Charged compact stellar model in Finch-Skea spacetime

For a static, spherically symmetric, anisotropic and charged distribution of matter, we present a new class of exact solutions to the Einstein-Maxwell system. By assuming specific forms of the electric field and anisotropy, we transform the master equation of the Einstein-Maxwell system to Bessel and modified Bessel differential equations. The subsequent solutions turn out to be generalizations of the isotropic and uncharged stellar model of Finch and Skea (1989), the isotropic and charged stellar model of Hansraj and Maharaj (2006) and the anisotropic and charged stellar model of Maharaj et al (2017). We analyze the physical viability of the solutions and utilize one particular class of solutions to examine the effects of charge and anisotropy on the mass-radius relationship of compact stars.

“…(13). Our study reconfirms [25] earlier claims that electric field and/or anisotropy can serve as tuning parameters to fine-tune the mass-radius relationship of compact stars.…”

Section: Physical Viabilitysupporting

confidence: 89%

Effects of electric field and anisotropy on the mass-radius relationship of a particular class of compact stars

Komathiraj

Sharma

Chanda

2022

“…Consequently, for a given central and/or surface density, an external observer sees no change in its mass-radius relationship. In a separate study (Ratanpal et al (2017)) it has been observed that in the presence of an electric field a stellar configuration tends to accommodate more mass. However, it should be stressed that incorporation of an electromagnetic field changes the exterior spacetime from Schwarzschild to Reissner-Nordström whereas in our case the exterior spacetime remains unaltered.…”

Section: Physical Analysismentioning

confidence: 94%

“…The original Finch-Skea stellar model as well as the charged stellar model developed by Hansraj and Maharaj (2006) can be regained from the new class of solutions. For a specific charge distribution, Ratanpal et al (2017) obtained a new class of solutions in terms of Bessel functions for a matter distribution in the Finch-Skea background spacetime. The physically viable solution has been utilized to study the impact of charge on the mass-radius (M − R) relationship, in particular.…”

mentioning

confidence: 99%

Anisotropic extension of Finch and Skea stellar model

Sharma¹,

Das²,

Thirukkanesh³

2017

In this paper, the spacetime geometry of Finch and Skea [Class. Quantum Grav. 6 (1989) 467] has been utilized to obtain closed-form solutions for a spherically symmetric anisotropic matter distribution. By examining its physical admissibility, we have shown that the class of solutions can be used as viable models for observed pulsars. In particular, a specific class of solutions can be used as an 'anisotropic switch' to examine the impact of anisotropy on the gross physical properties of a stellar configuration. Accordingly, the mass-radius relationship has been analyzed.

“…By relaxing the pressure isotropy condition, Sharma et al (2017) generalized the Finch and Skea (1989) stellar model. For a specific charge distribution, Ratanpal et al (2017) also made a generalization of the Finch and Skea stellar model to analyze the impact of the charge on the mass-radius relationship of a compact star, in particular. The relativistic stellar model of Mak and Harko (2004) was extended by to include charge into the system.…”

Section: Introductionmentioning

confidence: 99%

Electromagnetic and anisotropic extension of a plethora of well-known solutions describing relativistic compact objects

Komathiraj

Sharma

2020

We demonstrate a technique to generate new class of exact solutions to the Einstein-Maxwell system describing a static spherically symmetric relativistic star with anisotropic matter distribution. An interesting feature of the new class of solutions is that one can easily switch off the electric and/or anisotropic effects in this formulation. Consequently, we show that a plethora of well known stellar solutions can be identified as sub-class of our class of solutions. We demonstrate that it is possible to express our class of solutions in a simple closed form so as to examine its physical viability for the studies of relativistic compact stars.