论文标题
X射线二进制中的积聚圆盘喷射耦合
Accretion Disc-Jet Couplings in X-ray Binaries
论文作者
论文摘要
当伴侣恒星的物质朝向中央紧凑型增生器（即黑洞（BH）或中子星（NS））时，会形成积聚盘和喷气流出，从而提供BIGHT X射线和无线电发射，这被称为X射线二进制文件（XRBS）。在低/硬状态下，XRB中存在圆盘喷射耦合，但仍不确定射流功率是来自光盘还是中央吸积。此外，与NSXRB相比，BHXRB具有不同的特性：静态BHXRB通常比X射线中的NSXRB低两到三个数量级，而BHXRB比NSXRB的无线电大。在观察中，无线电和X射线发光度之间已经建立了经验相关性，$ l _ {\ rm rm r} \ propto l _ {\ rm x}^b $，其中$ b \ sim 0.7 $用于bhxrbs和$ b \ sim 1.4 $用于非脉冲NSXRBS。但是，有一些BHXRB的异常值表现出异常陡峭的相关性，就像NSXRB较高的亮度相关性。在这项工作中，在假设喷气功率的起源与内盘的内部能量有关的假设下，我们将磁化，辐射有效的薄盘模型以及众所周知的辐射效率低效率的积聚流模型应用于NSXRBS和BHXRB。我们发现，通过圆盘喷射耦合可以很好地理解XRB中观察到的无线电/X射线相关性。
When the matter from a companion star is accreted towards the central compact accretor, i.e. a black hole (BH) or a neutron star (NS), an accretion disc and a jet outflow will form, providing bight X-ray and radio emission, which is known as X-ray binaries (XRBs). In the low/hard state, there exist disc-jet couplings in XRBs, but it remains uncertain whether the jet power comes from the disc or the central accretor. Moreover, BHXRBs have different properties compared with NSXRBs: quiescent BHXRBs are typically two to three orders of magnitude less luminous than NSXRBs in X-ray, whereas BHXRBs are more radio loud than NSXRBs. In observations, an empirical correlation has been established between radio and X-ray luminosity, $L_{\rm R} \propto L_{\rm X}^b$, where $b\sim 0.7$ for BHXRBs and $b \sim 1.4$ for non-pulsating NSXRBs. However, there are some outliers of BHXRBs showing unusually steep correlation as NSXRBs at higher luminosities. In this work, under the assumption that the origin of jet power is related to the internal energy of the inner disc, we apply our magnetized, radiatively efficient thin disc model and the well-known radiatively inefficient accretion flow model to NSXRBs and BHXRBs. We find that the observed radio/X-ray correlations in XRBs can be well understood by the disc-jet couplings.
