X-ray spectrum of Hercules X-1 in the low state of the 35-day cycle

Details X-ray spectrum of Hercules X-1 in the low state of the 35-day cycle X-ray spectrum of Hercules X-1 in the low state of the 35-day cycle

Jun 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pasj...43..501m&link_type=abstract

Astronomical Society of Japan, Publications (ISSN 0004-6264), vol. 43, no. 3, 1991, p. 501-521.

Astronomy and Astrophysics

Astronomy

41

Accretion Disks, Hercules Nova, Line Spectra, X Ray Sources, X Ray Spectra, Light Curve, Metallicity, Power Spectra, Stellar Spectrophotometry

Scientific paper

A high-quality spectrum of Her X-1 in the low-state of the 35-d cycle, obtained in 1988 with Ginga, is presented. The observed X-ray flux is 4.2 x 10 exp -10 erg/sq cm s in energy range 2-37 keV, about 5 percent of the flux in the main-on state. A 3-Sigma upper limit for the amplitude of the 1.24 s sinusoidal pulse is 2.4 percent of the average low-state flux. The iron line shows a center energy of 6.53 +/- 0.08 keV, an intrinsic FWHM of 0.8 +/- 0.4 keV, and an equivalent width of 1.0 +/- 0.1 keV, respectively. A comparison of the low-state spectrum with the main-on and the dip data reveals two spectral components: a 'scattered' component, showing the same spectral shape with the main-on emission, and an'absorbed' component. The accretion disk corona (at a distance of r less than 5 x 10 exp 11 cm) and the outer edge (r greater than 2 x 10 exp 11 cm) of the disk are the likely origins for each component. The broad width of the iron line suggests contributions of fluorescent X-rays from both the outer edge region of the disk and the hot scattering region.

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