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V445 Pup (2000) is a unique object identified as a helium nova. Color indexesduring the outburst are consistent with those of free-free emission. We presenta free-free emission dominated light curve model of V445 Pup on the basis ofthe optically thick wind theory. Our light curve fitting shows that (1) thewhite dwarf (WD) mass is very massive (M_WD \gtrsim 1.35 M_\sun), and (2) ahalf of the accreted matter remains on the WD, both of which suggest that theincreasing WD mass. Therefore, V445 Pup is a strong candidate of Type Iasupernova progenitor. The estimated distance to V445 Pup is now consistent withthe recent observational suggestions, 3.5 < d < 6.5 kpc. A helium starcompanion is consistent with the brightness of m_v=14.5 mag just before theoutburst, if it is a little bit evolved hot (\log T (K) \gtrsim 4.5) star withthe mass of M_He \gtrsim 0.8 M_\sun. We then emphasize importance ofobservations in the near future quiescent phase after the thick circumstellardust dissipates away, especially its color and magnitude to specify the natureof the companion star. We have also calculated helium ignition masses forhelium shell flashes against various helium accretion rates and discussed therecurrence period of helium novae.

Helium Nova on a Very Massive White Dwarf -- A Light Curve Model of V445 Puppis (2000) Revised