Our sun is the star in our solar system, which lies within a galaxy (Milky Way) within the universe. A star is a large glowing ball of gas that generates energy through nuclear fusion in its core.
The solar system (or star system) is all objects that orbit a star.
A galaxy is a huge collection of stars (millions or trillions) that are bound together by gravity. The universe is the sum total of all matter and energy.
The Earth is about 150 million km from the sun. (Which equals an astronomical unit [A.U.]) The sun s diameter is about 1,400,000 km across.
The Sun s Interior Layers Convective Zone Pressure from energy inside pushes out and gravity pulls outer layers in, so there is a great amount of pressure and heat inside the sun. Radiative Zone Fusion Core
The core is where the sun s energy comes from and it consists mostly of hydrogen and helium in a plasma state. The sun s energy comes from fusion, when 4 hydrogens fuse into helium and energy is released. The core can reach 15,600,000 degrees C.
The radiation zone can reach temperatures of 8 million degrees C, near the core, to 2 million degrees C near the convection zone. The radiation zone is also plasma, and cooler than the core. (Radiation means energy is transferred to another body.)
The convection zone consists of rising and falling currents of plasma, which carry energy to the sun s surface. The convection zone can reach temperatures of 1.5 million degrees C to 6,000 degrees C.
The Sun s Surface The Sun s Surface: The Photosphere
The photosphere is the visible surface of the sun. Temperatures are lower, and reach about 6,000 degrees C.
Granulation of the Sun s Surface Granules are on top of the convection currents they are the top of the convection bubble. They give grainy appearance to photosphere. Center is hotter, and edges are cooler and appear darker.
Convection Bubbles Cooler Hot
Sunspots are dark spots on the photosphere. They are much cooler and darker than the surrounding photosphere. The magnetic field is about 1,000 times stronger in a sunspot than the surrounding photosphere. Sunspots
The length of the sunspot cycle (a cycle in which the average number of sunspots on the sun gradually rises and falls) is about 11 years. Its thought the sun s magnetic field flip-flops with each cycle (magnetic north becomes magnetic south, etc) but still much to learn.
So here is how the sunspots come about Sun rotates faster at its equator (about 25 days), than at its poles (30 days) this coils the magnetic field, it kinks and breaks through surface of sun making a sunspot.
Sunspot Cycle
Mini Ice Age coincidence?? Researching if these low activity in sunspot cycle are associated with Ice Ages/climate on Earth.
Solar Flare
Solar flares are outbursts of light that rise up suddenly in areas of sunspot activity.
The Sun s Electromagnetic Field
Prominence Loop
Solar prominences dense clouds of material suspended above the sun s surface by its magnetic field.
The Sun s Atmosphere
Chromosphere is the inner layer of the sun s atmosphere. Where hydrogen emits light with a reddish color. Temperature is about 20,000 degrees C. Solar prominences dense clouds of material suspended above the sun s surface by its magnetic field.
Spicules Flames on the Sun s Surface
The Corona
The Corona is the outer atmosphere. The temperature here is about 1 million to 3 million degrees C.
Solar winds are streams of electrically charged particles that come from the corona. (Solar flares are also a source of solar winds. So, when there is an increase in sunspot activity, there is an increase in solar flares and solar winds.
Variation in material in Corona related to Sunspot Cycle
S O H O
Coronal Mass Ejection
Aurora occur when solar winds blow past Earth and interact with Earth s magnetic field. Gives off a beautiful display of colors and light in Earth s upper atmosphere. Auroras are usually seen near the Earth s magnetic poles and are often called Northern or Southern Lights.