Multi-wavelength view of the galactic black-hole binary GRS 1716-249. (arXiv:2012.12616v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Rout_S/0/1/0/all/0/1">Sandeep K. Rout</a> (1 and 2), <a href="http://arxiv.org/find/astro-ph/1/au:+Vadawale_S/0/1/0/all/0/1">Santosh V. Vadawale</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+E%2E_A/0/1/0/all/0/1">Aarthy E.</a> (1 and 2), <a href="http://arxiv.org/find/astro-ph/1/au:+Ganesh_S/0/1/0/all/0/1">Shashikiran Ganesh</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Joshi_V/0/1/0/all/0/1">Vishal Joshi</a> (1), <a href="http://arxiv.org/find/astro-ph/1/au:+Roy_J/0/1/0/all/0/1">Jayashree Roy</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Misra_R/0/1/0/all/0/1">Ranjeev Misra</a> (3), <a href="http://arxiv.org/find/astro-ph/1/au:+Yadav_J/0/1/0/all/0/1">J. S. Yadav</a> (4) ((1) Physical Research Laboratory Ahmedabad India (2) Indian Institute of Technology Gandhinagar India (3) The Inter-University Center for Astronomy and Astrophysics Pune India and (4) Indian Institute of Technology Kanpur India)
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.
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.
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