Astrophysical Signatures of Charged Anisotropic Compact Star in f(R,T) Gravity via Minimal Geometric Deformation
Abstract
This work employs minimal geometric deformation to develop two new anisotropic solutions under the effects of an electromagnetic field in the context of f(R,T) theory. Our investigation begins with a static spherical system with an anisotropic fluid as a seed source. After that, a new source is inserted to the existing fluid distribution and both the fluid distributions are assumed to be gravitationally coupled with each other. After computing the Einstein-Maxwell field equations, a radial transformation is applied which results in two different sets of equations. These systems are solved individually under different constraints, generating new solutions. To obtain the constants in our interior solutions, we match the internal geometry with the external Reissner-Nordström spacetime at the surface. We further validate our models by using the known mass and radius of a star LMC X-4. Our investigation confirms that both relativistic stellar models satisfy all the physical requirements for the specified decoupling parametric values.
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BibTeX
@misc{shadab2026astrophysical,
title = {{Astrophysical Signatures of Charged Anisotropic Compact Star in f(R,T) Gravity via Minimal Geometric Deformation}},
author = {Hira Shadab and M. Sharif and Tayyab Naseer},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.23993},
eprint = {2610.23993},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.23993},
}
RIS
TY - UNPB
TI - Astrophysical Signatures of Charged Anisotropic Compact Star in f(R,T) Gravity via Minimal Geometric Deformation
AU - Hira Shadab
AU - M. Sharif
AU - Tayyab Naseer
PY - 2026
DA - 2026/10/15
PB - arXiv
DO - 10.48550/arxiv.2610.23993
UR - https://arxiv.org/abs/2610.23993
AB - This work employs minimal geometric deformation to develop two new anisotropic solutions under the effects of an electromagnetic field in the context of f(R,T) theory. Our investigation begins with a static spherical system with an anisotropic fluid as a seed source. After that, a new source is inserted to the existing fluid distribution and both the fluid distributions are assumed to be gravitationally coupled with each other. After computing the Einstein-Maxwell field equations, a radial transformation is applied which results in two different sets of equations. These systems are solved individually under different constraints, generating new solutions. To obtain the constants in our interior solutions, we match the internal geometry with the external Reissner-Nordström spacetime at the surface. We further validate our models by using the known mass and radius of a star LMC X-4. Our investigation confirms that both relativistic stellar models satisfy all the physical requirements for the specified decoupling parametric values.
ER -