Solar prominence

A solar prominence is a large structure of relatively cool, dense plasma suspended in the Sun’s hot corona by magnetic fields. Seen against the solar disk, it appears as a dark filament.

Solar filament: A prominence viewed against the solar disk, where it appears as a dark, elongated feature. The same suspended plasma looks dark when it is silhouetted against the brighter disk.
Quiescent prominence: A relatively long-lived prominence located away from active solar regions. Its slow evolution contrasts with the rapid changes of eruptive structures.
Solar spectroscopy: The study of the Sun through its emitted or absorbed spectrum. Spectral lines reveal prominence temperature, composition, density, and motion.
Solar flare: A sudden brightening of the Sun caused by energy release in its atmosphere. Flares and prominence eruptions can arise from related magnetic energy release.
Solar magnetic field: The magnetic field produced by the Sun’s moving, electrically conducting plasma. Its structure provides the forces that suspend and shape prominence material.
Active-region prominence: A prominence associated with a magnetically active region of the Sun. Its location links prominence formation to complex, evolving magnetic fields.
H-alpha: A red spectral line of hydrogen produced by a transition between atomic energy levels. H-alpha observations make many prominences visible against the solar disk.
Space weather: Conditions in space influenced by solar activity and its effects on planetary environments and technology. Eruptions involving prominences can contribute to disturbances in near-Earth space.
Magnetic flux rope: A bundle of magnetic field lines twisted around a shared axis. Flux ropes can hold prominence plasma and may become unstable before an eruption.
Hanging prominence: A prominence configuration whose plasma appears suspended in dips of magnetic field lines. It illustrates how magnetic geometry can support dense material above the solar surface.

Linked from 14 pages