The Origin of Soft X-rays in Dq Herculis

DQ Herculis (Nova Herculis 1934) is a deeply eclipsing cataclysmic variable containing a magnetic white dwarf primary. The accretion disk is thought to block our line of sight to the white dwarf at all orbital phases because of its extreme inclination angle. Nevertheless, soft X-rays were detected from DQ Her with the ROSAT PSPC. To probe the origin of these soft X-rays, we have performedChandraACIS observations. We confirm that DQ Her is an X-ray source. The bulk of the X-rays are from a pointlike source and exhibit a shallow partial eclipse. We interpret this as being due to scattering of the unseen central X-ray source, probably in an accretion disk wind. At the same time, we observe what appear to be weak extended X-ray features aroundDQHer, which we interpret as an X-ray–emitting knot in the nova shell. Subject headings: binaries: eclipsing — novae, cataclysmic variables — stars: individual (DQHerculis) — X-rays: stars