In this paper temperature enhanced α-decay at high stellar temperatures is investigated in conjunction withs-process nucleosynthesis. The temperature dependence of α-decay is the result of more energetic, hence faster, decay from thermally excited nuclear states. A formula for the effective halflife is derived as a function of the atomic number and weight, temperature, and the α-decayQ-value of the isotope. The effect of such enhanced α-decay upons-process abundances is discussed, and information abouts-process neutron flux intensities is deduced based on the calculated α-decay halflives of the isotopes Nd 144 and Sm 150. The neutron flux-temperature relationships are compared to specific constant temperature carbon-burning models of massive stars which are considered to be possible sources of solar systems-process abundances. Finally, information regarding the time betweens-process termination and final interstellar injection ofs-process material is derived using the decay calculations.