We have investigated the likelihood that the canonical p-nuclei (bypassed nuclei) may have been synthesized, at least in part, within degenerate hydrogen burning zones via low temperature photonuclear reactions triggered by photons released through proton capture by triply heavy hydrogen (/sup 3/T). For combinations of temperatures generally less than T/sub 6/=15, and densities greater than 10,000 g cm/sup -3/, the hydrogen burning cycle closes via the /sup 3/He(e/sup -/)/sup 3/T(p,..gamma..)/sup 4/Hebranch. The /sup 3/T(p,..gamma..)/sup 4/He photon is the most energetic (approx.20 MeV) known to be due to proton capture inside stars. This allows for the (..gamma..,n) and (..gamma..,2n) synthesis and destruction of the p-nuclei.We show that a likely astrophysical site for the photonuclear synthesis of the nuclei exists in white dwarfs accreting surface layers of hydrogen-rich material, eventually leading to nova outbursts as shown by Starrfield, Truran, and Sparks. In order to produce a nova outburst the accreting object must initially be of low luminosity, and this initial condition is sufficient for the ejection of processed matter into the interstellar medium. To determine the physical conditions within the degenerate hydrogen burning shell, we make use of the recent models by Sienkowicz which suggest, but do not conclusively demonstrate, that formore » the stationary shell approximation, the bypassed nuclei can be synthesized and the initial conditions established for the subsequent nova outburst.Under the conditions of degenerate hydrogen burning, we compute the abundances for several exposure periods, and find reasonable agreement with that for observed solar system p-nuclei, providing the solar s-nuclei distribution characterizes that for the seed nuclei. The strongest feature of the model is its ability to reproduce the isotopic abundance ratios of the double p-nuclei such as those for tin, xenon, barium, etc., and overabundances of heavy nuclei in the mass range 120< or =A< or =196.« less