The Sun is a type star: a huge sphere of gaseous, incadescent hydrogen.
Its source of energy is hidden into its deepest core where the temperature reaches 15 million grades.
The nucleus can be compared to an endless explosion of enormous
nuclear bombs. It converts 4 million tons of hydrogen into heat and light every second. The gas around its nucleus is expelled as energy and is carried to the surface of the Sun, where it is released as heat and light into the space.
A total solar eclipse is an extraordinary event.
For a few minutes the day changes into night: the sky turns dark, planets and stars can be seen, street lamps light up and birds stop twittering.
In a few words, it is a very exciting sight.
Eclipses take place when the sunlight or moonlight is darkened for a short time. They also happen in relation to other planets, when, for instance, Jupiter satellites move in the shadow of the planet but, in that case, they can be seen only through a telescope.
It is important to remember that it is necessary to wear a suitable eye protection while looking at the Sun during a solar eclipse.
| Diameter | 1,392,000 km |
| Flattening | 0.001 |
| Rotational period-mean sideral | 25.4 days |
| Rotational period-mean synoptic | 27.3 days |
| Mass (Earth=1) | 330,000 |
| Mean density (water=1) | 1.41 |
| Escape velocity | 617.5 km/s |
| Surface temperature | +5,800° K |
| Nucleus temperature | 15,000,000° K |
| Rotational period around the galactic centre | 225 milion years |
| Mean distance from Earth (=1AU) | 149,597,870 Km |
| Maximun distance | 152,100,000 Km |
| Minimum distance | 147,100,000 Km |
| Light distance from Earth | 8.3 light-minutes |
| Distance from the Galaxy centre | 25,000 light-years |
| Orbital eccentricity around the galactic centre | 0.206 |
| Spectrum type | G2 |
| Mean visible magnitude | -26,7 |
Oh shining Sun,
what on earth would you be,
if I were not, down here,
on whom to shine?
(Friedrich Nietzsche)
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