Failed-transition outbursts in black hole low-mass X-ray binaries
Failed-transition outbursts in black hole low-mass X-ray binaries
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DOI：
10.1093/mnras/stab2241
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发表时间：
2021-07
影响因子：
4.8
通讯作者：
K. Alabarta;D. Altamirano;M. M'endez;V. C'uneo;F. Vincentelli;N. Castro-Segura;F. García;B. Luff;A. V. S. O. Physics;Astronomy;U. Southampton;K. Institute;U. Groningen;Instituto de Astrof'isica de Canarias-Instituto-de-Astrof'isica-de-Canarias-1410640555;D. D. Astrof'isica-D.;U. L. Laguna;D. O. Physics;Nordita;K. R. I. O. Technology;S. University;S. Sciences
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文献类型：
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作者：
K. Alabarta;D. Altamirano;M. M'endez;V. C'uneo;F. Vincentelli;N. Castro-Segura;F. García;B. Luff;A. V. S. O. Physics;Astronomy;U. Southampton;K. Institute;U. Groningen;Instituto de Astrof'isica de Canarias-Instituto-de-Astrof'isica-de-Canarias-1410640555;D. D. Astrof'isica-D.;U. L. Laguna;D. O. Physics;Nordita;K. R. I. O. Technology;S. University;S. Sciences
黑洞低质量x射线双星（BH LMXBs）在爆发过程中以类似的方式演化。基于x射线光谱和变异性，这种演化可以分为三种典型状态：低/硬、中、高/软状态。BH lmxb在一些爆发（这里称为“完全爆发”）中通过中间状态从低/硬状态演变到高/软状态。然而，在其他情况下，BH lmxb经历了源从未达到高/软状态的爆发，这里称为“失败跃迁爆发”（FT爆发）。从经历128次爆发的56个BH lmxb样本中，我们发现这些BH lmxb中有36%经历了至少一次FT爆发，而FT爆发占样本爆发的33%，表明这些是常见事件。我们比较了来自RXTE/PCA、Swift/BAT和MAXI的所有可用的BH lmxb全爆发和全爆发的x射线数据，发现在爆发开始后的最初10-60天内，FT和全爆发无法从它们的x射线光曲线、硬度-强度图或x射线变异性中区分出来。这表明两种类型的爆发都是由相同的物理过程驱动的。我们还比较了FT和GX 339−4全爆发的光学和红外（O/IR）数据。我们发现，在FT爆发之前，该系统的O/IR波段通常更亮，这表明O/IR通量指向后来导致FT爆发的物理过程。我们在描述吸积x射线双星爆发的开始和演化的模型背景下讨论我们的结果。
Black hole low-mass X-ray binaries (BH LMXBs) evolve in a similar way during outburst. Based on the X-ray spectrum and variability, this evolution can be divided into three canonical states: low/hard, intermediate, and high/soft state. BH LMXBs evolve from the low/hard to the high/soft state through the intermediate state in some outbursts (here called ‘full outbursts’). However, in other cases, BH LMXBs undergo outbursts in which the source never reaches the high/soft state, here called ‘failed-transition outbursts’ (FT outbursts). From a sample of 56 BH LMXBs undergoing 128 outbursts, we find that 36 per cent of these BH LMXBs experienced at least one FT outburst, and that FT outbursts represent ∼33 per cent of the outbursts of the sample, showing that these are common events. We compare all the available X-ray data of full and FT outbursts of BH LMXBs from RXTE/PCA, Swift/BAT, and MAXI, and find that FT and full outbursts cannot be distinguished from their X-ray light curves, hardness–intensity diagrams, or X-ray variability during the initial 10–60 d after the outburst onset. This suggests that both types of outbursts are driven by the same physical process. We also compare the optical and infrared (O/IR) data of FT and full outbursts of GX 339−4. We found that this system is generally brighter in O/IR bands before an FT outburst, suggesting that the O/IR flux points to the physical process that later leads to a full or an FT outburst. We discuss our results in the context of models that describe the onset and evolution of outbursts in accreting X-ray binaries.