The Be9(α, n)C12 reaction has been studied at Ēα=5.6 and 5.78 Mev. Neutron groups have been observed to the first three states of C12. The ratio of the population of the 4.43- and 7.66- Mev states has been determined to be 8.1+/-1 at Ēα=5.6 Mev. This value, together with information from a number of other sources, demonstrates that the 7.66-Mev state has Jπ=0+, that its width for alpha emission is approximately the Wigner limit (Γ~8 ev) and that in ~10-3% of the cases the state decays to the ground state of C12 by pair emission. It is also estimated that the 7.66-Mev state can decay by γ emission via the 2+, 4.43-Mev state with a probability of 15000. This information reinforces the proposal that the 7.66-Mev state has the necessary properties to participate in the buildup of the elements in red giant stars.