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 .

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 _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 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 _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

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 mass loss in the following: ._(1)^(2)H + ._(1)^(3)H to ._(2)^(4)He + ._(0)^(1)n given the masses: ._(1)^(2)H = 2.014 amu, ._(1)^(3)H = 3.016 amu: ._(2)^(4)He = 4.004 amu, ._(0)^(1)n = 008 amu

Calculate the binding energy of the deuteron, which consistss of a proton and a neutron, given that the atomic mass of the deuteron is 2.014102 amu,. Take mass of proton (m_(p))=1.007825 amu, mass of a neutron (m_(n))=1.008665 amu and 1amu=931.5 MeV