Solar Prominence
What is solar prominence?
A prominence is a prominent, light feature covering outward from the Sun’s come on, often in a loop shape. A prominence forms above timescales of about a day, and stable prominences may persist in the corona for various months. Some prominences break apart and give rise to coronal mass ejections. Scientists are presently researching how and why prominences are organized. Filaments are large areas of very dense, cool gas, held in place by magnetic fields.
When a prominence is viewed from a different perspective so that it is against the sun instead of against space, it appears darker than the surrounding background. Filaments are large regions of very dense, cool gas, held in place by magnetic fields. Filaments last for a few weeks or months. The gas in a filament will eventually move to a different layer in the Sun and will no longer be visible in an image of the chromosphere. Flocculi (plural of flocculus) are another term for these filaments, and dark flocculi typically describe the appearance of solar prominences when viewed against the solar disk in certain wavelengths.
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