Corona
From open-encyclopedia.com - the free encyclopedia.
- For other meanings, see corona (disambiguation)
The corona is the luminous "atmosphere" of the Sun extending millions of kilometres into space, most easily seen during a total solar eclipse, but also observable in a coronagraph.
An interesting feature of the corona is the fact that it is much hotter than the visible "surface" of the Sun: the photosphere is approximately 6000°C compared to the corona at over one million °C. The corona is much less dense than the photosphere, however, and so produces less light. The corona is separated from the photosphere by the relatively shallow chromosphere. The exact mechanism by which the corona is heated is still the subject of some debate, but likely possibilities include induction by the Sun's magnetic field and sonic pressure waves from below (the latter being less probable now that coronae are known to be present in early-type stars). The outer edges of the sun's corona are constantly being lost as solar wind.
During periods of quiet Sun the corona is more or less confined to the equatorial regions, with "coronal holes" covering the polar regions. During the Sun's active periods, the corona is evenly distributed over the equatorial and polar regions, though it is most prominent in areas with sunspot activity.
Generated by solar flares or large solar prominences, "coronal transients" are sometimes released. These are enormous loops of coronal material travelling outward from the Sun at over a million kilometres per hour, containing roughly 10 times the energy of the solar flare or prominence that triggered them.
Stars other than the Sun have coronae, which can be detected using X-ray telescopes. Some stellar coronae, particularly in young stars, are much more luminous than the sun's.
The high temperature of the corona gives it unusual spectral features, which led some to suggest that it was composed of a previously unknown substance, "coronium"; however these spectral features have since been traced to known elements in high states of ionisation.
Coronal heating problem
The coronal heating problem is the title of a problem in astronomy and astrophysics as to why the temperature of the Sun's corona is millions of degrees Celsius higher than that of the surface. Two separate theories have emerged to explain why the corona is so hot, wave heating and magnetic twisting.
The wave heating theory, proposed by Alan Hood, suggests that magnetic field waves are carried upwards from the center of the Sun. The energy of the waves are dumped in the corona causing it to heat rapidly.
The magnetic twisting theory, proposed by Richard Harrison, suggests that the Sun's magnetic field becomes looped and twisting as it rotates at different speeds depending on the lattitude. When these magnetic loops snap, they release their energy heating the coronal gas.
External links
da:Korona de:Korona fr:couronne solaire he:עטרה nl:Corona ja:コロナ pl:Korona słoneczna zh:日冕
