The electrons in the Sun, as well as in any ordinary matter, are primarily obtained through the formation and evolution of stars. The Sun consists mainly of hydrogen atoms, which are composed of a single proton and a single electron. The majority of the Sun's mass is in the form of protons within its core, where nuclear fusion reactions occur.
Stars like the Sun form through a process known as stellar nucleosynthesis. In the case of the Sun, it formed from a massive cloud of gas and dust, primarily composed of hydrogen and a smaller amount of helium, with trace amounts of other elements. Gravitational forces caused the cloud to collapse under its own gravity, leading to the formation of a dense, hot core. As the core contracted, it became hot enough and dense enough to trigger nuclear fusion.
Nuclear fusion in the Sun's core involves the conversion of hydrogen nuclei (protons) into helium nuclei. This process releases vast amounts of energy and sustains the Sun's radiation and luminosity. It is through these nuclear fusion reactions that protons combine to form helium nuclei, and in the process, electrons are involved as well.
Neutrons, on the other hand, are not as abundant in the Sun. Neutrons are electrically neutral particles found within atomic nuclei. They play a vital role in stabilizing atomic nuclei by balancing the repulsive forces between protons. However, free neutrons are not stable and undergo beta decay, where a neutron is converted into a proton, an electron, and an electron antineutrino. The presence of free neutrons in significant quantities in stars like the Sun is not observed.
In summary, the Sun consists mainly of protons (hydrogen nuclei) and electrons. The Sun formed from a cloud of primarily hydrogen and helium gas, and through nuclear fusion reactions, hydrogen nuclei combine to form helium nuclei, releasing energy in the process. Neutrons are not as prevalent in the Sun and do not play a significant role in its formation or composition.