Radial modes of oscillations of slowly rotating magnetized compact hybrid stars

Panda, R. N.; Mohanta, K K; Sahu, Kirti Chandra

doi:10.1088/1742-6596/599/1/012036

Cited by 18 publications

(12 citation statements)

References 21 publications

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“…In the present investigation, we have assumed the MIT bag EOS to describe anisotropic SQM, made of up, down and strange quark only [23]. Many researchers have successfully used the MIT bag EOS in their recent studies [60,61,62,63,64,65,66,67] for SQM. The MIT bag EOS is given as…”

Section: Basic Stellar Equationsmentioning

confidence: 99%

Anisotropic strange stars in Tolman–Kuchowicz spacetime

et al. 2018

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We attempt to study a singularity-free model for the spherically symmetric anisotropic strange stars under Einstein's general theory of relativity by exploiting the Tolman-Kuchowicz (Tolman in Phys Rev 55:364, 1939; Kuchowicz in Acta Phys Pol 33:541, 1968) metric. Further, we have assumed that the cosmological constant Λ is a scalar variable dependent on the spatial coordinate r . To describe the strange star candidates we have considered that they are made of strange quark matter distribution, which is assumed to be governed by the MIT bag equation of state. To obtain unknown constants of the stellar system we match the interior Tolman-Kuchowicz metric to the exterior modified Schwarzschild metric with the cosmological constant, at the surface of the system. Following Deb et al. (Ann Phys 387:239, 2017) we have predicted the exact values of the radii for different strange star candidates based on the observed values of the masses of the stellar objects and the chosen parametric values of the Λ as well as the bag constant B. The set of solutions satisfies all the physical requirements to represent strange stars. Interestingly, our study reveals that as the values of the Λ and B increase the anisotropic system become gradually smaller in size turning the whole system into a more compact ultra-dense stellar object.

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Section: Basic Stellar Equationsmentioning

confidence: 99%

Anisotropic strange stars in Tolman–Kuchowicz spacetime

et al. 2018

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“…It is observed that ignoring critical aspects of the quantum particle physics in the framework of GR several authors [91][92][93][94][95][96][97][98] successfully have been introduced this simplified form of the MIT Bag EOS to study stellar systems made of SQM.…”

Section: Basic Stellar Equations In F (R T ) Theory Of Gravitymentioning

confidence: 99%

Anisotropic strange stars under simplest minimal matter-geometry coupling in the f ( R,T ) gravity

et al. 2018

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We study strange stars in the framework of f (R, T ) theory of gravity. To provide exact solutions of the field equations it is considered that the gravitational Lagrangian can be expressed as the linear function of the Ricci scalar R and the trace of the stress-energy tensor T , i.e. f (R, T ) = R + 2χT , where χ is a constant. We also consider that the strange quark matter (SQM) distribution inside the stellar system is governed by the phenomenological MIT Bag model equation of state (EOS), given as pr = 1 3 (ρ − 4 B), where B is the Bag constant. Further, for a specific value of B and observed values of mass of the strange star candidates we obtain the exact solution of the modified Tolman-Oppenheimer-Volkoff (TOV) equation in the framework of f (R, T ) gravity and have studied in detail the dependence of the different physical parameters, like the metric potentials, energy density, radial and tangential pressures and anisotropy etc., due to the chosen different values of χ. Likewise in GR, as have been shown in our previous work [Deb et al., Ann. Phys. (Amsterdam) 387, 239 (2017)] in the present work also we find maximum anisotropy at the surface which seems an inherent property of the strange stars in modified f (R, T ) theory of gravity. To check the physical acceptability and stability of the stellar system based on the obtained solutions we have performed different physical tests, viz., the energy conditions, Herrera cracking concept, adiabatic index etc. In this work, we also have explained the effects, those are arising due to the interaction between the matter and the curvature terms in f (R, T ) gravity, on the anisotropic compact stellar system. It is interesting to note that as the values of χ increase the strange stars become more massive and their radius increase gradually so that eventually they gradually turn into less dense compact objects. The present study reveals that the modified f (R, T ) gravity is a suitable theory to explain massive stellar systems like recent magnetars, massive pulsars and super-Chandrasekhar stars, which can not be explained in the framework of GR. However, for χ = 0 the standard results of Einsteinian gravity are retrieved.

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“…In the recent times applying this simplified form of the MIT bag EOS several authors successfully studied strange star model [21,23,41,49,52,53,26,54,51,50,27,55,28,45,56]. Following Rahaman et al [57] we consider the value of the bag constant as B = 83 M eV /f m 3 .…”

Section: The Mit Bag Equation Of State and The Electric Charge Distri...mentioning

confidence: 99%

Anisotropic strange stars in the Einstein–Maxwell spacetime

et al. 2018

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We present here a detailed analysis on the effects of charge on the anisotropic strange star candidates by considering a spherically symmetric interior spacetime metric. To obtain exact solution of the Einstein-Maxwell field equations we have considered the anisotropic strange quark matter (SQM) distribution governed by the simplified MIT bag equation of state (EOS), p = 1 3 (ρ − 4 B), where B is the bag constant and the distribution of the electrical charge is given as q(r) = Q (r/R) 3 = αr 3 , where α is a cona

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Radial modes of oscillations of slowly rotating magnetized compact hybrid stars

Cited by 18 publications

References 21 publications

Anisotropic strange stars in Tolman–Kuchowicz spacetime

Anisotropic strange stars in Tolman–Kuchowicz spacetime

Anisotropic strange stars under simplest minimal matter-geometry coupling in the f ( R,T ) gravity

Anisotropic strange stars in the Einstein–Maxwell spacetime

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