Time Variation of X-Rays from GX 5--1

Details Time Variation of X-Rays from GX 5--1 Time Variation of X-Rays from GX 5--1

Oct 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997pasj...49..589k&link_type=abstract

Publications of the Astronomical Society of Japan, v.49, p.589-605.

Astronomy and Astrophysics

Astronomy

3

Stars: Neutron, Time Variations, X-Rays: Binaries, X-Rays: Sources

Scientific paper

Long- and short-term variations of X-rays from GX 5-1 (a neutron-star X-ray binary) were investigated based on the Eastern energy spectral model: a disk-blackbody component plus a blackbody component model. In the horizontal branch (HB), an increase in the X-ray intensity is mainly due to the disk component; this increase is mainly due to an increase in R_in (the inner radius of the accretion disk), although T_in (the temperature of the inner edge of the accretion disk) decreases slightly. A fraction of the blackbody component decreases with the X-ray intensity in HB. In the normal branch (NB), an increase in the X-ray intensity is due to both components. The hardening of the X-ray energy spectrum with the X-ray intensity in NB is mainly due to an increase in the blackbody component: the fraction of the blackbody component increases with the X-ray intensity. The X-ray intensities of the disk component and the blackbody component show different long-term variations from each other, which are similar to the case of the disk component and the power-law component of black-hole candidate X-ray binaries (BHCXBs); GX 339-4 and GS 1124-683. It is possible that the behavior of the Z source from HB to NB is due to hysteretic behavior, such as that shown by the BHCXBs. Short-term variations of X-rays from GX 5-1 were investigated using normalized power spectral density functions (NPSDs), and were compared with those of a BHCXB, GS 1124-683. NPSD of the disk component has a power-law shape, and has an energy dependence: the higher is the X-ray energy, the larger is the variation. NPSD of the blackbody component has a flat-top shape, and has no energy dependence. These are the same as that of the disk component and the power-law energy spectral component of GS 1124-683, in spite of their different energy spectra and different category of X-ray stars. The very-low-frequency noise (VLFN) of GX 5-1 has minimum values in the transition part between HB and NB, where the total X-ray intensity has its maximum value. VLFN seems to be related to a variation of the mass-accretion rate.

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