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A star initially has 1040 deuterons. It produces energy via the processes 1 H² +₁H² →→ ₁H³ + p and ₁ + p and, H²+₁H³ →→ ₂He¹ + n. If the average power radiated by the star is 10¹6 W, the deuteron supply of the star is exhausted in a time of the order of (a) 106 s (c) 10¹² s (b) 108 s (d) 10¹6 S The mass of the nuclei are as follows M(H²) = 2.014 amu; M(n) = 1.008 amu; M(p) = 1.007 amu; M(He4 ) = 4.001 amu.

A star initially has 1040 deuterons. It produces energy via the processes 1 H² +₁H² →→ ₁H³ + p and ₁ + p and, H²+₁H³ →→ ₂He¹ + n. If the average power radiated by the star is 10¹6 W, the deuteron supply of the star is exhausted in a time of the order of (a) 106 s (c) 10¹² s (b) 108 s (d) 10¹6 S The mass of the nuclei are as follows M(H²) = 2.014 amu; M(n) = 1.008 amu; M(p) = 1.007 amu; M(He4 ) = 4.001 amu.

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15. A star initially has 1040 deuterons. It produces energy via the 3 4 processes, H² +₁H² →→ ₁H³ + p and, H² + ₁H³ → ₂Heª + n. 1 the If the average power radiated by the star is 10¹6 W, deuteron supply of the star is exhausted in a time of the order of (a) 106 S (c) 10 ¹² s (b) 108 s (d) 10¹6 s The mass of the nuclei are as follows M(H²) = 2.014 amu; M(n) = 1.008 amu; M(p) = 1.007 amu; M(He* )= 4.001 amu. 4
Transcribed Image Text:15. A star initially has 1040 deuterons. It produces energy via the 3 4 processes, H² +₁H² →→ ₁H³ + p and, H² + ₁H³ → ₂Heª + n. 1 the If the average power radiated by the star is 10¹6 W, deuteron supply of the star is exhausted in a time of the order of (a) 106 S (c) 10 ¹² s (b) 108 s (d) 10¹6 s The mass of the nuclei are as follows M(H²) = 2.014 amu; M(n) = 1.008 amu; M(p) = 1.007 amu; M(He* )= 4.001 amu. 4
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