The overall hydrogen burning reaction in stars can be represented as the conversion of four protons to one alpha particle. Use the data for the mass of H-1 and He-4 to calculate the energy released by this process.

Verified step by step guidance

1. Identify the reactants and products in the reaction: 4 protons (H-1) are converted into 1 alpha particle (He-4).
2. Determine the mass of the reactants: Calculate the total mass of 4 protons using the given mass of H-1.
3. Determine the mass of the product: Use the given mass of He-4 to find the mass of the alpha particle.
4. Calculate the mass defect: Subtract the mass of the product (He-4) from the total mass of the reactants (4 protons).
5. Use Einstein's equation, \( E = \Delta m c^2 \), to calculate the energy released, where \( \Delta m \) is the mass defect and \( c \) is the speed of light.

Key Concepts

Nuclear Fusion

Nuclear fusion is the process by which two light atomic nuclei combine to form a heavier nucleus, releasing energy in the process. In stars, hydrogen nuclei (protons) fuse to form helium, specifically an alpha particle, which is a helium-4 nucleus. This reaction is fundamental to stellar energy production and is responsible for the immense energy output of stars.

Mass-Energy Equivalence

Mass-energy equivalence, encapsulated in Einstein's equation E=mc², states that mass can be converted into energy and vice versa. In the context of nuclear fusion, the mass of the resulting helium nucleus is less than the total mass of the original hydrogen nuclei. This 'missing' mass is converted into energy, which can be calculated to determine the energy released during the fusion process.

Binding Energy

Binding energy is the energy required to disassemble a nucleus into its constituent protons and neutrons. It is also the energy released when a nucleus is formed from these particles. In fusion reactions, the binding energy per nucleon increases as lighter nuclei combine to form a heavier nucleus, resulting in a net release of energy, which is a key factor in understanding the energy output of stars.