Charged Anisotropic Compact Stars in f(R,ϕ,X) Gravity: A Class I Embedding Approach with Reissner-Nordström Exterior
Abstract
This work examines the physical characteristics of charged, anisotropic compact spheres within the framework of f(R,ϕ,X) modified gravity. Starting from a static, spherically symmetric spacetime, we employ an Adler-type ansatz for the temporal metric component gtt. The corresponding radial metric component grr is then systematically derived through application of the Karmarkar condition, which ensures a class-one embedding for the interior geometry. A crucial aspect of our approach involves matching the interior solution at the stellar boundary to the exterior Reissner--Nordstr0̈m spacetime---the established vacuum solution for charged, non-rotating masses. This matching procedure is essential for determining integration constants and verifying global physical consistency. Our comprehensive analysis of the resulting stellar model investigates multiple physical aspects, including energy density, radial and tangential pressures, anisotropy, equation-of-state parameters, energy conditions, mass function, compactness, and surface redshift. Stability assessment further incorporates examination of the adiabatic index and the Tolman--Oppenheimer--Volkoff equation. Collectively, our findings demonstrate that the charged compact star model presented here constitutes a physically viable configuration---free of singularities and maintaining stable equilibrium across the considered parameter space.
Related
- Astrophysical signatures of charged anisotropic compact star in f(R, T) gravity via minimal geometric deformation
- Testing Charged Black Holes Embedded in Anisotropic Matter and Surrounded by Plasma through Gravitational Lensing: Bounds from the Sloan Lens ACS Survey
- Magnetohydrodynamics of charged interstellar dust. Multifluid models and study of the linear modes
- Perturbations of Charged Black Holes with Higher-Order Interactions
- Buchdahl type anisotropic stellar configurations in Rastall gravity
BibTeX
@misc{malik2026charged,
title = {{Charged Anisotropic Compact Stars in $f(R,ϕ,X)$ Gravity: A Class I Embedding Approach with Reissner-Nordström Exterior}},
author = {Adnan Malik and Fatemah Mofarreh and Ayesha Almas and Wedad Albalawi and Aishah Alshehri},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.01630},
eprint = {2609.01630},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.01630},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Charged Anisotropic Compact Stars in f(R,ϕ,X) Gravity: A Class I Embedding Approach with Reissner-Nordström Exterior
AU - Adnan Malik
AU - Fatemah Mofarreh
AU - Ayesha Almas
AU - Wedad Albalawi
AU - Aishah Alshehri
PY - 2026
DA - 2026/09/01
PB - arXiv
DO - 10.48550/arxiv.2609.01630
UR - https://arxiv.org/abs/2609.01630
AB - This work examines the physical characteristics of charged, anisotropic compact spheres within the framework of f(R,ϕ,X) modified gravity. Starting from a static, spherically symmetric spacetime, we employ an Adler-type ansatz for the temporal metric component g_tt. The corresponding radial metric component g_rr is then systematically derived through application of the Karmarkar condition, which ensures a class-one embedding for the interior geometry. A crucial aspect of our approach involves matching the interior solution at the stellar boundary to the exterior Reissner--Nordstr0̈m spacetime---the established vacuum solution for charged, non-rotating masses. This matching procedure is essential for determining integration constants and verifying global physical consistency. Our comprehensive analysis of the resulting stellar model investigates multiple physical aspects, including energy density, radial and tangential pressures, anisotropy, equation-of-state parameters, energy conditions, mass function, compactness, and surface redshift. Stability assessment further incorporates examination of the adiabatic index and the Tolman--Oppenheimer--Volkoff equation. Collectively, our findings demonstrate that the charged compact star model presented here constitutes a physically viable configuration---free of singularities and maintaining stable equilibrium across the considered parameter space.
ER -