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We revisit hydrogen shell burning on white dwarfs (WDs) with higher massaccretion rates than the stability limit, \dot M_stable, above which hydrogenburning is stable. Novae occur with mass accretion rates below the limit. Foran accretion rate > \dot M_stable, a first hydrogen shell flash occurs followedby steady nuclear burning, so the shell burning will not be quenched as long asthe WD continuously accretes matter. On the basis of this picture, somepersistent supersoft X-ray sources can be explained by binary models with highaccretion rates. In some recent studies, however, the claim has been made thatno steady hydrogen shell burning exists even for accretion rates > \dot M_{\rmstable}. We demonstrate that, in such cases, repetitive flashes occurredbecause mass accretion was artificially controlled. If we stop mass accretionduring the outburst, no new nuclear fuel is supplied, so the shell burning willeventually stop. If we resume mass accretion after some time, the next outbursteventually occurs. In this way, we can design the duration of outburst andinterpulse time with manipulated mass accretion. We call such a controlled novaa "forced nova." These forced novae, if they exist, could have much shorterrecurrence periods than "natural novae." We have obtained the shortestrecurrence periods for forced novae for various WD masses. Based on theresults, we revisit WD masses of some recurrent novae including T Pyx.

Shortest Recurrence Periods of Forced Novae