An Apparent Hard X-ray Decline of CH Cygni

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 K-alpha line, we show that the hard X-rays observed with Suzaku are dominated by scattering.

arXiv comment8 pages, 4 figures, accepted by Publications of the Astronomical Society of Japan

References in corpus (7)

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• In-Orbit Performance of the Hard X-ray Detector on board Suzaku
• An X-Ray Jet from a White Dwarf - Detection of the Collimated Outflow from CH Cygni with Chandra
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• ChaMPlane Discovery of Candidate Symbiotic Binaries in Baade's and Stanek's Windows
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• The Nature of the Hard-X-Ray Emitting Symbiotic Star RT Cru
• CH Cyg X-ray Jet Activity and Multi-component Structures
• Suzaku and NuSTAR X-Ray Spectroscopy of gamma Cas and HD110432
• A Precessing Jet in the CH Cyg Symbiotic System
• The Symbiotic System SS73 17 Seen with Suzaku
• Detection of X-rays from the jet-driving Symbiotic Star MWC 560
• Symbiotic stars in X-rays III: Suzaku observations
• Peering into the central region of a nano-quasar: XMM-Newton and Chandra views of the CH Cyg Symbiotic System
• Hydrodynamical simulations of the jet in the symbiotic star MWC 560 III. Application to X-ray jets in symbiotic stars
• Spectroscopy of the symbiotic star CH Cygni from 1996 to 2007
• Detection of X-rays from the symbiotic star V1329 Cyg
• Detection of X-rays from the jet-driving symbiotic star Hen 3-1341
• An XMM-Newton view of the Symbiotic Stars HM Sge, NQ Gem, and PU Vul
• X-ray Variability in the Symbiotic Binary RT Cru: Principal Component Analysis
• The symbiotic star CH Cygni. I. An analysis of the shocked nebulae at different epochs
• New Clues to the Evolution of Dwarf Carbon Stars From Their Variability and X-ray Emission
• Broad Observational Perspectives Achieved by the Accreting White Dwarf Sciences in the XMM-Newton and Chandra Eras