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They are powered by thermonuclear runaways (TNR) in their WD's hydrogen-rich envelopes Starrfield et al. After ejecting their erupting envelopes, novae self-extinguish (Prialnik, Shara & Shaviv 1978).Early nova simulations exclusively dealt with the WD, and most of them only with the accretion phase, up to the TNR.
Our code is not designed to follow the entire evolution of a WD and to simulate it experiencing an SN explosion.In this study, we allowed a WD with a near Chandrasekhar mass of 1.4 M to evolve over tens of thousands of nova cycles, accumulating mass secularly while undergoing periodic nova eruptions.We present the mass accretion limits within which an SNIa can possibly occur.It has long been argued that steady burning cannot arise in WDs accreting hydrogen-rich material, and both this paper and recent works have confirmed this conclusion, e.g. We focus on the results for an initial core temperature of 3 × 10 K showed a slightly longer cycle duration (in both cases, about a 5 per cent difference compared with the corresponding baseline model).The shorter and longer cycle durations affected the accreted and ejected mass accordingly; however, the net mass gain was essentially the same for the three temperatures.In Section 3, we present the results of long-term evolutionary calculations.
In Section 4, we discuss the limits and limitations of these simulations and present three super-soft X-ray sources that display many of the characteristics of the models of Section 3. Throughout the calculations, we use a hydrodynamic Lagrangian code, designed to evolve a WD through multiple consecutive nova cycles Prialnik & Kovetz (1995).
To test this hypothesis, we have attempted to ‘push’ a sub-Chandrasekhar mass WD, in a semi-detached binary system, over the mass required to initiate an SNIa.
We test a range of accretion rates that lead to net mass accumulation on the surface of the WD, through a long series of nova cycles.
In order to result in an SNIa explosion, a WD must reach the Chandrasekhar limit (Chandrasekhar 1931).
We must numerically follow many consecutive nova cycles while the WD secularly accumulates mass.
To allow for a continually growing WD, while keeping the numerical grid no larger in size than necessary for accurate and reproducible calculations (Epelstain et al.