The hot and cool component of the symbiotic nova SMC 3. A supersoft X-ray variable and a small-amplitude red variable

Astronomy and Astrophysics – Astrophysics

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Galaxies: Magellanic Clouds, Stars: Binaries: Symbiotic, Stars: Individual: Rx J0048.4-7332 (=Smc 3), Stars: Mass-Loss, X-Rays: Stars

Scientific paper

The ˜6 year supersoft X-ray lightcurve of the symbiotic nova SMC 3 (=RX J0048.4-7332) in the Small Magellanic Cloud is derived from archival ROSAT PSPC and HRI data. It shows one deep X-ray eclipse during which the count rate decreased by a factor of ≈gt80. In MACHO B-band data sinusoidal variation is found with a quasi-periodicity of ˜4 years. The minimum of the B-band flux occurs during the X-ray eclipse. In OGLE II I-band observations performed after the ROSAT observations we detect 110±2 day oscillations which we interpret as pulsations of the M0 giant star in the symbiotic system. The observed duration of the supersoft X-ray eclipse of ˜0.4-1.8 years is explained by the occultation of the white dwarf by the giant companion with an orbital period of ˜(4.0-4.8) years and a strong wind blown from its surface with a mass loss rate of ˜(2.6-8.2)× 10 -7 M&sun; yr-1, assuming that ˜(1-3.5)% of the ionized phase is neutral (e.g. due to dust) and assuming a terminal velocity of ˜30 km s-1. The ˜4 year quasi-periodicity found in the optical is explained as the binary orbital period of the system. It is less likely that it reflects the activity (or mass-loss) time scale of the red giant star. A ˜(700-800) day quasi-periodicity found in the OGLE II and MACHO data is explained as the first harmonic of a binary orbital cycle. SMC 3 therefore may be classified as a small-amplitude red variable star (SARV). The hot star most likely is in a state of steady nuclear burning with an accretion rate somewhat below the upper critical value of ˜10-7 M&sun; yr-1.
Based on archival data from the ROSAT, OGLE-II and MACHO project.

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