A star initially has `10^40` deuterons. It produces energy via the processes `_1^2H+_1^2Hrarr_1^3H+p` and `_1^2H+_1^3Hrarr_2^4He+n`. Where the masses of the nuclei are
`m(`^2H)=2.014` amu, `m(p)=1.007` amu, `m(n)=1.008` amu and `m(`^4He)=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 10^40 deuterons. It produces energy via the processes _1H^2+_1H^2rarr_1H^3+p _1H^2+_1H^3rarr_2He^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(He^4)=4.001 amu if the average power radiated by the star is 10^16W , the deuteron supply of the star is exhausted in a time of the order of

A star initially has 10^(40) deuterons it product energy via the process _(1)H^(2) + _(1)H^(2) + rarr _(1) H^(3) + p. and _(1)H^(2) + _(1)H^(3) + rarr _(2) He^(4) + n If the deuteron supply of the average power radiated by the state is 10^(16) W , the deuteron supply of the state is exhausted in a time of the order of . 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(He^(4)) = 4.001 amu.

A star initially has 10^40 deuterons. It produces energy via the processes _1H^2+ _1H^2rarr_1H^3+p and _1H^2+_1H^3rarr_2He^4+n . 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) 10^6s (b) 10^8s (c) 10^12s The masses of the nuclei are as follows M(H^2)=2.014 amu, M(n)=1.008 amu, M(p)=1.007 amu, M(He^4)=4.001 amu

A star initially has 10^40 deuterons. It produces energy via the processes _1H^2+_1H^2rarr_1H^3+p and _1H^2+_1H^3rarr_2He^4+n . 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) 10^6s (b) 10^8s (c) 10^12s The masses of the nuclei are as follows M(H^2)=2.014 amu, M(n)=1.008 amu, M(p)=1.007 amu, M(He^4)=4.001 amu

A star initially has 10^(40) deuterons. It produces energy via the process _(1)H^(2) + _(1)H^(2) + rarr _(1) H^(3) + p. and _(1)H^(2) + _(1)H^(3) + rarr _(2) He^(4) + n .If the average power radiated by the state is 10^(16) W , the deuteron supply of the star is exhausted in a time of the order of . 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(He^(4)) = 4.001 amu .

The source of energy of stars is nuclear fusion. Fusion reaction occurs at very high temperature, about 10^(7) . Energy released in the process of fusion is due to mass defect. It is also called Q -value. Q = Delta mc^(2), Delta m = mass defect. A star has 10^(40) deutrons. It produes via the process ._(1)H^(2) + ._(1)H^(2) rarr ._(1)He^(3) + ._(1)H^(1) ._(1)H^(3) + ._(1)H^(3) rarr ._(2)He^(4) + ._(0)n^(1) If the average power radiated by the star is 10^(16) W , when the deutron supply of the star is exhausted in a time of the order of

Calculate the binding energy of alpha - particle. Given m_p = 1.007825 amuo, m_n 1.008665 amu, m(_2^4He) = 4.002800 amu].

Calculate the Q-values of the following fusion reactions: (a) _1^2H+ _1^2H rarr _1^3H+ _1^1H . _1^2H+ _1^2H rarr _2^3(He)+n _1^2H+ _1^3H rarr _2^4(He)+n . Atomic masses are m( _1^2H)=2.014102 u, m( _1^3H)=3.016049 u, m( _2^3(He))=3.016029 u, m( _2^4(He))=4.002603 u.