论文标题
Maxi〜J1348--630：使用缩放技术估算黑洞质量和二进制倾斜度
MAXI~J1348--630: Estimating the black hole mass and binary inclination using a scaling technique
论文作者
论文摘要
Maxi〜J1348--630中的爆发活动引发了很大的争议，无论消息来源是否包含黑洞（BH）。在这里，我们介绍了使用Swift/XRT数据分析Maxi J348--630爆发的结果。我们发现，所有光谱状态中的能光谱都可以使用组合和高斯铁线成分的组合进行建模。此外，我们表明X射线光子指数Gamma与质量增生率MDOT相关。我们发现，伽玛用MDOT从LHS到HSS单调增加，然后在γ〜3处饱和。这种指数行为与许多其他BH候选者所表现出的行为相似。该结果代表了Maxi〜J1348--630中BH存在的观察证据。我们还表明，伽马的值与QPO频率ν_{L}相关。基于此相关性，我们使用缩放方法将BH质量估计为14.8 +/- 0.9 m _ {\ odot}，使用BH二进制XTE〜J1550--564作为参考来源。 SRG/Erosita最近发现了Maxi〜J1348--630周围巨大的灰尘散射环的发现，对此X射线源进行了完善的距离估计。在此距离的情况下，我们能够使用缩放技术估算磁盘倾斜度i =（65 +/- 7）^0，以使伽马与与MDOT成比例的归一化之间的相关性。随着照明分数的增加，KT_S的初始减少同时减少。在爆发开始时，康普顿云（或“电晕”）非常扩展，因此，从相对较远的磁盘区域注入了电晕的种子光子，KT_S约为0.2---0.4 kev。尽管MDOT增加（或发光度增加），但电晕收缩，从而升高了种子光子温度KT_S。
The outburst activity in the MAXI~J1348--630 has sparked a great deal of controversy, whether the source contains a black hole (BH). Here, we present the results of our analysis of the outburst of MAXI J348--630 using Swift/XRT data. We find that energy spectra in all spectral states can be modeled using a combination of Comptonization and Gaussian iron-line components. In addition, we show that the X-ray photon index, Gamma, is correlated with the mass accretion rate, Mdot. We find that Gamma increases monotonically with Mdot from the LHS to the HSS, and then saturated at Gamma~3. This index behavior is similar to that exhibited by a number of other BH candidates. This result represents observational evidence of the presence of a BH in MAXI~J1348--630. We also show that the value of Gamma is correlated with the QPO frequency, ν_{L}. Based on this correlation, we applied a scaling method to estimate a BH mass of 14.8 +/- 0.9 M_{\odot}, using the BH binary XTE~J1550--564 as a reference source. The recent discovery of a giant dust scattering ring around MAXI~J1348--630 by SRG/eROSITA has refined distance estimates to this X-ray source. With this distance, we were able to estimate the disk inclination i = (65+/- 7)^0 using the scaling technique for the correlation between Gamma and normalization proportional to Mdot. An initial decrease in kT_s occurred simultaneously with an increase in the illumination fraction, f. At the start of the outburst, the Compton cloud (or "corona") is very extended and, thus, the seed photons injected to the corona from the relatively far-away disk region, where kT_s is about 0.2--0.4 keV. While Mdot increases (or luminosity increases), the corona contracts, thus increasing the seed photon temperature, kT_s.
