A star initially has 1040 deuterons. It produces energy via the processes \[_{1}{{H}^{2}}+{}_{1}{{H}^{2}}\to {}_{1}{{H}^{3}}+p\] \[_{1}{{H}^{2}}+{}_{1}{{H}^{3}}\to {}_{2}{{H}^{4}}+n\] The masses of the nuclei are as follows: \[M({{H}^{2}})\] = 2.014 amu; M (p) = 1.007 amu; \[M(n)\] = 1.008 amu; \[M(H{{e}^{4}})\] = 4.001 amu If the average power radiated by the star is \[{{10}^{16}}\]W, the deuteron supply of the star is exhausted in a time of the order of

A star initially has 1040 deuterons. It produces energy via the proces

1.	A star initially has 1040 deuterons. It produces energy via the processes \[_{1}{{H}^{2}}+{}_{1}{{H}^{2}}\to {}_{1}{{H}^{3}}+p\] \[_{1}{{H}^{2}}+{}_{1}{{H}^{3}}\to {}_{2}{{H}^{4}}+n\] The masses of the nuclei are as follows: \[M({{H}^{2}})\] = 2.014 amu; M (p) = 1.007 amu; \[M(n)\] = 1.008 amu; \[M(H{{e}^{4}})\] = 4.001 amu If the average power radiated by the star is \[{{10}^{16}}\]W, the deuteron supply of the star is exhausted in a time of the order of
A.	\[{{10}^{6}}\]
B.	\[{{10}^{8}}\sec \]
C.	\[{{10}^{12}}\sec \]
D.	\[{{10}^{16}}\sec \]
Answer» D. \[{{10}^{16}}\sec \]