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A coronal hole at the Sun's north pole observed in soft X-ray. Coronal hole size and population correspond with the solar cycle. As the Sun heads toward solar maximum, the coronal holes move closer and closer to the Sun's poles. [4] During solar maxima, the number of coronal holes decreases until the magnetic fields on the Sun reverse.
A coronal mass ejection (CME) Solar storms of different types are caused by disturbances on the Sun, most often from coronal mass ejections (CMEs) and solar flares from active regions, or, less often, from coronal holes.
A video of the series of coronal mass ejections in August 2010. A coronal mass ejection (CME) is a massive burst of solar wind and magnetic fields rising above the solar corona. [15] Near solar maxima, the Sun produces about three CMEs every day, whereas solar minima feature about one every five days. [16]
This sort of feature, which is called a coronal hole, develops every now and then and, at worst, ... RELATED: New NASA video shows the sun in stunning HD: Show comments. Advertisement.
Solar flare, a large explosion in the Sun's atmosphere caused by tangling, crossing or reorganizing of magnetic field lines; Coronal mass ejection (CME), a massive burst of plasma from the Sun, sometimes associated with solar flares; Geomagnetic storm, the interaction of the Sun's outburst with Earth's magnetic field
Solar jets are transient, collimated flows of plasma in the Sun's atmosphere. They occur at many different scales, temperatures, and locations, and are driven by the release of magnetic energy via magnetic reconnection. The plasma ejected by a solar jet travels away from the Sun along straight or oblique paths, tracing the local magnetic field.
On 8 May 2024, a solar active region which had been assigned the NOAA region number 13664 (AR3664) produced an X1.0-class and multiple M-class solar flares and launched several coronal mass ejections (CMEs) toward Earth. [6] On 9 May, the active region produced an X2.25- and X1.12-class flare each associated with a full-halo CME.
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. Prominences are anchored to the Sun's surface in the much brighter photosphere, and extend outwards into the solar corona.