类星体的动能和MOJAVE超光速运动的统计超量
Kinetic power of quasars and statistical excess of MOJAVE superluminal motions
摘要：
MOJAVE巡天包含101个类星体，共观测到354个不同于射电核心的射电分量，其中95%以相对于核心的视投影超光速运动，45%的投影速度大于10 c（最大速度为60 c）。多普勒增强效应进行了分析，以确定超光速运动的统计。我们在所有可能的洛伦兹因子值上积分对应于每个分量的动能值。通过假设最小能量状态来计算喷射中的质量。该动能乘以产生被标识为“液滴”的喷射流体部分的频率。因此，我们在pc尺度上估计了类星体以动能形式长期释放的平均总功率。结果在选择效应中，类星体的核心和斑点都受到多普勒增强的巨大影响，这增加了在视线10度范围内发现喷流的概率，比人们对随机喷射分布的预期高出约40倍，这解释了上面给出的非常高的投影速度的比率。每个MOJAVE类星体的平均总动力学功率应该非常高，以获得这种分布：~ 7 E47 erg/s。这一数值远高于先前对kpc尺度的动能功率的估计，该估计是基于对射电光度低得多但黑洞质量相似的天体样本中X射线气体或射电瓣中的空洞的分析。动力学功率是爱丁顿光度的重要组成部分，在辐射热光度的数量级上，并且平均与射电光度的平方根成比例，尽管这种相关性可能是由类似马尔奎斯特的偏差引起的。
英文摘要：
The MOJAVE survey contains 101 quasars with a total of 354 observed radio components that are different from the radio cores, among which 95% move with apparent projected superluminal velocities with respect to the core, and 45% have projected velocities larger than 10c (with a maximum velocity 60c). Doppler boosting effects are analyzed to determine the statistics of the superluminal motions. We integrate over all possible values of the Lorentz factor the values of the kinetic energy corresponding to each component. The calculation of the mass in the ejection is carried out by assuming the minimum energy state. This kinetic energy is multiplied by the frequency at which the portions of the jet fluid identified as "blobs" are produced. Hence, we estimate the average total power released by the quasars in the form of kinetic energy in the long term on pc-scales. RESULTS. A selection effect in which both the core and the blobs of the quasar are affected by huge Doppler-boosting enhancement increases the probability of finding a jet ejected within 10 degrees of the line of sight >~40 times above what one would expect for a random distribution of ejection, which explains the ratios of the very high projected velocities given above. The average total kinetic power of each MOJAVE quasar should be very high to obtain this distribution: ~7E47 erg/s. This amount is much higher than previous estimates of kinetic power on kpc-scales based on the analysis of cavities in X-ray gas or radio lobes in samples of objects of much lower radio luminosity but similar black hole masses. The kinetic power is a significant portion of the Eddington luminosity, on the order of the bolometric luminosity, and proportional on average to square root of the radio luminosity, although this correlation might be induced by Malmquist-like bias.
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