The origins of X-ray and radio emissions during an X-ray binary outburst are comparatively better understood than those of ultraviolet, optical and infrared radiation. This is because multiple competing mechanisms – emission from intrinsic and irradiated disk, secondary star emission, synchrotron emission from jet and/or non-thermal electron cloud, etc – peak in these mid-energy ranges. Ascertaining the true emission mechanism and segregating the contribution of different mechanisms, if present, is important for correct understanding of the energetics of the system and hence its geometry and other properties. We have studied the multi-wavelength spectral energy distribution of the galactic X-ray binary GRS 1716-249 ranging from near infrared (\(5 \times 10^{-4}\) keV) to hard X-rays (120 keV) using observations from AstroSat, Swift, and Mount Abu Infrared Observatory. Broadband spectral fitting suggests that the irradiated accretion disk dominates emission in ultraviolet and optical regimes. The near infrared emission exhibits some excess than the prediction of the irradiated disk model, which is most likely due to Synchrotron emission from jets as suggested by radio emission. Irradiation of the inner disk by the hard X-ray emission from the Corona also plays a significant role in accounting for the soft X-ray emission.

在 X 射线双星爆发期间 X 射线和无线电发射的起源比紫外线、光学和红外线辐射的起源更容易理解。这是因为多种相互竞争的机制——来自内在和受辐照盘的发射、二次星发射、来自喷射和/或非热电子云的同步加速器发射等——在这些中等能量范围内达到峰值。确定真正的发射机制并分离不同机制的贡献（如果存在）对于正确理解系统的能量学及其几何形状和其他属性很重要。我们研究了银河系 X 射线双星 GRS 1716-249 的多波长光谱能量分布，范围从近红外 ( \(5 \times 10^{-4}\) keV) 到硬 X 射线 (120 keV) 使用来自 AstroSat、Swift和 Mount Abu 红外天文台的观测。宽带光谱拟合表明，受辐照的吸积盘在紫外线和光学区域中占主导地位。近红外发射显示出比辐照盘模型的预测多一些，这很可能是由于射流发射所暗示的喷流的同步加速器发射。来自日冕的硬 X 射线辐射对内盘的辐射在解释软 X 射线发射方面也起着重要作用。