Open AccessOn the X‐ray time‐lags in the black hole candidates
Author(s) -
Kotov O.,
Churazov E.,
Gilfanov M.
Publication year - 2001
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2001.04769.x
Subject(s) - physics , component (thermodynamics) , astrophysics , range (aeronautics) , black hole (networking) , energy (signal processing) , computational physics , quantum mechanics , computer network , routing protocol , routing (electronic design automation) , computer science , composite material , link state routing protocol , materials science
It is shown that the energy dependence of the time‐lags in Cygnus X‐1 excludes any significant contribution of the standard reflected component to the observed lags. The conclusion is valid in the frequency range where time‐lags have been detected with sufficient significance. In fact, the data hint that the reflected component is working in the opposite direction, reducing the lags at energies where the contribution of the reflected component is significant. We argue that the observed logarithmic dependence of time‐lags on energy could be due to the small variations of the spectral index in the frame of a very simple phenomenological model. We assume that an optically thin flow/corona, emitting a power law like spectrum, is present at a range of distances from the compact object. The slope of the locally emitted spectrum is a function of distance, with the hardest spectrum emitted in the innermost region. If perturbations with different time‐scales are introduced to the accretion flow at different radii, then X‐ray lags naturally appear, caused by the inward propagation of perturbations on the diffusion time‐scales.