2021/02/04 by Kaushik Chatterjee, Dipak Debnath, Debjit Chatterjee +4
Earth and Planetary Sciences · Physics and Astronomy · #Accretion (finance) #Accretion disc #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Gamma-ray bursts and supernovae #High-pressure geophysics and materials #Physics #Spectral analysis #Spectral line #Spectral properties #Spectroscopy #astro-ph.HE
paper · pdf · doi:10.1007/s10509-021-03967-x
18 Pages, 8 Figures, 3 Tables (in Communication)
arxiv created 2021/02/04 · openalex created_date 2021/02/15 · openalex publication_date 2021/07/01 · arxiv updated 2021/08/25 · openalex updated_date 2026/08/05
In 2016-17, the Galactic transient black hole candidate GRS 1716-249 exhibited an outburst event after a long period of quiescence of almost 23 years. The source remained in the outbursting phase for ∼ 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 nature of the variation of the spectral and temporal properties, we find the source remains in hard state during the entire outburst. It never had a transition to other states which makes this event a `failed' outburst. An absence of the softer spectral states is consistent with the class of short orbital period objects, where the source belongs to. 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 5.02+0.91-0.52 M_\odot.