出版社：SISSA, Scuola Internazionale Superiore di Studi Avanzati
摘要：Based on repeated RXTE observations of Her X-1 between 1996 and 2005, Staubert et al. (2007) had reported a positive correlation between the energy of the Cyclotron Resonance Scattering Feature (CRSF) and the maximum X-ray flux of the respective 35 d Main-On, as determined from the RXTE/ASM. This dependence is opposite to the negative correlation observed in bright, super Eddington transient pulsars. Here we address the question whether the ASM flux used in that work can really be taken as a measure of the bolometric luminosity of the source. We repeated the spectral analysis of the same 35 d cycles used in the original work by using data from both instruments (PCA and HEXTE) and re-determined the energy of the cyclotron line, as well as the 5–60 keV bolometric flux from those spectra. This flux is then scaled to represent the 35 d maximum flux. We confirm the result of the original analysis: the cyclotron line energy changes by 6...7% for a change in flux by a factor of two.
