In 2016–17, the Galactic transient black hole candidate GRS 1716-249 exhibited an outburst event after a long quiescence period of almost 23 years. The source remained in the outbursting phase for almost 9 months. We study the spectral and temporal properties of the source during this outburst using archival data from four astronomy satellites, namely MAXI, Swift, NuSTAR and AstroSat. Initial spectral analysis is done using combined disk black body and power-law models. For a better understanding of the accretion flow properties, we studied spectra with the physical two component advective flow (TCAF) model. Accretion flow parameters are extracted directly from the spectral fits with the TCAF model. Low frequency quasi periodic oscillations are also observed in the Swift/XRT and AstroSat/LAXPC data. From the spectral fit, we also estimate the probable mass of GRS 1716-249 to be in the range of 4.50–\(5.93 M_{\odot }\) or \(5.01^{+0.92}_{-0.51} M_{\odot }\). Refitting of all spectra is done by freezing the mass at its average value. An insignificant deviation of the TCAF model parameters is observed. From the nature of the variation of the newly fitted spectral and temporal properties, we find that the source stays in only the harder (hard and hard-intermediate) states during the outburst. It does not make a transition to the softer states which makes it a ‘failed’ outburst.

在 2016-17 年，银河瞬变黑洞候选者 GRS 1716-249 在经历了近 23 年的长期静止期后表现出爆发事件。源头在爆发阶段保持了近 9 个月。我们使用来自四颗天文卫星（即 MAXI、Swift、NuSTAR 和 AstroSat）的档案数据研究了这次爆发期间震源的光谱和时间特性。初始光谱分析是使用组合的圆盘黑体和幂律模型完成的。为了更好地理解吸积流特性，我们使用物理双分量平流 (TCAF) 模型研究了光谱。吸积流参数直接从 TCAF 模型的光谱拟合中提取。在 Swift/XRT 和 AstroSat/LAXPC 数据中也观察到低频准周期性振荡。从光谱拟合，\(5.93 M_{\odot }\)或\(5.01^{+0.92}_{-0.51} M_{\odot }\)。通过将质量冻结为其平均值来重新拟合所有光谱。观察到 TCAF 模型参数的微小偏差。从新拟合的光谱和时间特性的变化性质来看，我们发现源在爆发期间仅停留在较硬（硬和硬中间）状态。它不会过渡到较软的状态，这使其成为“失败”的爆发。