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.

Answer 2

Solar energy is formed when photons from the sun's rays hit solar panels, causing an electrical current to be generated through the photovoltaic effect. These panels absorb sunlight, which is then converted into electrical energy that can be used to power homes, businesses, and other applications. The energy is then either stored in batteries or fed directly into the grid for immediate use.