AI 中文总结
该研究在低能Hořava引力框架下，分析旋转LV黑洞周围辐射低效吸积流照亮的Sgr A*亮环，揭示LV参数对亮环及主图像、n=1光子环的效应，并结合EHT数据约束LV参数与黑洞自旋的关系。
AI 中文摘要
我们在低能Hořava引力框架下，研究了旋转洛伦兹破缺（LV）黑洞周围辐射低效吸积流产生的230 GHz热同步辐射照亮的Sgr A*图像亮环中洛伦兹破缺（LV）的效应。结果表明，LV参数会减小亮环直径，但增大其宽度、光度、方位不对称性和取向角；更高的自旋参数会增强LV对亮环的效应，盘厚度减小会使亮环直径减小并增强LV对该直径的效应，亮环宽度则与盘厚度无系统依赖关系，这些亮环量对旋转LV黑洞的黑洞自旋和LV参数呈现相似的变化趋势。利用Sgr A*的EHT观测数据，我们发现，在固定盘厚度时，LV参数的允许范围随黑洞自旋增大先拓宽后收缩，并向更小的LV参数值偏移；此外，LV参数会缩小黑洞自旋的允许范围：负LV参数值将该范围向更高自旋偏移，正LV参数值则向更低自旋偏移。最后，我们探究了LV参数对旋转LV黑洞的主图像和n=1光子环的峰值位置值及宽度的效应：除狭窄区间外，峰值位置及其宽度随LV参数减小；对于纯开普勒吸积流，不同LV参数的峰值位置差异更显著；此外，纯径向自由下落流产生的主图像和n=1光子环比纯开普勒流产生的对应图像更宽。
英文摘要
We have investigated effects of Lorentz violation (LV) on bright ring in Sgr A* images illuminated by the 230 GHz thermal synchrotron emission from radiation ineffective accretion flows around a rotating LV black hole within the low-energy Hořava gravity framework. Our results reveal that the LV parameter reduces the bright ring diameter yet increases its width, luminosity, azimuthal asymmetry and orientation angle. Higher spin parameter strengthens the LV-induced effects on bright ring properties.Increasing disk thickness reduces the ring diameter and enhances the LV parameter's effects on this diameter. The ring width shows no systematic dependence on the disk thickness. These quantities of bright ring display similar trends against black hole spin and the LV parameter for the rotating LV black hole. Using EHT observational data of Sgr A*, we find that, at fixed disk thickness, the allowed range of the LV parameter first broadens and then contracts with growing black hole spin, and shifts toward smaller LV parameter values. In addition, the LV parameter narrows the permitted range of black hole spin: negative LV parameter values shift this range to higher spin, while positive values shift it to lower spin. Finally, we probe effects of the LV parameter on the peak position value and the width of the primary image and the $n=1$ photon ring for the rotating LV black hole. The peak positions and their widths decrease with the LV parameter, except for a narrow range. The peak position differences for various LV parameter are more pronounced for pure Keplerian accretion flow. In additional, the primary image and the $n=1$ photon ring produced by pure radially free-falling flows are broader than their counterparts generated by pure Keplerian flows.
Comments17 pages, 9 figures
