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Accreting neutron stars exhibit Type I X-ray bursts from both frequenthydrogen/helium flashes as well as rare carbon flashes. The latter(superbursts) ignite in the ashes of the former. Hydrogen/helium bursts,however, are thought to produce insufficient carbon to power superbursts.Stable burning could create the required carbon, but this was predicted to onlyoccur at much larger accretion rates than where superbursts are observed. Wepresent models of a new steady-state regime of stable hydrogen and heliumburning that produces pure carbon ashes. Hot CNO burning of hydrogen heats theneutron star envelope and causes helium to burn before the conditions of ahelium flash are reached. This takes place when the mass accretion rate isaround 10% of the Eddington limit: close to the rate where most superburstsoccur. We find that increased heating at the base of the envelope sustainssteady-state burning by steepening the temperature profile, which increases theamount of helium that burns before a runaway can ensue.

Carbon production on accreting neutron stars in a new regime of stable nuclear burning