芬斯勒引力中超越广义相对论极限的大质量致密星：对GW190814次级天体的一种可能解释
Massive Compact Stars Beyond the General Relativity Limit in Finslerian Gravity: A Possible Explanation for the GW190814 Secondary
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中文总结 AI 辅助
研究在芬斯勒引力框架下，利用海因茨曼IIa引力势探讨致密星结构和性质，通过构建各向异性恒星模型，分析质量半径、转动惯量等关系，发现可提高致密星最大质量至2.67 $M_{\odot}$，为GW190814次级天体等提供合理解释。
中文摘要 AI 辅助
致密星存在质量上限是广义相对论的基本预测之一，对致密双星合并结果及中子星黑洞质量间隙性质有重要意义。LIGO-Virgo合作组发现GW190814致密双星合并事件，其中致密星质量为2.5至2.67 $M_\odot$，引发关于中子星最大质量与黑洞最小质量间是否存在间隙的讨论。该引力波探测挑战传统恒星模型，促使探索修正引力理论能否容纳此类超大质量致密天体。本文在芬斯勒引力框架下，利用海因茨曼IIa引力势研究致密星结构和物理性质，结果表明模型可大幅提高致密星最大质量至2.67 $M_{\odot}$，为GW190814次级天体等大质量致密天体提供合理解释。此外，转动惯量增加，意味着更强的转动支撑和内部质量分布重新调整。分析聚焦关键天体物理可观测量，包括质量半径和转动惯量质量关系，并与广义相对论对应情况详细比较。假设线性状态方程，构建一类物理上可行的各向异性恒星模型并分析其在芬斯勒修正影响下的行为，通过稳定性标准严格测试模型的物理可行性。
英文摘要
The existence of an upper mass limit for compact stars is one of the fundamental predictions of general relativity (GR), with important implications for the outcome of compact binary mergers and the nature of the proposed neutron star black hole mass gap. The LIGO Virgo collaboration announced the discovery of a compact binary merger, GW190814, containing a compact star with mass 2.5 to 2.67 $M_\odot$ [R. Abbott et al.(2020) ApJ Lett., 896, L44], which provided an exciting new stimulus to the ongoing debate on whether a gap exists between the maximum mass of NS and the minimum mass of black hole. Such GW detection has also challenged conventional stellar models and renewed interest in exploring whether modified theories of gravity can accommodate such ultra-massive compact objects without invoking black hole formation. The present work investigated the structure and physical properties of compact stars within the framework of Finslerian gravity, employing the Heintzmann IIa gravitational potentials and showed that the our model can substantially enhance the maximum mass of compact stars upto $2.67 M_{\odot}$, thereby offering a plausible explanation for massive compact objects such as the secondary component of GW190814. In addition, the moment of inertia is found to increase, indicating stronger rotational support and a redistribution of the internal mass profile. The analysis focuses on key astrophysical observables, including the mass radius and moment of inertia mass relations, and a detailed comparison with the GR counterpart is performed. Assuming a linear equation of state, we construct a class of physically viable anisotropic stellar models and analyze their behavior under the influence of Finslerian corrections. The physical viability of the model is rigorously tested through stability criteria.
