Two Types of Soft X-ray Spectra in Cataclysmic Variables

Details Two Types of Soft X-ray Spectra in Cataclysmic Variables Two Types of Soft X-ray Spectra in Cataclysmic Variables

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...20112004m&link_type=abstract

American Astronomical Society, 201st AAS Meeting, #120.04; Bulletin of the American Astronomical Society, Vol. 34, p.1302

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In cataclysmic variables (CVs), accretion onto white dwarfs produces high temperature, high density plasmas, which cool down from kT ~10 keV principally via bremsstrahlung continuum and K and L shell line emissions. In ROSAT and ASCA spectra, some CVs show little sign of Fe L emission lines, even though the cooling of kT ~1 keV plasma should be dominated by these lines. Here we compare the Chandra HETG spectra of all 7 CVs that were observed using HETG by 2002 March. One group of systems, consisting of EX Hya, SS Cyg, U Gem and V603 Aql, all have a similar spectrum. We demonstrate that the cooling flow model can successfully describe the detailed emission line spectra. The spectra of V1223 Sgr, AO Psc, and GK Per, are similar to each other, and cannot be described by as cooling flows. Instead, they resemble the spectra of Seyfert 2 galaxies, showing weak Fe L lines compared to K lines of medium Z elements. We show that photoionization models can reproduce the line spectra of these three CVs.

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