论文标题
Astrosat在Maxi J1535-571中观察非共鸣型C QPO
AstroSat Observation of Non-Resonant Type-C QPOs in MAXI J1535-571
论文作者
论文摘要
银河瞬态黑洞候选者（BHC）Maxi J1535-571在2017年9月02日被{\ it Maxi}/gsc同时发现，{\ it Swift}/bat Instruments。印度在2017 - 18年度爆发的上升阶段，印度的第一个多波长天文卫星{\ it astrosat}也观察到了这一点。我们使用{\ it astrosat}的大面积X射线比例计数器（LAXPC）的数据在2017年9月12日至17日对源的光谱和时间分析进行了，以$ 3-40 $ 〜KEV推断来源的积聚流量。通过基于物理的两组分流流（TCAF）解决方案{\ it FITS}文件进行光谱分析。根据TCAF模型拟合物理流程参数的变化的性质，我们得出结论并确认源在我们的分析期间处于中间光谱状态。我们在$ \ sim 1.75-2.81 $ 〜Hz的频率范围内观察到尖锐的C型准周期振荡（QPO）。为了更好地理解这些类型C QPO的性质和演变，对功率密度光谱进行了动态研究。我们还通过冲击振荡模型研究了这些QPO的起源。我们发现，兰金·霍尼奥特（Rankine-Hugoniot）条件不满意，而不是它们的共振振荡是观察到的型C QPO的原因。
Galactic transient black hole candidate (BHC) MAXI J1535-571 was discovered on 2017 September 02 simultaneously by {\it MAXI}/GSC and {\it Swift}/BAT instruments. It has also been observed by India's first multi-wavelength astronomy-mission satellite {\it AstroSat}, during the rising phase of its 2017-18 outburst. We make both the spectral and the temporal analysis of the source during 2017 September 12-17 using data of {\it AstroSat}'s Large Area X-ray Proportional Counter (LAXPC) in the energy range of $3-40$~keV to infer the accretion flow properties of the source. Spectral analysis is done with the physical two-component advective flow (TCAF) solution-based {\it fits} file. From the nature of the variation of the TCAF model fitted physical flow parameters, we conclude and confirm that the source was in the intermediate spectral state during our analysis period. We observe sharp type-C quasi-periodic oscillations (QPOs) in the frequency range of $\sim 1.75-2.81$~Hz. For a better understanding of the nature and evolution of these type-C QPOs, a dynamic study of the power density spectra is done. We also investigate the origin of these QPOs from the shock oscillation model. We find that non-satisfaction of Rankine-Hugoniot conditions for non-dissipative shocks and not their resonance oscillations is the cause of the observed type-C QPOs.
