arXiv 2512.024392025-12-02gr-qc

带电致密天体的结构和质量-半径稳定性研究：对称Teleparallel爱因斯坦-海森堡引力中的情况

Structure and Mass-Radius Stability of Charged Compact Objects in Symmetric Teleparallel Euler-Heisenberg Gravity

Allah Ditta, M. Yousaf, G. Mustafa, S. K. Maurya, Farruh Atamurotov, Orhan Donmez, Sardor Murodov

备注：: 19 pages, 7 figures

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AI总结：

本文研究了在f(Q)-爱因斯坦-海森堡引力框架下带电致密天体的结构和质量-半径稳定性，通过建立各向异性流体配置与非线性电磁源耦合的场方程解，验证了模型的物理可行性及稳定性。

摘要：

在本文中，我们开发了一个新的相对论模型，用于描述带电各向异性致密星体，在修改的对称Teleparallel引力框架下，即f(Q)-爱因斯坦-海森堡引力中。通过采用MIT袋模型方程状态，我们建立了度规势之间的关系，从而得到一个各向异性流体配置与非线性电磁源耦合的场方程的精确解。内部时空通过使用f(Q)-爱因斯坦-海森堡引力的理论设置，利用Darmois-Israel接合条件与外部几何进行平滑匹配，确保度规函数及其导数在恒星边界处的连续性。通过常规性、能量和因果性条件检验模型的物理可行性，所有条件在整个恒星内部均得到满足。研究强调了压力各向异性、声速传播速度以及Tolman-Oppenheimer-Volkoff平衡条件之间的相互关联，表明只有当引力、流体静力学、电和各向异性贡献适当抵消时，恒星才能保持机械平衡。此外，通过要求等熵指数Γ>4/3，进一步支持了配置的动力学稳定性，表明其对小径向扰动具有韧性。紧凑性、表面红移以及质量-半径曲线的图示证实了所有物理量在恒星内部行为正常且变化平滑。我们绘制了质量-半径曲线。

英文摘要：

In this work, we develop a new relativistic model for a charged anisotropic compact star in the framework of modified symmetric teleparallel gravity, namely $f(Q)$-Euler-Heisenberg gravity. By employing the MIT bag model equation of state, we establish a relation between the metric potentials, leading to an exact solution of the field equations for an anisotropic fluid configuration coupled with a non-linear electromagnetic source. The interior spacetime is smoothly matched with the exterior geometry calculated from the theoretical setup of $f(Q)$-Euler-Heisenberg gravity using the Darmois-Israel junction conditions, ensuring the continuity of the metric functions and their derivatives at the stellar boundary. The physical viability of the model is examined through regularity, energy, and causality conditions, all of which are satisfied throughout the stellar interior. The study highlights how the pressure anisotropy, the propagation speeds of sound, and the Tolman-Oppenheimer-Volkoff balance condition are interconnected, showing that the star remains in mechanical equilibrium only when the gravitational, hydrostatic, electric, and anisotropic contributions counterbalance one another appropriately. The dynamical stability of the configuration is further supported by the requirement $Γ> \tfrac{4}{3}$ for the adiabatic index, indicating resilience against small radial perturbations. The plots of compactness, surface redshift, and the mass--radius profiles confirm that all physical quantities behave regularly and vary smoothly throughout the stellar interior. We graphically plotted the mass-radius curves.

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