ABSTRACT
The proposed mechanism involves binary systems with one degenerate objects, like white dwarfs or neutron stars and is characterized by the revival of the dormant objects via mass overflow and index accretionaccretion from the binary companion. Novae are associated with binary stellar systems and are often recurrent. A typical nova outburst occurs when a larger companion star accretes hydrogen-rich matter onto a smaller white dwarf companion. Novae are identified as white dwarfs in binary systems, accreting matter from the binary companion star in a burning stage close to main sequence H-burning which is filling its Roche Lobe. The accreted material forms a thin, but high density electron degenerate envelope at the surface of the white dwarf. The nuclear physics information required to understand this higher-temperature burning includes measurements of nuclear reactions on proton-rich unstable isotopes. These reaction rates still carry consider able uncertainties since they are mostly estimated on the basis of nuclear structure and nuclear level analysis.
