SIMBAD references

The development of a nova eruption is well known to be determined by the white dwarf (WD) mass and the rate at which it accretes mass from its donor. One of the advancements in this field is the understanding that the occurrence of a nova eruption depends on the presence of heavy elements in the envelope, and that the concentration of these elements is highly dependent on the time allotted for accretion. This results in many features of the eruption being correlated with the mass fractions of heavy elements in the ejected material, however, the accreted material is always assumed to be of solar metallicity. Here, we explored the entire range of accretion rates on to a 1.25 M_☉ WD for two cases of highly enriched accreted material and find enrichment to have an influence on certain features for high accretion rates, while the effect of enrichment on low accretion rates is negligible. We further find that the ignition of the thermonuclear runaway which is known to be dependent on the accumulation of a critical mass, is actually dependent on the accumulation of a critical amount of heavy elements.