发表机构
Universidade Federal da Paraíba; Universidade Federal de Campina Grande; Khazar University; Damghan University; Instituto de Astrofísica e Ciências do Espaço, Faculdade de Ciências da Universidade de Lisboa; Departamento de Física, Faculdade de Ciências da Universidade de Lisboa（帕拉伊巴联邦大学; 坎皮纳格兰德联邦大学; 哈扎尔大学; 达姆甘大学; 里斯本大学理学院空间科学与天体物理研究所; 里斯本大学理学院物理学系）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
本文在无迹度规-仿射大黄蜂引力中构造了一般静态球对称黑洞解，研究了其热力学、扰动及太阳系约束，发现洛伦兹破缺改变霍金温度和潮汐场，且无临界点，光偏折给出严格约束。
AI 中文摘要
我们通过考虑具有时间分量和径向分量的真空期望值，在无迹度规-仿射大黄蜂引力中构造并分析了一个一般精确静态球对称黑洞解。时间分量保持恒定，辅助几何是Ricci平坦的，而洛伦兹对称性破缺通过度规-仿射形变传递到物理度规。在引入面积半径并将Killing时间在空间无穷远处归一化后，几何由单一的不变形变参数控制。由此产生的时空是渐近锥形的，具有正则Killing视界，并保留了史瓦西黑洞的因果结构，曲率奇点位于原点。首先，我们研究了其热力学性质、引力多普勒效应和潮汐力。洛伦兹对称性破缺改变了霍金温度和潮汐场的强度，尽管径向拉伸与横向压缩之间的特征比率得以保持。热力学-拓扑分析显示，在允许的黑洞扇区内没有临界点。此外，我们还通过WKB和特征时域解研究了无质量标量扰动，显示在所采样的参数范围内具有衰减轮廓和依赖形变的准正则频率。最后，光偏折和近日点进动被用来建立对不变形变的严格太阳系约束，在领头阶，该约束依赖于大黄蜂场的时间扇区和范数扇区的组合。
英文摘要
We construct and analyze a general exact static and spherically symmetric black hole solution in traceless metric-affine bumblebee gravity by considering a vacuum expectation value with temporal and radial components. The temporal component remains constant and the auxiliary geometry is Ricci flat, while Lorentz symmetry breaking is transferred to the physical metric through the metric-affine deformation. After introducing the areal radius and normalizing the Killing time at spatial infinity, the geometry is controlled by a single invariant deformation parameter. The resulting spacetime is asymptotically conical, possesses a regular Killing horizon, and retains the causal structure of the Schwarzschild black hole, with a curvature singularity located at the origin. Initially, we examine its thermodynamic properties, gravitational Doppler effect, and tidal forces. Lorentz symmetry breaking modifies the Hawking temperature and the magnitude of the tidal field, although the characteristic ratio between radial stretching and transverse compression is preserved. The thermodynamic-topology analysis reveals no critical point within the admissible black hole sector. Furthermore, massless scalar perturbations are also investigated through WKB and characteristic time domain solution, showing decaying profiles throughout the sampled parameter range and deformation-dependent quasinormal frequencies. Finally, light deflection and perihelion advance are used to establish stringent Solar System bounds on the invariant deformation, which, at leading order, depends on a combination of the temporal and norm sectors of the bumblebee field.
Comments62 pages and 12 figures. Suggestions/Comments are welcome (about the contents and refs as well)
