论文标题
宽带“光谱 - 时空”特征LMC X-1和LMC X-3的特征：Astrosat Perspective
Broadband 'spectro-temporal' features of extragalactic black hole binaries LMC X-1 and LMC X-3: An AstroSat perspective
论文作者
论文摘要
我们使用Astrosat在$ 2016-2020 $的期间内使用Astrosat的所有档案和遗产观察到$ 2016-2020 $的所有档案和遗产观察，介绍了外部黑洞X射线X射线X射线LMC X-1和LMC X-3。从SXT和LAXPC上获得的两个来源的宽带能源光谱（$ 0.5-20 $ keV）的特征是强烈的热盘黑体组件（$ kt_ {in} \ sim1 $ kev，$ f_ {disc}> 79> 79 \％$）以及陡峭的powerlaw（$ uplaws）（$ uplawl）（$ guphlaw）（$γ\ sim \ sim \ sim2.4--2.4-3.2 $ 3.2 $）。 LMC X-1的射光光度从$ 7-10 \％$ $的Eddington发光度（$ L_ {EDD} $）和LMC X-3的范围内$ 7-13 \％$ of $ l_ {EDD} $。我们使用Maxi数据研究光曲线的长期变化，并发现LMC X-1的分数差异为$ \ sim25 \％$，而LMC X-3的LMC X-1和$ \ sim53 \％$。我们检查了这两个源的时间属性，并在频率范围内获得PDS的分数RMS变异性$ 0.002-10 $ Hz为$ \ sim9 \％-17 \％-17 \％$对于LMC X-3的$ \％-17 \％$，以及$ \ sim7 \％-11 \％-11 \％$。 “光谱 - 颞”特性表明这两个来源都处于热支配的软状态。通过使用相对论积聚盘模型对光谱进行建模，我们确定LMC X-1和LMC X-3的质量在$ 7.64-10.00 $ $ $ $ M _ {\ odot} $和$ 5.35-6.22 $ $ M _ {\ odot} $分别。我们还以90 \％的信心将LMC X-1的旋转限制为$ 0.82-0.92 $，而LMC X-3的旋转为0.22-0.41 $。我们讨论了结果在黑洞二进制文件周围积聚动态的背景下的含义，并将其与两个来源的先前发现进行了比较。
We present the first results of extragalactic black hole X-ray binaries LMC X-1 and LMC X-3 using all the archival and legacy observations by AstroSat during the period of $2016-2020$. Broadband energy spectra ($0.5-20$ keV) of both sources obtained from the SXT and LAXPC on-board AstroSat are characterized by strong thermal disc blackbody component ($kT_{in}\sim1$keV, $f_{disc}>79\%$) along with a steep power-law ($Γ\sim2.4-3.2$). Bolometric luminosity of LMC X-1 varies from $7-10\%$ of Eddington luminosity ($L_{Edd}$) and for LMC X-3 is in the range $7-13\%$ of $L_{Edd}$. We study the long-term variation of the light curve using MAXI data and find the fractional variance to be $\sim25\%$ for LMC X-1 and $\sim53\%$ for LMC X-3. We examine the temporal properties of both sources and obtain fractional rms variability of PDS in the frequency range $0.002-10$ Hz to be $\sim9\%-17\%$ for LMC X-1, and $\sim7\%-11\%$ for LMC X-3. The `spectro-temporal' properties indicate both sources are in thermally dominated soft state. By modelling the spectra with relativistic accretion disc model, we determine the mass of LMC X-1 and LMC X-3 in the range $7.64-10.00$ $M_{\odot}$ and $5.35-6.22$ $M_{\odot}$ respectively. We also constrain the spin of LMC X-1 to be in the range $0.82-0.92$ and that of LMC X-3 in $0.22-0.41$ with 90\% confidence. We discuss the implications of our results in the context of accretion dynamics around the black hole binaries and compare it with the previous findings of both sources.
