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Solar prominence seen in true color during totality of a solar eclipse. In solar physics , a prominence , sometimes referred to as a filament , [ a ] is a large plasma and magnetic field structure extending outward from the Sun 's surface, often in a loop shape.
The hypothesis was based on the idea that a star passed close enough to the sun early in its life to cause tidal bulges to form on its surface, which along with the internal process that leads to solar prominences, caused material to be ejected repeatedly from the sun. Due to the gravitational effects of the passing star, two spiral-like arms ...
Pre-eruption structures originate from magnetic fields that are initially generated in the Sun's interior by the solar dynamo. These magnetic fields rise to the Sun's surface—the photosphere—where they may form localized areas of highly concentrated magnetic flux and expand into the lower solar atmosphere forming active regions.
Solar prominences, explains NASA, are large, bright loops of plasma anchored to the Sun's surface in the photosphere — the visible surface of the Sun — that extend into the Sun's outer ...
A video clip of an erupting solar prominence, a CME. A prominence is a large, bright, gaseous feature extending outward from the Sun's surface, often in the shape of a loop. Prominences are anchored to the Sun's surface in the photosphere and extend outwards into the corona.
NASA's Parker Solar Probe is intended to approach the Sun to a distance of approximately 9.5 solar radii to investigate coronal heating and the origin of the solar wind. It was successfully launched on August 12, 2018 [ 36 ] and by late 2022 had completed the first 13 of more than 20 planned close approaches to the Sun. [ 37 ]
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 slow solar wind is twice as dense and more variable in nature than the fast solar wind. [32] [38] The slow solar wind appears to originate from a region around the Sun's equatorial belt that is known as the "streamer belt", where coronal streamers are produced by magnetic flux open to the heliosphere draping over closed magnetic loops.