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"What insights about the sun are shared in the translated edition of Shams Al Ma'arif, the Book of Sun?"
The Sun is so massive that it makes up about 99.8% of the mass of our solar system.
The surface temperature of the Sun is about 5,500°C (10,000°F), but its core is a scorching 15,000,000°C (27,000,000°F).
The Sun is actually white, not yellow, but our atmosphere scatters the shorter, blue wavelengths of light, making it appear yellow to our eyes.
The Sun's energy is so powerful that it would take a train of coal 100 times longer than the Earth's circumference to generate the same amount of energy the Sun produces in one second.
The Sun is so massive that it warps the space around it, creating a gravitational pull that keeps planets in their orbits.
The Sun's core is so dense that a sugar-cube-sized amount of its material would weigh about the same as a mountain.
The Sun loses about 1% of its mass every billion years, which is about the same rate at which it loses energy.
The Sun's surface is covered in granules, which are hot, bright patches of gas that are about 1,000 km (620 miles) across.
The Sun's magnetic field is so strong that it affects the Earth's magnetic field, causing the aurora borealis (northern lights) and aurora australis (southern lights).
The Sun's light takes about 8 minutes and 20 seconds to reach Earth, which means that if the Sun were to suddenly go dark, we wouldn't even know it for 8 minutes and 20 seconds.
The Sun is not round in shape, but is actually slightly flattened at the poles and bulging at the equator due to its rapid rotation.
The Sun's corona, or outer atmosphere, is about 100 times hotter than its surface, with temperatures reaching up to 2,000,000°C (3,600,000°F).
The Sun is responsible for creating the solar wind, a stream of charged particles that flows away from the Sun at speeds of up to 400 km/s (250 miles/s).
The Sun's gravity holds our solar system together, and without it, the planets would fly off into space.
The Sun is so massive that it affects the orbits of nearby stars, which is why astronomers can use it to study the properties of other stars.
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