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We present photometric and spectroscopic observations of a peculiar variable(designated DASCH J075731.1+201735 or J0757) discovered from our DASCH projectusing the digitized Harvard College Observatory archival photographic plates.It brightened by about 1.5 magnitudes in B within a year starting in 1942, andthen slowly faded back to its pre-outburst brightness from 1943 to the 1950s.The mean brightness level was stable before and after the outburst, andellipsoidal variations with a period of $P=119.18\pm0.07$ days are seen,suggesting that the star is tidally distorted. Radial-velocity measurementsindicate that the orbit is nearly circular ($e=0.02\pm0.01$) with aspectroscopic period that is the same as the photometric period. The binaryconsists of a $1.1\pm0.3 M_\odot$ M0III star, and a $0.6\pm0.2 M_\odot$companion, very likely a white dwarf (WD). Unlike other symbiotic binaries,there is no sign of emission lines or a stellar wind in the spectra. With anoutburst timescale of ~10 years and estimated B band peak luminosity M_B~0.7,J0757 is different from any other known classic or symbiotic novae. The mostprobable explanation of the outburst is Hydrogen shell-burning on the WD,although an accretion-powered flare cannot be ruled out.

DASCH Discovery of A Possible Nova-like Outburst in A Peculiar Symbiotic Binary