SIMBAD references

Nuclear burning near the surface of an accreting neutron star produces ashes that, when compressed deeper by further accretion, alter the star's thermal and compositional structure. Bygone nucleosynthesis can be constrained by the impact of compressed ashes on the thermal relaxation of quiescent neutron star transients. In particular, Urca cooling nuclei pairs in nuclear burning ashes that cool the neutron star crust via neutrino emission from e^–-capture/β^–-decay cycles and provide signatures of prior nuclear burning over the ∼century timescales it takes to accrete to the e^–-capture depth of the strongest cooling pairs. Using crust cooling models of the accreting neutron star transient MAXI J0556-332, we show that this source likely lacked Type I X-ray bursts and superbursts >=120 years ago. Reduced nuclear physics uncertainties in rp-process reaction rates and e^–-capture weak transition strengths for low-lying transitions will improve nucleosynthesis constraints using this technique.