The thermonuclear process in solar and less massive stars which produces one atom of helium from four of hydrogen is the?
The thermonuclear process in solar and less massive stars that produces one atom of helium from four atoms of hydrogen is called nuclear fusion. More specifically, this particular fusion process is known as the proton-proton chain reaction.
To understand how this fusion process occurs, we need to consider the conditions inside a star. Due to the high temperature and pressure at the core of a star, hydrogen atoms (protons) are moving with high energy. In order for fusion to occur, two protons must come close enough together for the strong nuclear force to overcome the electrostatic repulsion between them.
Here's a step-by-step explanation of the proton-proton chain reaction:
1. Step 1: Two protons (hydrogen nuclei) come close enough for one of them to undergo a quantum-mechanical process called quantum tunneling. This process allows one proton to convert into a neutron through the weak nuclear force, releasing a positron (a positively charged electron) and a neutrino.
2. Step 2: The newly formed deuterium (a nucleus consisting of one proton and one neutron) combines with another proton to form the nucleus of helium-3, also known as a lone Helium-3 atom.
3. Step 3: Two helium-3 nuclei collide, and a process known as the Helium-3 cycle takes place. Two protons are then kicked out, leaving behind a helium-4 nucleus (two protons and two neutrons). This process also releases two extra protons, which can go on to partake in further fusion reactions.
Overall, the proton-proton chain reaction converts four protons (hydrogen nuclei) into one helium-4 nucleus, releasing a tremendous amount of energy in the form of gamma rays. This energy is what powers our Sun and other less massive stars, enabling them to emit light, heat, and other forms of electromagnetic radiation.