MAXI ~ J1348 --630：用定标技术估算黑洞质量和双星倾角
MAXI~J1348--630: Estimating the black hole mass and binary inclination using a scaling technique
摘要：
MAXI~J1348--630的爆发活动引发了很大的争议，即爆发源是否包含一个黑洞（BH）。在这里，我们提出了我们的分析结果的爆发MAXI J348- 630使用Swift/XRT数据。我们发现，在所有的光谱状态的能谱可以建模使用康普顿化和高斯铁线组件的组合。此外，我们表明，X射线光子指数，伽玛，与质量吸积率，Mdot。我们发现，从LHS到HSS，Gamma随Mdot单调增加，然后在Gamma~3处饱和。该索引行为类似于许多其他BH候选者所表现出的索引行为。这一结果代表了MAXI~J1348- 630中存在BH的观测证据。我们还发现Gamma值与QPO频率ν_{L}相关。基于这种相关性，我们采用一种定标方法，以BH双星XTE~J1550- 564为参考源，估算出BH的质量为14.8 +/- 0.9 M_{\odot}。SRG/eROSITA最近在MAXI~J1348- 630周围发现了一个巨大的尘埃散射环，这一发现改进了对该X射线源的距离估计。有了这个距离，我们就能够利用Gamma和与Mdot成比例的归一化之间的相关性的缩放技术来估计盘倾角i =（65+/- 7）^0。初始kT_s的降低与光照分数f的增加同时发生。在爆发开始时，康普顿云（或“日冕”）非常扩展，因此种子光子从相对较远的盘区注入日冕，那里kT_s约为0.2- 0.4 keV。当Mdot增加（或亮度增加）时，日冕收缩，从而增加种子光子温度kT_s。
英文摘要：
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.
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