How does solar energy formed step by step?

Answer 1

• Hydrogen atoms collect in the center of the star, and are held together by gravity.
• This gravity causes an increase in temperature and pressure.
• The temperature increases to the point where the electron shells are stripped off, creating a fully ionized form of hydrogen - protons only.
• The ionized form of hydrogen is easier to fuse because the repulsive effect of the electrons is gone.
  • There is still repulsion from the protons, but it is easier to overcome with the electrons missing.
• The pressure causes the protons to fuse together; four protons binding together to form one helium nucleus.
  • The weak interaction causes two of the protons to change to neutrons, participating in the creation of helium.
• The resulting loss of mass is accompanied by a substantial release of energy, using Einstein's mass-equivalence equation e = mc2.
• This released energy contributes to the fusion reaction, and it is also released as radiation to the Solar System.
• The reaction stays in equilibrium, balancing gravity against the pressure created by the reaction.
• Over time, fuel (hydrogen) is consumed and, ultimately, the star runs out of fuel.
• When that happens, various scenarios ensue, based on the total mass of the star. In the case of our star, it will go to a red giant, consuming the four inner planets, Mercury, Venus, Earth, and Mars. That is probably three or four billion years away - so don't worry about it right now.
• For larger stars, other processes occur, such as the carbon-nitrogen-oxygen cycle. Our Sun uses the proton-proton cycle, as described above.