• Understanding the inner structure of accretion disk in GX $17+2$: AstroSat’s outlook

• Fulltext

https://www.ias.ac.in/article/fulltext/joaa/042/0096

• Keywords

Accretion; accretion disk; binaries: close; stars: individual (GX $17+2$); X-rays: binaries.

• Abstract

We performed the timing and spectral studies of a Z source GX $17+2$ observed from Astrosat LAXPC instrument. Cross-Correlation Function (CCF) was performed using soft (3–5 keV) and hard (16–40 keV) X-ray bands across the hardness intensity diagram and found correlated/anti-correlated hard and soft lags which seems to be a common feature in these sources. We performed spectral analysis for few of these observations and found no consistent variation in the spectral parameters during the lags, however 10–40% change was noticed in diskbb and power-law components in few of observations. For the first time, we report the detection of HBOs around $\sim$25 Hz and $\sim$33 Hz along with their harmonics using AstroSat LAXPC data. On comparison with spectral results of HB and other branches, we found that inner disk front is close to the last stable orbit and as such no systematic variations are observed. We suggest that the detected lags are readjustment time scales of corona close to the NS and constrained its height to be around few tens to hundreds of km. The detected lags and no significant variation of inner disk front across the HID stronglyindicate that structural variation in corona is the most possible cause of Z track in HID.

• Author Affiliations

1. Department of Astronomy, Osmania University, Hyderabad 500 007, India.
2. Space Astronomy Group, ISITE Campus, U R Rao Satellite Center, Bangalore 560 037, India.

• Journal of Astrophysics and Astronomy

Volume 42, 2021
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