Luminosity: Measure of the brightness of the Sun.
Chemical Energy Content: Estimated at around 10,000 years.
Gravitational Potential: Roughly 25 million years.
Nuclear Potential Energy: Estimated to last about 10 billion years.
Energy Balance: Energy radiated from the Sun's surface equals energy produced by nuclear fusion in the core.
Gravitational Equilibrium: Balances the Sun's inward gravitational crush with energy produced by fusion.
Core Heating: Energies from gravitational contraction ceased once nuclear fusion started.
Core: Site of nuclear fusion, temperature ~15 million K.
Radiation Zone: Energy moves out via photons.
Convection Zone: Hot gas rises, carrying energy to the surface.
Photosphere: Visible surface, temperature ~6,000 K.
Chromosphere: Middle layer, temp ~4,500 K.
Corona: Outermost layer, temp ~1 million K, affected by solar wind.
Fusion vs. Fission: Fusion combines small nuclei (e.g., hydrogen fusing into helium); fission splits large nuclei.
Proton–Proton Chain: Main fusion process in the Sun, resulting in helium from hydrogen.
Energy Release: Conversion leads to a mass loss of about 0.7% of original mass.
Energy Escape: Energy gradually leaks out via random photons; convection moves hot gas upwards.
Solar Thermostat: Regulates fusion rate and core temperature.
Solar Phenomena: Includes sunspots, solar flares, and prominences, all tied to magnetic fields.
Sunspots: Cooler areas (~4,000 K) where strong magnetic fields exist.
Solar Flares and Prominences: Driven by magnetic activities and can affect solar wind.
Cycle Duration: Approximately 11 years, with varying sunspot density.
Solar Activity Variation: Effects on Earth’s climate considered negligible despite solar cycles.
Magnetic Field Influence: Sunspots and solar activity related to the twisting of magnetic fields.