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Some prominences are ejected from the Sun in what is known as a prominence eruption. These eruptions can have speeds ranging from 600 km/s to more than 1000 km/s. [ 1 ] At least 70% of prominence eruptions are associated with an ejection of coronal material into the solar wind known as a coronal mass ejection .
Solar flares were first observed by Richard Carrington and Richard Hodgson independently on 1 September 1859 by projecting the image of the solar disk produced by an optical telescope through a broad-band filter. [50] [51] It was an extraordinarily intense white light flare, a flare emitting a high amount of light in the visual spectrum. [50]
X1.2(X1.3)-class flares [93] and X4.5-class flare. [94] The flares with a magnitude of 6–7 occurred between 30 April and 4 May 2024. On 5 May the strength of the solar storm reached 5 points, which is considered strong according to the K-index. The rapidly growing sunspot AR3663 became the most active spot of the 25th solar cycle.
Murphy explained people were probably witnessing a "post eruptive solar prominence," which was likely the location of a solar flare. When a solar prominence is 'post eruptive'
How fast does a coronal mass ejection travel vs. a solar flare? A CME can reach speeds of almost 1,900 miles per second. At that speed one can reach Earth in about 15 to 18 hours. But CMEs do like ...
Typical coronal loops observed by TRACE Dynamics of coronal loops observed by SDO. In solar physics, a coronal loop is a well-defined arch-like structure in the Sun's atmosphere made up of relatively dense plasma confined and isolated from the surrounding medium by magnetic flux tubes.
The early evolution of CMEs is frequently associated with other solar phenomena observed in the low corona, such as eruptive prominences and solar flares. CMEs that have no observed signatures are sometimes referred to as stealth CMEs. [11] [12] Prominences embedded in some CME pre-eruption structures may erupt with the CME as eruptive prominences.
Often accompanying large solar flares and prominences are coronal mass ejections (CME). These are enormous emissions of coronal material and magnetic field that travel outward from the Sun at up to 3000 km/s, [ 24 ] containing roughly 10 times the energy of the solar flare or prominence that accompanies them.