Abstract
CH Cygni is a symbiotic star consisting of an M giant and an accreting white dwarf, which is known to be a highly variable X-ray source with a complex, two-component, spectra. Here, we report on two Suzaku observations of CH Cyg, taken in 2006 January and May, during which the system was seen to be in a soft X-ray bright, hard X-ray faint state. Based on the extraordinary strength of the 6.4 keV fluorescent Fe Kα line, we show that the hard X-rays observed with Suzaku are dominated by scattering. accretion, accretion disk - stars: binaries: symbiotic - stars: individual (CH Cyg) - X-rays: stars © 2007. Astronomical Society of Japan.
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CITATION STYLE
Mukai, K., Ishida, M., Kilbourne, C., Mori, H., Terada, Y., Chan, K. W., & Soong, Y. (2007). An apparent hard X-ray decline of CH cygni. Publications of the Astronomical Society of Japan, 59(1 SPEC. ISS.). https://doi.org/10.1093/pasj/59.sp1.s177
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