论文标题
瞬态BE/X射线二进制的无线电监视和强磁化的中子星的出入流量耦合
Radio monitoring of transient Be/X-ray binaries and the inflow-outflow coupling of strongly-magnetized accreting neutron stars
论文作者
论文摘要
强烈磁化（$ b \ geq10^{12} $ g）积聚中子星（NSS）是研究具有坚实表面的物体对喷气机推出的主要目标；尽管经典的喷气发射模型预测这种NSS无法发射喷气机，但最近的观察和模型也是如此。瞬态BE/X射线二进制文件（BEXRB）是探测这种射流形成的参数空间不佳的关键实验室。在这里，我们介绍了四个爆发中的三个BEXRB的协调监控活动：SAX 2103.5+4545、1A 0535+262和GRO J1008-57的巨大爆发以及后者的I型I爆炸。在二十个观察结果中，我们获得了1A 0535+262的无线电检测，而其他目标仍未发现，以$ 20 $ - $ 50 $ $ $ $ $ $ $ $ jy的典型限制。 1A 0535+262的无线电发光度与其不断发展的X射线光度呈正相关，并且居住在$ L_X $ -L_R $平面的一个区域，继续以前在Bexrb Swift J0243.6+6124上观察到的相关性。我们测量bexrb $ l_x $ - $ l_r $耦合指数为$β= 0.86 \ pm 0.06 $（$ l_r \ propto l_x^β$），类似于在NS和黑洞和黑洞低质量X射线二进制文件中测得的指数。令人惊讶的是，耦合的$ L_R $归一化为$ \ sim 275 $和$ \ sim 6.2 \ times10^3 $倍，分别比这两个比较样本低。我们得出的结论是，射流发射可能在巨大爆发的主要峰值中占主导地位，但仅在当前无线电敏感性下用于近距离或超级埃德丁顿系统。我们在X射线二进制无线电研究的更广泛背景下讨论了这些结果，得出的结论是，我们的结果表明，超级X射线二进制文件如何容纳当前未识别的其他无线排放机制。
Strongly-magnetized ($B\geq10^{12}$ G) accreting neutron stars (NSs) are prime targets for studying the launching of jets by objects with a solid surface; while classical jet-launching models predict that such NSs cannot launch jets, recent observations and models argue otherwise. Transient Be/X-ray binaries (BeXRBs) are critical laboratories for probing this poorly-explored parameter space for jet formation. Here, we present the coordinated monitoring campaigns of three BeXRBs across four outbursts: giant outbursts of SAX 2103.5+4545, 1A 0535+262, and GRO J1008-57, as well as a Type-I outburst of the latter. We obtain radio detections of 1A 0535+262 during ten out of twenty observations, while the other targets remained undetected at typical limits of $20$-$50$ $μ$Jy. The radio luminosity of 1A 0535+262 positively correlates with its evolving X-ray luminosity, and inhabits a region of the $L_X$-$L_R$ plane continuing the correlation observed previously for the BeXRB Swift J0243.6+6124. We measure a BeXRB $L_X$-$L_R$ coupling index of $β= 0.86 \pm 0.06$ ($L_R \propto L_X^β$), similar to the indices measured in NS and black hole low-mass X-ray binaries. Strikingly, the coupling's $L_R$ normalisation is $\sim 275$ and $\sim 6.2\times10^3$ times lower than in those two comparison samples, respectively. We conclude that jet emission likely dominates during the main peak of giant outbursts, but is only detectable for close-by or super-Eddington systems at current radio sensitivities. We discuss these results in the broader context of X-ray binary radio studies, concluding that our results suggest how supergiant X-ray binaries may host a currently unidentified additional radio emission mechanism.
