logistic_guy
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In the later stages of stellar evolution, a star (if massive enough) will begin fusing carbon nuclei to form, for example, magnesium:
\(\displaystyle {}^{12}_{\ \ 6}\text{C} + {}^{12}_{\ \ 6}\text{C} \rightarrow {}^{24}_{12}\text{Mg} + \gamma\)
\(\displaystyle \bold{(a)}\) How much energy is released in this reaction? \(\displaystyle \bold{(b)}\) How much kinetic energy must each carbon nucleus have (assume equal) in a head-on collision if they are just to touch so that the strong force can come into play? \(\displaystyle \bold{(c)}\) What temperature does this kinetic energy correspond to?
\(\displaystyle {}^{12}_{\ \ 6}\text{C} + {}^{12}_{\ \ 6}\text{C} \rightarrow {}^{24}_{12}\text{Mg} + \gamma\)
\(\displaystyle \bold{(a)}\) How much energy is released in this reaction? \(\displaystyle \bold{(b)}\) How much kinetic energy must each carbon nucleus have (assume equal) in a head-on collision if they are just to touch so that the strong force can come into play? \(\displaystyle \bold{(c)}\) What temperature does this kinetic energy correspond to?