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In our calculation of neutron star crust heating we include several key newmodel features. In earlier work electron capture (EC) only allowed neutronemission from the daughter ground-state; here we calculate, in a deformed QRPAmodel, EC decay rates to all states in the daughter that are allowed byGamow-Teller selection rules and energetics. The subsequent branching ratiosbetween the 1n,...,xn channels and the competing $\gamma$-decay are calculatedin a Hauser-Feshbach model. Since EC accesses excited states, many moreneutrons are emitted in our calculation than in previous work, leading toaccelerated reaction flows. In our multi-component plasma model a single(EC,xn) reaction step can produce several neutron-deficient nuclei, each ofwhich can further decay by (EC,xn). Hence, the neutron emission occurs morecontinuously with increasing depth as compared to that in a one-componentplasma model.

Neutron reactions in accreting neutron stars: a new pathway to efficient crust heating