Editing Helium flash (section)

==Binary white dwarfs==

When hydrogen gas is accreted onto a ''white dwarf'' from a binary companion star, the hydrogen can fuse to form helium for a narrow range of accretion rates, but most systems develop a layer of hydrogen over the degenerate white dwarf interior. This hydrogen can build up to form a shell near the surface of the star. When the mass of hydrogen becomes sufficiently large, runaway fusion causes a [[nova]]. In a few binary systems where the hydrogen fuses on the surface, the mass of helium built up can burn in an unstable helium flash. In certain binary systems the companion star may have lost most of its hydrogen and donate helium-rich material to the compact star. Note that [[X-ray burster|similar flashes]] occur on neutron stars.{{citation needed|date=February 2016}}