<P> Causes of the dramatic appearance of a nova vary, depending on the circumstances of the two progenitor stars . All observed novae involve closely located binary stars (the progenitors), either a pair of red dwarfs in the process of merging, or a white dwarf and another star . </P> <P> The main sub-classes of novae are classical novae, recurrent novae (RNe), and dwarf novae . They are all considered to be cataclysmic variable stars . Luminous red novae share the name and are also cataclysmic variables, but are a different type of event caused by a stellar merger . Also with similar names are the much more energetic supernovae (SNe) and kilonovae . </P> <P> Classical nova eruptions are the most common type of nova . They are likely created in a close binary star system consisting of a white dwarf and either a main sequence, sub-giant, or red giant star . When the orbital period falls in the range of several days to one day, the white dwarf is close enough to its companion star to start drawing accreted matter onto the surface of the white dwarf, which creates a dense but shallow atmosphere . This atmosphere is mostly hydrogen and is thermally heated by the hot white dwarf, which eventually reaches a critical temperature causing rapid runaway ignition by fusion . </P> <P> From the dramatic and sudden energies created, the now hydrogen - burnt atmosphere is then dramatically expelled into interstellar space, and its brightened envelope is seen as the visible light created from the nova event, and previously was mistaken as a "new" star . A few novae produce short - lived nova remnants, lasting for perhaps several centuries . Recurrent nova processes are the same as the classical nova, except that the fusion ignition may be repetitive because the companion star can again feed the dense atmosphere of the white dwarf . </P>

Where does the hydrogen fuel come from to cause a white dwarf to nova or supernova