标题： 新黑洞X射线双星Swift J1910.2-0546状态过渡的多波长观测 显示英文标题

标题： Multi-Wavelength Coverage of State Transitions in the New Black Hole X-Ray Binary Swift J1910.2-0546

摘要： 理解黑洞如何吸积物质并向其环境提供反馈是现代天体物理学面临的重大挑战之一。 Swift J1910.2-0546 是一个候选的低质量X射线双星黑洞系统，它于2012年在进入吸积爆发时被发现。 为了研究这个双星系统的配置和吸积形态，我们使用Swift和SMARTS，在X射线、紫外、光学（B、V、R、I）以及近红外（J、H、K）波段监测了约3个月的爆发演化。 该源从硬X射线谱态演变为软X射线谱态，伴随有一个相对较冷的吸积盘，在~0.5 keV处达到峰值。 在此软态期间获得的Chandra/HETG光谱未揭示出电离盘风的特征。 低盘温以及无法检测到风的存在可能表明该系统以相对较低的倾角观测。 多波段光变曲线揭示了两个值得注意的特征，似乎与X射线态的变化有关。 首先，在源进入软态前约1-2周，在所有波段观察到了显著的流量下降。 这个下降在(0.6-10 keV) X射线中比在更长波长上晚了大约6天发生，这可能反映了盘的粘滞时间尺度。 其次，在源转回硬态约两周后，紫外发射显著增加，而X射线则持续衰减。 我们讨论了这些观测结果如何可能反映吸积流形态的变化，也许与喷流的熄灭/发射或热流的坍缩/恢复有关。 显示英文摘要

摘要： Understanding how black holes accrete and supply feedback to their environment is one of the outstanding challenges of modern astrophysics. Swift J1910.2-0546 is a candidate black hole low-mass X-ray binary that was discovered in 2012 when it entered an accretion outburst. To investigate the binary configuration and the accretion morphology we monitored the evolution of the outburst for ~3 months at X-ray, UV, optical (B,V,R,I), and near-infrared (J,H,K) wavelengths using Swift and SMARTS. The source evolved from a hard to a soft X-ray spectral state with a relatively cold accretion disk that peaked at ~0.5 keV. A Chandra/HETG spectrum obtained during this soft state did not reveal signatures of an ionized disk wind. Both the low disk temperature and the absence of a detectable wind could indicate that the system is viewed at relatively low inclination. The multi-wavelength light curves revealed two notable features that appear to be related to X-ray state changes. Firstly, a prominent flux decrease was observed in all wavebands ~1-2 weeks before the source entered the soft state. This dip occurred in (0.6-10 keV) X-rays ~6 days later than at longer wavelengths, which could possibly reflect the viscous time scale of the disk. Secondly, about two weeks after the source transitioned back into the hard state, the UV emission significantly increased while the X-rays steadily decayed. We discuss how these observations may reflect changes in the accretion flow morphology, perhaps related to the quenching/launch of a jet or the collapse/recovery of a hot flow.