Vanishing hardness-flux correlation in Cygnus X-1: signs of the disc moving out

TL;DR

This study examines high-hardness, low-flux states of Cygnus X-1, revealing a vanishing hardness-flux correlation and suggesting the accretion disc moves outward, affecting characteristic frequencies and variability timescales.

Contribution

It provides new insights into the disc geometry during high-hardness states by linking PDS features and hardness-flux behavior to the disc's inner radius.

Findings

Characteristic frequencies are at their lowest in high-hardness states.

Weak or absent hardness-flux correlation during these states.

Inner disc radius estimated to be greater than 50 Rg.

Abstract

Aims. We investigate observations of the X-ray binary Cygnus X-1 with unusually high hardness and low flux. In particular, we study the characteristic frequencies seen in the PDS and the hardness-flux correlation within and between these observations. Methods. We analyse observations of Cyg X-1 during periods when the source reaches its highest hardness levels (> 1 for the 9-20 keV over 2-4 keV RXTE/PCA count ratios, corresponding to Gamma < 1.6). Using the relativistic precession model to interpret the PDS we estimate a value for the inner radius of the accretion disc. We also study the hardness-flux correlation. Results. In the selected observations, the characteristic frequencies seen in the power spectrum are shifted to the lowest end of their frequency range. Within a single observation, the hardness-flux correlation is very weak, contrary to the negative correlation normally observed in the hard state. We suggest that this could be interpreted as the inner disc boundary being at large radii (> 50 Rg), thereby requiring more time to adjust to a changing accretion rate than allowed by a single RXTE observation, and compare our findings to estimates of the viscous time scale responsible for small scale variability in the system.