The Sun radiates energy at the rate of 3.85 ×10^26 W . Suppose the net reaction 4(1 H)+2(-1^0 e)

step 1 Everyone, this is the problem based on energy radiation by the sun. As we know that, sun is radi

The Sun radiates energy at the rate of 3.85 ×10^26 W ....

The Sun radiates energy at the rate of $3.85 \times 10^{26} \mathrm{W} .$ Suppose the net reaction $$ 4(1 \mathrm{H})+2\left(-_{1}^{0} \mathrm{e}\right) \rightarrow_{2}^{4} \mathrm{He}+2 \nu+\gamma $$ accounts for all the energy released. Calculate the number of protons fused per second.

The Sun radiates energy at the rate of $3.85 \times 10^{26} \mathrm{W} .$ Suppose the net reaction
$$
4(1 \mathrm{H})+2\left(-_{1}^{0} \mathrm{e}\right) \rightarrow_{2}^{4} \mathrm{He}+2 \nu+\gamma
$$
accounts for all the energy released. Calculate the number of protons fused per second.

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Key Concepts

Proton-Proton Chain

The proton-proton chain is the dominant fusion reaction in stars like the Sun. It involves a series of steps in which protons are fused into helium nuclei, emitting energy in the form of gamma rays, neutrinos, and positrons, thereby sustaining the star's radiative energy output.

Stellar Luminosity

Stellar luminosity is the total energy output per unit time a star emits in the form of electromagnetic radiation. It is a critical concept in astrophysics because it quantifies the power generated by the processes occurring in the star’s core and governs the energy available for influencing the star’s immediate environment.

Nuclear Fusion

Nuclear fusion is the process by which atomic nuclei combine to form a heavier nucleus, releasing energy as a result of the mass difference between the reactants and the products. This process is the fundamental energy source in stars, where hydrogen nuclei fuse to form helium through a series of reactions.

Mass-Energy Equivalence

Mass-energy equivalence, expressed by Einstein’s equation E=mc², describes how mass can be converted into energy. In stellar fusion, a small loss of mass results in the release of a large amount of energy, which explains the prodigious energy output observed in stars.

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