Revisiting Vaidya–Tikekar stellar model in the linear regime

Sharma, Ranjan; Das, Shyam; Govender, M.; Pandya, D. M.

doi:10.1016/j.aop.2020.168079

Cited by 20 publications

(15 citation statements)

References 57 publications

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“…The above expression of the action in f (R, T ) theory of gravity in the presence of charge is modified as [31] S 4 x, (…”

Section: Basic Field Equations In F (R T ) Gravity With Chargementioning

confidence: 99%

“…: V,-vol 123 p r (ρ) reduces the problem of finding an exact model of the Einstein field equations using a single generating function. The imposition of an EoS has richly rewarded researchers with a handle on understanding complicated microphysics on a macroscale [3][4][5][6]. The color-flavor locked (CFL) EoS describing strange quark matter was shown to mimic the linear EoS.…”

Section: Introductionmentioning

confidence: 99%

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Charged compact star in f(R, T) gravity in Tolman–Kuchowicz spacetime

Rej¹,

Bhar²,

Govender

2021

Eur. Phys. J. C

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In this current study, our main focus is on modeling the specific charged compact star SAX J 1808.4-3658 (M = 0.88 $$M_{\odot }$$ M ⊙ , R = 8.9 km) within the framework of $$f(R,\,T)$$ f ( R , T ) modified gravity theory using the metric potentials proposed by Tolman–Kuchowicz (Tolman in Phys Rev 55:364, 1939; Kuchowicz in Acta Phys Pol 33:541, 1968) and the interior spacetime is matched to the exterior Reissner–Nordström line element at the surface of the star. Tolman–Kuchowicz metric potentials provide a singularity-free solution which satisfies the stability criteria. Here we have used the simplified phenomenological MIT bag model equation of state (EoS) to solve the Einstein–Maxwell field equations where the density profile ($$\rho $$ ρ ) is related to the radial pressure ($$p_{\mathrm{r}}$$ p r ) as $$p_{\mathrm{r}}(r) = (\rho - 4B_{\mathrm{g}})/3$$ p r ( r ) = ( ρ - 4 B g ) / 3 . Furthermore, to derive the values of the unknown constants $$a,\, b,\, B,\, C$$ a , b , B , C and the bag constant $$B_{\mathrm{g}}$$ B g , we match our interior spacetime to the exterior Reissner–Nordström line element at the surface of stellar system. In addition, to check the physical validity and stability of our suggested model we evaluate some important properties, such as effective energy density, effective pressures, radial and transverse sound velocities, relativistic adiabatic index, all energy conditions, compactness factor and surface redshift. It is depicted from our current study that all our derived results lie within the physically accepted regime which shows the viability of our present model in the context of $$f(R,\,T)$$ f ( R , T ) modified gravity.

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“…The above expression of the action in f (R, T ) theory of gravity in the presence of charge is modified as [31] S 4 x, (…”

Section: Basic Field Equations In F (R T ) Gravity With Chargementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Charged compact star in f(R, T) gravity in Tolman–Kuchowicz spacetime

Rej¹,

Bhar²,

Govender

2021

Eur. Phys. J. C

Self Cite

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“…In the literature y is given and a 1 is found from Eq (32) [30], [31], [32], [33], [34], [35], [36], [37], [38], [39]. Due to Eqs (6, 7) one finds quickly y form µ or m. Solutions with LEOS and known µ are given in [40], [41], [42] and [43].…”

Section: It Turns Into a Linear Equation Formentioning

confidence: 99%

Linear and Riccati equations in generating functions for stellar models in general relativity

Иванов

2020

Eur. Phys. J. Plus

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It is shown that the expressions for the tangential pressure, the anisotropy factor and the radial pressure in the Einstein equations may serve as generating functions for stellar models. The latter can incorporate an equation of state when the expression for the energy density is also used. Other generating functions are based on the condition for the existence of conformal motion (conformal flatness in particular) and the Karmarkar condition for embedding class one metrics. In all these cases the equations are linear first order differential equations for one of the metric components and Riccati equations for the other. The latter may be always transformed into second order homogenous linear differential equations. These conclusions are illustrated by numerous particular examples from the study of stellar models.

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“…Imposing a barotropic EoS of the form p r = p r (ρ) reduces the problem of finding an exact model of the Einstein field equations to a single generating function. The imposition of an EoS has richly rewarded researchers with a handle on understanding complicated microphysics on a macroscale [3][4][5][6]. The colour-flavour locked (CFL) EoS describing strange quark matter was shown to mimic the linear EoS.…”

Section: Introductionmentioning

confidence: 99%

Charged compact star in $f(R,T)$ gravity in Tolman-Kuchowicz spacetime

Rej,

Bhar,

Govender

2021

Preprint

Self Cite

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In this current study, our main focus is to model a specific charged compact star SAX J 1808.4-3658 (M = 0.88 M⊙, R = 8.9 km) within the realm of f (R, T ) modified gravity theory using the metric potentials proposed by Tolman-Kuchowicz (Tolman, Phys Rev 55:364, 1939; Kuchowicz Acta Phys Pol 33:541, 1968) and the interior spacetime is matched to the exterior Reissner-Nordström line element at the surface of the star. Tolman-Kuchowicz metric potentials provide a singularity-free solution which satisfies the stability criteria. Here we have used the simplified phenomenological MIT bag model equation of state (EoS) to solve Einstein-Maxwell field equations where the density profile (ρ) is related to the radial pressure (pr) as pr(r) = (ρ − 4Bg)/3. Further, to derive the values of unknown constants a, b, B, C and the bag constant Bg, we match our interior space-time to the exterior Reissner-Nordström line element at the surface of stellar system. In addition to this, to check the physical validity and stability of our suggested model, we evaluate some important properties such as effective energy density, effective pressures, radial and transverse sound velocities, relativistic adiabatic index, all energy conditions, compactness factor and surface redshift. It is depicted from our current study that all our derived results lie within the physically accepted regime which provides the viability of our present model in the context of f (R, T ) modified gravity.

show abstract

Revisiting Vaidya–Tikekar stellar model in the linear regime

Cited by 20 publications

References 57 publications

Charged compact star in f(R, T) gravity in Tolman–Kuchowicz spacetime

Charged compact star in f(R, T) gravity in Tolman–Kuchowicz spacetime

Linear and Riccati equations in generating functions for stellar models in general relativity

Charged compact star in $f(R,T)$ gravity in Tolman-Kuchowicz spacetime

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