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Some binary evolution scenarios to Type Ia supernovae include long-periodbinaries that evolve to symbiotic supersoft X-ray sources in their late stageof evolution. However, symbiotic stars with steady hydrogen burning on thewhite dwarf's (WD) surface are very rare, and the X-ray characteristics are notwell known. SMC3 is one such rare example and a key object for understandingthe evolution of symbiotic stars to Type Ia supernovae. SMC3 is an eclipsingsymbiotic binary, consisting of a massive WD and red giant (RG), with anorbital period of 4.5 years in the Small Magellanic Cloud. The long-term Vlight curve variations are reproduced as orbital variations in the irradiatedRG, whose atmosphere fills its Roche lobe, thus supporting the idea that the RGsupplies matter to the WD at rates high enough to maintain steady hydrogenburning on the WD. We also present an eclipse model in which an X-ray emittingregion around the WD is almost totally occulted by the RG swelling over theRoche lobe on the trailing side, although it is always partly obscured by along spiral tail of neutral hydrogen surrounding the binary in the orbitalplane.

An X-Ray and Optical Light Curv Model of the Eclipsing Symbiotic Binary SMC3