论文标题
AGN时间特性的相对论轨道模型
A relativistic orbit model for temporal properties of AGN
论文作者
论文摘要
我们提出了一个在狭窄的Seyfert 1（NLSY1）星系中，X射线准周期振荡（QPO）的统一模型，$γ$ -Ray和光带QPO在Blazars中可见。这些QPO的起源归因于电晕或这些AGN喷射的等离子体运动。对于X射线QPO，我们应用了NLSY1 1H 0707-945中两个同时QPO的一般相对论进动模型，并推断出轨道参数，例如发射区域的半径，以及旋转参数$ a $ a $ a $ a用于圆形轨道;在球形轨道溶液的情况下，我们获得了卡特的常量$ q $，$ a $和半径。在其他情况下，只有一个X射线QPO，我们将NLSY1星系的轨道参数REJ REJ 1034+396，2xMM J123103.2+110648，MS 2254.9-3712，MRK 766和MCG-06-30-15。通过应用灯塔模型，我们发现在相对论的MHD框架中，基于JET的$γ$ ray和光学QPO的运动学起源是可能的。基于仅由仅由圆形或球形轨迹组成的血浆轨道能量中的幂律分布的内置汉密尔顿公式，我们表明所得的傅立叶功率谱密度（PSD）具有与ISCO能量相对应的断裂。此外，我们在PSD中的斜率和能量分布的斜率之间得出了连接公式。总体而言，考虑到这些相对论轨道模型的初步但有希望的结果，可以匹配观测到的QPO频率和pSD在内部电动机和喷气机中的不同尺度上，它激发了我们促使我们构建详细模型，包括Corona和相对论MHD JET模型的传输功能，用于等离子体流动及其极化属性。
We present a unified model for X-ray quasi-periodic oscillations (QPOs) seen in Narrow-line Seyfert 1 (NLSy1) galaxies, $γ$-ray and optical band QPOs that are seen in Blazars. The origin of these QPOs is attributed to the plasma motion in corona or jets of these AGN. In the case of X-ray QPOs, we applied the general relativistic precession model for the two simultaneous QPOs seen in NLSy1 1H 0707-945 and deduce orbital parameters, such the radius of the emission region, and spin parameter $a$ for a circular orbit; we obtained the Carter's constant $Q$, $a$, and the radius in the case of a spherical orbit solution. In other cases where only one X-ray QPO is seen, we localized the orbital parameters for NLSy1 galaxies REJ 1034+396, 2XMM J123103.2+110648, MS 2254.9-3712, Mrk 766, and MCG-06-30-15. By applying the lighthouse model, we found that a kinematic origin of the jet based $γ$-ray and optical QPOs, in a relativistic MHD framework, is possible. Based on the inbuilt Hamiltonian formulation with a power-law distribution in the orbital energy of the plasma consisting of only circular or spherical trajectories, we show that the resulting Fourier power spectral density (PSD) has a break corresponding to the energy at ISCO. Further, we derive connection formulae between the slopes in the PSD and that of the energy distribution. Overall, given the preliminary but promising results of these relativistic orbit models to match the observed QPO frequencies and PSD at diverse scales in the inner corona and the jet, it motivates us to build detailed models, including a transfer function for the energy spectrum in the corona and relativistic MHD jet models for plasma flow and its polarization properties.
