We present our AstroSat soft X-ray observations of a compact binary system, AR Sco, and analysis of its X-ray observations with Chandra that were taken only about a week before the AstroSat observations. An analysis of the soft X-ray (0.3–2.0 keV) data limits the modulation of the spin, orbital, or beat periods to less than 0.03 counts s\(^{-1}\) or <10% of the average count rate. The X-ray flux obtained from both observatories is found to be almost identical (within a few percent) in flux, and about 30% lower than reported from the nine months older observations with XMM-Newton. A two-temperature thermal plasma model with the same spectral parameters fit Chandra and AstroSat data very well, and requires very little absorption in the line of sight to the source. The low-temperature component has the same temperature (\(\sim \)1 keV) as reported earlier, but the high-temperature component has a lower temperature of 5.0\(^{+0.8}_{-0.7}\) keV as compared to 8.0 keV measured earlier, however, the difference is not statistically significant.

我们展示了我们对紧凑双星系统 AR Sco的AstroSat软 X 射线观测，以及使用Chandra对其 X 射线观测的分析，这些观测仅在AstroSat观测前一周进行。对软 X 射线 (0.3–2.0 keV) 数据的分析将自旋、轨道或节拍周期的调制限制为小于 0.03 计数 s \(^{-1}\)或 < 平均计数的 10%速度。发现从两个天文台获得的 X 射线通量几乎相同（在几个百分点之内），比XMM-牛顿9 个月前的观测报告低约 30% 。具有相同光谱参数的双温度热等离子体模型拟合Chandra和AstroSat数据非常好，并且在到源的视线中几乎不需要吸收。低温组件的温度与之前报道的相同 ( \(\sim \) 1 keV)，但高温组件的温度较低，为 5.0 \(^{+0.8}_{-0.7}\)  keV然而，与之前测量的 8.0 keV 相比，差异在统计上并不显着。