2020/12/31 by Sandeep K. Rout, Santosh V. Vadawale, Aarthy E. +6 · 1 citation
Physics and Astronomy · #Accretion (finance) #Accretion disc #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Binary number #Emission spectrum #Gamma-ray bursts and supernovae #Infrared #Infrared excess #Spectral energy distribution #Synchrotron #Synchrotron radiation #astro-ph.HE
paper · pdf · doi:10.1007/s12036-021-09696-5
published as Journal of Astrophysics and Astronomy volume 42, Article number: 39 (2021) · 11 pages, 8 figures and 2 tables. Published in the Journal of Astrophysics & Astronomy
openalex created_date 2021/01/05 · arxiv created 2021/06/11 · openalex publication_date 2021/06/11 · arxiv updated 2021/06/15 · openalex updated_date 2026/08/05
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 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. We have studied the multi-wavelength spectral energy distribution of the galactic X-ray binary GRS 1716-249 ranging from near infrared (0.0005 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.