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We propose a helium nova model for the Large Magellanic Cloud (LMC) supersoftX-ray source (SSS) [HP99]159. This object has long been detected as a faint andpersistent SSS for about 30 years, and recently been interpreted to be a sourceof steady helium-shell burning, because no hydrogen lines are observed. We findthat the object can also be interpreted as in a decaying phase of a heliumnova. The helium nova is slowly decaying toward the quiescent phase, duringwhich the observed temperature, luminosity, and SSS lifetime ($\gtrsim 30$years) are consistent with a massive white dwarf model of $\sim$ 1.2 $M_\odot$.If it is the case, this is the second discovery of a helium nova outburst afterV445 Pup in our Galaxy and also the first identified helium nova in the LMC. Wealso discuss the nature of the companion helium star in relation to Type Iasupernova progenitors.

A helium nova in the Large Magellanic Cloud -- the faint supersoft X-ray source [HP99]159