Solar spicules
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Solar spicules are structures found in the Sun's atmosphere, specifically in the chromosphere.
These columns of hot, glowing gas rise from the solar surface upwards, reaching heights of several thousand kilometres. They can be observed during solar eclipses or with specialised solar telescopes.
These structures are of vital importance for understanding solar activity and behaviour.
Solar spicules provide us with information about the dynamics and processes occurring in the solar atmosphere. In addition, they are also related to larger phenomena, such as coronal mass ejections and solar storms.
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Solar spicules are mainly composed of hydrogen, although they can also contain other elements. They form due to the magnetic energy present in the Sun.
As magnetic fields twist and intertwine in the Sun's atmosphere, they create forces that push the gas upwards, creating these impressive structures.
The duration of solar spicules can vary from a few minutes to several hours. Their size can also be quite significant, reaching dimensions of up to several thousand kilometres in length.
Their appearance is very striking, with an intense glow and a shape that resembles spears or rising jets of solar gas.
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Studying solar spicules gives us a better understanding of solar physics and their influence on our solar system.
They are also important for research and monitoring of solar phenomena that can affect the Earth, such as geomagnetic storms.
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