In the later stages of stellar evolution, a star (if massive enough) will begin fusing carbon nuclei

Question:

In the later stages of stellar evolution, a star (if massive enough) will begin fusing carbon nuclei to form, for example, magnesium;

(a) How much energy is released in this reaction (see Appendix B).
(b) How much kinetic energy must each carbon nucleus have (assume equal) in a head-on collision if they are just to touch (use Eq. 30-1) so that the strong force can come into play?
(c) What temperature does this kinetic energy correspond to?