Open AccessX‐ray spectral evolution of Her X‐1 in a low state and the following short high state
Author(s) -
İnam Sıtkı Cağdaş,
Baykal Altan
Publication year - 2005
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 - 10.1111/j.1365-2966.2005.09272.x
Subject(s) - physics , astrophysics , flux (metallurgy) , spectral line , opacity , eclipse , line (geometry) , absorption (acoustics) , proportional counter , state (computer science) , emission spectrum , x ray , atomic physics , astronomy , optics , detector , mathematics , materials science , geometry , algorithm , computer science , metallurgy
We analysed spectral variations of ∼8.5‐d long Rossi X‐ray Timing Explorer ( RXTE ) monitoring observations of Her X‐1 in 2001 December. This set of observations enables, for the first time, frequent continuous monitoring (111 pointings in ∼8.5 d) of the source with RXTE including a ∼1.7‐d‐long low state part and the following ∼6.8‐d‐long short high state part. We used an absorbed power‐law model with an iron line energy complex modelled as a Gaussian to fit both the 3–60 keV Proportional Counter Array–High Energy X‐ray Timing Experiment (PCA–HEXTE) overall short high state spectrum and 3–20 keV individual PCA spectra. An additional partial cold absorber model was used for both cases. Using 3–20 keV individual PCA spectra, absorption in anomalous dips (ADs) and pre‐eclipse dips (PDs) in the short high state was compared. Decreasing the ratio of unabsorbed to absorbed flux with increasing unabsorbed flux in ADs and PDs was interpreted as evidence of the fact that the regions causing opaque obscuration and soft absorption are not geometrically far away from each other. Higher iron line peak energies in the low state and the short high state (∼6.6–6.9 keV) were interpreted as a clue of the presence of iron line components other than the Kα emission line.