2020/11/26 by Tilak Katoch, Blessy Elizabeth Baby, Blessy E. Baby +5 · 1 citation
Medicine · Physics and Astronomy · #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Heartbeat #Optics #Physics #Pulsars and Gravitational Waves Research #Pulse (music) #Spectral line #Streptococcal Infections and Treatments #astro-ph.HE
paper · pdf · doi:10.1093/mnras/staa3756
17 pages, 13 Figures, 6 Tables; Accepted for publication in MNRAS
arxiv created 2020/11/26 · openalex publication_date 2020/12/03 · openalex created_date 2020/12/07 · arxiv updated 2020/12/16 · openalex updated_date 2026/08/05
ABSTRACT IGR J17091−3624 is a transient galactic black hole which has a distinct quasi-periodic variability known as ‘heartbeat’, similar to the one observed in GRS 1915 + 105. In this paper, we report the results of ∼125 ks AstroSat observations of this source during the 2016 outburst. For the first time, a double-peaked QPO (DPQ) is detected in a few time segments of this source with a difference of δf ∼ 12 mHz between the two peaks. The nature of the DPQ was studied based on hardness ratios and using the static as well as the dynamic power spectrum. Additionally, a low-frequency (25–48 mHz) ‘heartbeat’ single-peak QPO (SPQ) was observed at different intervals of time along with harmonics (50–95 mHz). Broad-band spectra in the range 0.7–23 keV, obtained with Soft X-ray Telescope and Large Area X-ray Proportional Counter, could be fitted well with combination of a thermal Comptonization and a multicolour disc component model. During AstroSat observation, the source was in the soft-intermediate state (SIMS) as observed with Swift/XRT. We present a comparative study of the ‘heartbeat’ state variability in IGR J17091−3624 with GRS 1915 + 105. Significant difference in the timing properties is observed although spectral parameters (Γ ∼ 2.1–2.4 and Tmax ∼ 0.6–0.8 keV) in the broad energy band remain similar. Spectral properties of segments exhibiting SPQ and DPQ are further studied using simple phase-resolved spectroscopy which does not show a significant difference. Based on the model parameters, we obtain the maximum ratio of mass accretion rate in GRS 1915 + 105 to that in IGR J17091−3624 as ∼25: 1. We discuss the implications of our findings and comment on the physical origin of these exotic variabilities.