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The solar corona It is the outermost part of the solar atmosphere, consisting of gases at very high temperatures, around 2 million degrees. It extends from about 16,000 km over the Photosphere (the visible surface of the Sun) to a few million km higher.
It is a true rehirviente atmosphere, that extends in radial direction giving life to that flow of particles, called Solar wind, that floods all interplanetary space.
The crown becomes visible to the naked eye during the total eclipses of the Sun, appearing as a suggestive white-pearl luminosity around the disk of the Sun hidden by the Moon.
In the forties it was discovered that the crown is much warmer than the photosphere. The photosphere of the Sun, or visible surface, has a temperature of almost 6,000 K. The chromosphere, which extends several thousand kilometers above the photosphere, has a temperature close to 30,000 K. But the crown, which extends from just above the chromosphere to the limit with the interplanetary space, it has a temperature of 1,000,000 K. To maintain this temperature, the crown needs a power supply.
The search for the mechanism by which energy reaches the crown is one of the classic problems of astrophysics. It is still unsolved, although many explanations have been proposed. Recent observations of space have shown that the crown is a collection of magnetic curls, and how these curls are heated has become the main focus of astrophysical research.
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