 There is the Core, the inside of the sun which makes the heat.  The Radiative zone is the second to the inside zone.  Next is the Convective zone, the zone after the Radiative zone.  Then there is the Photosphere, the surface of the sun and the part we see.  The Chromosphere is next.  After that is the Corona and we can only see this part during a solar eclipse.  Solar Flares go out into space, from the Chromosphere. (The loops on the sun).

 The core is the hottest part of the sun. This is the only part of the sun where it makes it’s own heat. Around here it is about 27 million degrees Fahrenheit.  In the Radiative zone, it gets cooler, (as expected) and around here it ranges from 3.6 million degrees to 12.6 million degrees F.  The convective zone, is reasonably cooler and here it is around 3.6 million degrees F.  The photosphere is 10,000 degrees F.  The sunspots on the sun are about 7,300 degrees! It’s getting cold now!  The Chromosphere is 7,800 degrees. These loops are awesome! But wait a minute, this is hotter than sunspots!  The Corona, you can’t see regularly on earth. Although in this region, it unexpectedly and unknown gets hotter to 3 million degrees! It’s pretty confusing!

 The core of the sun is white.  White is all colors, so the inside of the sun is scientifically all colors.

 Sunspots are caused by the Chromospheres breaking.

 The core of the sun is 200,000 miles across.  It is ¼ the size of the entire sun.

 109 Earths could fit around the sun, and that’s not even including the inside of the sun! Not even the whole surface!!!!  The diameter is 860,000 miles!

 This is a stream of energized, charged, particles.  Electrons and protons flow out from the sun, and their speeds are as high as 500 miles per second!  Solar wind is caused by the Chromosphere.  Solar Wind is 800 km per hour.

 In the core, helium comes together to form hydrogen, which makes a lot of heat.  This constantly happens, so the sun produces LOTS of heat.  This process only happens in the core of the sun.

 The light radiates outward from the core of the sun.  Heat moves through all of the zones.  The chromosphere breaks.  Plasma hurdles out to space.  This process is called a Solar Storm.  After about 6 hours, it passes the planet Mercury.  After about 12 hours, it passes the planet Venus.  After about 18 hours, it reaches Earth.  When it reaches Earth, our planet’s magnetic field extends, and throws the plasma into the poles.  That plasma travels, and makes the night time auroras on Earth.

 Age: 4.6 billion years old  Type: Yellow Dwarf  Diameter: 1,392,684 km  Circumference at equator: 4,320,005.6 km  Mass: 1,989,100,000,000,000,000,000 billion kg

 Sunspots come in pairs.  The sun has many magnetic fields.  A very long time away, the sun will be the same size as Earth.  The sun has 99.86% of the mass in the solar system.  It takes thousands of years for the light from the core of the sun to go to the surface.