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Time-domain variability properties of XTE J1650−500 during its 2001 outburst: evidence of disc–jet connection
Monthly Notices of the Royal Astronomical Society ( IF 4.7 ) Pub Date : 2020-08-06 , DOI: 10.1093/mnras/staa2263
Arka Chatterjee 1 , Broja G Dutta 2, 3 , Prantik Nandi 1 , Sandip K Chakrabarti 3
Affiliation  

Evolution of variability properties of Galactic transient sources is a diagnostic tool to understand various regimes of the accretion flow and its dynamics close to the central black hole. In this paper, we concentrate on the variability properties of the X-ray transient XTE J1650-500 and investigate the evolution of viscous delay, time lag, QPO frequency, and their energy dependence throughout the rising phase as observed by RXTE during its outburst in 2001. Our analysis reveals (1) a delay of 12 \pm 1 days between one day averaged hard (5-12 keV) and soft (1.5-3 keV) photon light-curves as observed by RXTE/ASM; (2) QPOs with high rms values are observed in lower energy (4-8 keV) range; (3) the QPO frequencies and associated time lags were anti-correlated during the initial days of the rising phase, and later on, they were found to be correlated; (4) the time lags of iron line photons with respect to hard and soft photons remained almost constant during the initial days of hard state and the lag magnitude increased during the state transition. We perform comparative studies with outbursts of GX 339-4 and XTE J1550-564. We find the evolution of time lags associated with the QPO characteristics during the outburst - stronger QPOs at low energy, and constant lags of broad Fe-line photons present a unique nature of outburst profile in XTE J1650-500. The possible cause of such variabilities is explained by considering disk-jet geometry closer to the central black hole.

中文翻译:

XTE J1650-500 在 2001 年爆发期间的时域变化特性:圆盘喷射连接的证据

银河瞬变源可变性特性的演变是一种诊断工具,可用于了解吸积流的各种状态及其靠近中心黑洞的动力学。在本文中,我们专注于 X 射线瞬态 XTE J1650-500 的可变性特性,并研究了 RXTE 在其爆发期间观察到的整个上升阶段的粘性延迟、时滞、QPO 频率及其能量依赖性的演变。 2001. 我们的分析表明 (1) RXTE/ASM 观察到的一天平均硬 (5-12 keV) 和软 (1.5-3 keV) 光子光曲线之间有 12 pm 1 天的延迟;(2) 在较低能量 (4-8 keV) 范围内观察到具有高 rms 值的 QPO;(3) 在上升阶段的最初几天,QPO 频率和相关的时滞是反相关的,后来发现它们是相关的;(4) 铁线光子相对于硬光子和软光子的时滞在硬态的最初几天几乎保持不变,并且在状态转变期间滞后幅度增加。我们对 GX 339-4 和 XTE J1550-564 的爆发进行了比较研究。我们发现爆发期间与 QPO 特性相关的时间滞后的演变——低能量下更强的 QPO 和宽铁线光子的恒定滞后在 XTE J1650-500 中呈现出独特的爆发剖面性质。通过考虑更靠近中心黑洞的圆盘喷射几何结构来解释这种变化的可能原因。我们对 GX 339-4 和 XTE J1550-564 的爆发进行了比较研究。我们发现爆发期间与 QPO 特性相关的时间滞后的演变——低能量下更强的 QPO 和宽铁线光子的恒定滞后在 XTE J1650-500 中呈现出独特的爆发剖面性质。通过考虑更靠近中心黑洞的圆盘喷射几何结构来解释这种变化的可能原因。我们对 GX 339-4 和 XTE J1550-564 的爆发进行了比较研究。我们发现爆发期间与 QPO 特性相关的时间滞后的演变——低能量下更强的 QPO 和宽铁线光子的恒定滞后在 XTE J1650-500 中呈现出独特的爆发剖面性质。通过考虑更靠近中心黑洞的圆盘喷射几何结构来解释这种变化的可能原因。
更新日期:2020-08-06
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