 2020;Biswas et al 2021b;Maurya & Tello-Ortiz 2020;Rej et al 2021;Vernieri 2019;Pretel 2022;Mota et al 2022;Ashraf et al 2020;Tangphati et al 2021b;Tangphati et al 2021a;Nashed 2021;Solanki & Said 2022;Pretel & Duarte 2022).…”

Section: Introductionmentioning

confidence: 99%

The Effect of f(R, T) Modified Gravity on the Mass and Radius of Pulsar HerX1

Nashed

2023

ApJ

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Millisecond pulsars are the perfect testable to examine potential matter-geometry coupling and its physical consequences in the context of the recent Neutron Star Interior Composition Explorer discoveries. We apply the field equations of modified gravity, f(R, T) = R + α T, to a spherically symmetric spacetime, where R is the Ricci scalar, α is a dimensional parameter, and T is the matter of the geometry. Five unknown functions are present in the output system of differential equations, which consists of three equations. To close the system, we make explicit assumptions about the anisotropy and the radial metric potential, g rr . We then solve the output differential equations and derive the explicit forms of the components of the energy-momentum tensor, i.e., density, radial, and tangential pressures. We look into the possibility that all of the physical parameters in the star can be reexpressed in terms of α and the compactness parameters, C = 2 GM Rc−2. We show that, for a given mass, the size permitted by Einstein’s general relativity is less due to the matter-geometry coupling in f(R, T). The validity of the hypothesis was validated by observations from an extra 21 pulsars. To achieve a surface density that is compatible with a neutron core at nuclear saturation density, the mass–radius curve enables masses up to 3.35M ⊙. We emphasize that although there is no assumption of an equation of state, the model fits well with a linear behavior. When comparing the surface densities of these 20 pulsars, we divided them into three groups. We show that these three groups are compatible with neutron cores.

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Section: Introductionmentioning

confidence: 99%

The Effect of f(R, T) Modified Gravity on the Mass and Radius of Pulsar HerX1

Nashed

2023

ApJ

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“…[9][10][11][12][13][14][15] The impact of anisotropies in astrophysical and cosmological models have received widespread attention amongst researchers. [16][17][18][19][20][21][22][23][24][25][26][27][28][29][30][31][32][33] There exists a huge body of work on the effect of anisotropy on the evolution of temperature profiles during dissipative collapse by Govender and coworkers [34][35][36][37][38] and references therein. It has been shown that the presence of anisotropic pressures leads to higher temperatures at each interior point of the collapsing distribution with this effect being prominent in the central regions of the body.…”

Section: Introductionmentioning

confidence: 99%

Complexity‐Free Anisotropic Solution of Buchdahl's Model and Energy Exchange Between Relativistic Fluids by Extended Gravitational Decoupling

Maurya

Singh

Govender

et al. 2023

Fortschritte der Physik

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In this work, we present an anisotropic generalization of the Buchdahl static stellar model by implementing the method of extended gravitational decoupling and further requirement of vanishing complexity (Herrera, Phys Rev D 97:044010,2018). Starting off with a general spherically symmetric static metric with two unknown gravitational potentials, we impose the condition of vanishing complexity which then reduces the problem to a single-generating metric function [Contreras and Stuchlik, Eur. Phys. J. C (2022) 82:706]. The Buchdahl ansatz is then employed to obtain the complete gravitational behavior of the isotropic seed solution. The method of extended gravitational decoupling is thereafter utilized to obtain an anisotropic counterpart of the Buchdahl perfect gravitating sphere. We subject our solution to rigorous physical tests to ensure that it serves as a viable candidate for compact objects such as neutron stars as well as pulsars. We show that the decoupling parameter plays a crucial role in determining the stability and regularity of several key physical features of the entire stellar model. A novel finding of our investigation is the energy exchange between the seed solution and the secondary source which we show is sensitive to the decoupling parameter. In addition, it has also been shown that the direction of energy flow depends on the radial distance of the shell from the center of the stellar configuration.

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“…[18][19][20][21][22][23][24] and references therein. In that regard, it has been shown that the presence of anisotropy can lead to significant changes in the main characteristics of compact stars [21][22][23][25][26][27][28][29][30][31]. Within the framework of extended theories of gravity, it is also important to mention that non-rotating anisotropic compact stars have been recently studied by some authors in Refs.…”

Section: Introductionmentioning

confidence: 99%

Moment of inertia of slowly rotating anisotropic neutron stars in $f(R,T)$ gravity

Pretel

2023

Preprint

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Anisotropic compact stars: Constraining model parameters to account for physical features of tidal Love numbers

Cited by 24 publications

References 54 publications

The Effect of f(R, T) Modified Gravity on the Mass and Radius of Pulsar HerX1

The Effect of f(R, T) Modified Gravity on the Mass and Radius of Pulsar HerX1

Complexity‐Free Anisotropic Solution of Buchdahl's Model and Energy Exchange Between Relativistic Fluids by Extended Gravitational Decoupling

Moment of inertia of slowly rotating anisotropic neutron stars in $f(R,T)$ gravity

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