The basic parameters of γ-ray-loud blazars
The basic parameters of γ-ray-loud blazars
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DOI：
10.1051/0004-6361:20034576
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发表时间：
2005-03
影响因子：
6.5
通讯作者：
J. H. Fan
中科院分区：
文献类型：
--
作者：
J. H. Fan
利用已有的变比时标，我们确定了23颗γ暴blazar的中心黑洞质量（M）、提升因子（或多普勒因子）（δ）、传播角（Φ）和沿轴向到γ射线产生点的沿着距离（d）。在这种方法中，吸收效应取决于γ射线的能量、辐射大小和吸积盘的性质。用内禀γ射线光度作为爱丁顿光度的分数A，则γ中的L = λL Edd。并且光学深度等于1，我们可以确定中心黑洞质量的上限。我们发现黑洞质量在10 - 7 M ○之间。和10 9 M ○。当A = 0.1和1.0时，由于该方法是基于γ射线辐射和源的短时标，因此也可用于高红移γ射线源的中心黑洞质量测定。在黑洞质量上限的情况下，Bls和FSRQs没有明显区别，表明中心黑洞质量在blazar演化序列中不起重要作用。
We determined the basic parameters, such as the central black hole mass (M), the boosting factor (or Doppler factor) (6), the propagation angle (Φ) and the distance along the axis to the site of γ-ray production (d) for 23 γ-ray-loud blazars using their available variability timescales. In this method, the absorption effect depends on the γ-ray energy, emission size and property of the accretion disk. Using the intrinsic γ-ray luminosity as a fraction A of the Eddington luminosity, L in γ = λL Edd . and the optical depth equal to unity, we can determine the upper limit of the central black hole masses. We found that the black hole masses range between 10 7 M ○. and 10 9 M ○. when A = 0.1 and 1.0 are adopted. Since this method is based on gamma-ray emissions and the short time-scale of the sources, it can also be used for central black hole mass determination of high redshift gamma-ray sources. In the case of the upper limit of black hole mass there is no clear difference between BLs and FSRQs, which suggests that the central black hole masses do not play an important role in the evolutionary sequence of blazars.