Long Term Variability of Cyg X-1 I. X-ray spectral-temporal correlations in the hard state

TL;DR

This study analyzes the long-term X-ray spectral-temporal behavior of Cygnus X-1 in the hard state, revealing changes in timing properties, spectral softening, and the association of Lorentzian components with the accretion disk corona.

Contribution

It provides a detailed modeling of the PSD with Lorentzians over several years, identifying state transitions and linking spectral-temporal features to accretion processes.

Findings

PSD modeled as sum of four Lorentzians

Detected state changes with spectral softening and timing shifts

Linked Lorentzian components to accretion disk corona

Abstract

We present the long term evolution of the timing properties of the black hole candidate Cygnus X-1 in the 0.002-128 Hz frequency range as monitored from 1998 to 2001 with the RXTE. The hard state power spectral density (PSD) is well modeled as the sum of four Lorentzians, which describe distinct broad noise components. Before 1998 July, Cyg X-1 was in a "quiet" hard state characterized primarily by the first three of these broad Lorentzians. Around 1998 May, this behavior changed: the total fractional rms amplitude decreased, the peak frequencies of the Lorentzians increased, the average time lag slightly increased, and the X-ray spectrum softened. The change in the timing parameters is mainly due to a strong decrease in the amplitude of the third Lorentzian. Since then, an unusually large number of X-ray flares have been observed. During these "failed state transitions", the X-ray power spectrum changes to that of the intermediate state. Modeling this PSD with the four Lorentzians, we find that the first Lorentzian component is suppressed relative to the second and third Lorentzian. Also the frequency-dependent time lags increase significantly. We confirm the interpretation as failed state transitions with observations from the 2001 Jan. and 2001 Oct. soft states. Such behavior suggests that some or all of the Lorentzian components are associated with the accretion disk corona. We discuss the physical interpretation of our results.