论文标题
使用XMM-Newton卫星研究Blazar的日内通量分布的研究
Study of Intra-Day Flux Distributions of Blazars Using XMM-Newton Satellite
论文作者
论文摘要
我们对使用XMM-Newton观测值进行了15个中间体和低能峰的样品的通量分布，总共在短期时间表上进行了57个时期。我们使用过量的分数可变性幅度表征了所有光曲线的X射线变异性，发现7个来源中只有24个光曲线显着可变。为了表征这些Blazar中X射线变异性的起源，我们使用高斯和对数正态分布符合所有这些光曲线的通量分布，因为任何非高斯扰动都可以表明吸积盘中波动的烙印，这可以通过Blazars中的Relativicistic Jets来增强多普勒。但是，如我们的观察结果所示，日内变异性很难使用圆盘成分来调和，因为这些来源中的排放主要由喷气机主导。我们使用了Anderson-Darling（AD）和$χ^{2} $测试来适合直方图。在11个观察结果中，即231、3C 273，PKS 0235+164和PKS 0521-365中，这两个模型同样适合通量分布。在其余的观测值中，我们无法用任何分布对它们进行建模。在两个来源，即Bl lacertae和S4 0954+650中，对数正态分布比正态分布优选，这可能是由于相对论的Jets或线性高斯扰动在粒子时间尺度中导致这种磁通分布的非高斯扰动所引起的。
We present a study of the flux distribution of a sample of 15 Intermediate and Low-energy peaked blazars using XMM-Newton observations in a total of 57 epochs on short-term timescales. We characterise the X-ray variability of all of the light curves using excess fractional variability amplitude and found that only 24 light curves in 7 sources are significantly variable. In order to characterise the origin of X-ray variability in these blazars, we fit the flux distributions of all these light curves using Gaussian and lognormal distributions, as any non-Gaussian perturbation could indicate the imprints of fluctuations in the accretion disc, which could be Doppler boosted through the relativistic jets in blazars. However, intra-day variability, as seen in our observations, is difficult to reconcile using disc components as the emissions in such sources are mostly dominated by jets. We used Anderson-Darling (AD) and $χ^{2}$ tests to fit the histograms. In 11 observations of 4 blazars, namely, ON 231, 3C 273, PKS 0235+164 and PKS 0521-365, both models equally fit the flux distributions. In the rest of the observations, we are unable to model them with any distribution. In two sources, namely, BL Lacertae and S4 0954+650, the lognormal distribution is preferred over the normal distribution, which could arise from non-Gaussian perturbations from relativistic jets or linear Gaussian perturbation in the particle time scale leading to such flux distributions.
