Prominences are huge clouds of gas which are often seen on or above the solar limb, and are the easiest H-alpha emission feature to observe, requiring a filter passband that can be one or two Angstroms wide. Prominences observed on the solar disk are the darker features known as Filaments, and need a passband under one Angstrom wide in order to be clearly visible. They often represent a sheared magnetic field boundary or neutral line between opposite polarities where gas is trapped around bunched field lines. The forms prominences can take vary widely, but the following general scheme is somewhat useful in categorizing them:
CLASS 1: QUIESCENT FILAMENTS/PROMINENCES (long lived, fairly static)
A: QRF (Quiet Region Filament)ie: hedgerow, curtains, floating arches, arcs, fans, ect.
B: ASCENDING PROMINENCES (end of the quiescent phase) disparition brusque "lifting off" eruption.
C: ARF (Active Region Filament): a filament in or near an active region (neutral lines.
CLASS 2: ACTIVE FILAMENTS/PROMINENCES (short lived, moving)
A: LIMB FLARES: (bright blobs, sometimes expanding into eruptive prominences).
B: SURGES: collimated ejected material previously not seen (very sudden jet of gas).
C: SPRAYS: uncollimated ejecta previously visible as pre-flare elevated features (violent explosion)>
D: FLARE LOOPS and CORONAL RAIN (often post-flare ejecta or other gas).
QUIESCENT PROMINENCES/FILAMENTS take a wide variety of forms, and tend to be much longer than they are wide. Quiet Region Filaments (QRFs) are some of the largest and longest lasting quiescents, with a few being visible for several solar rotations. They are most often found where there is little major activity such as the so-called "Polar Crown" high latitude areas, although they may sometimes be found between or even near active regions.
The Hedgerow prominence is a fairly common QRF, and tends to look like an irregular row of bushes. Hedgerows tend to highly detailed, with considerable branching and fine structure being visible at high resolution. QRFs appear in many other forms, including floating arches, fans, curtains, large curving blades, flames, and magnificent spiderweb-like arcs. Many have upper edges that tend to be sharper than their lower sides, which can be irregular or scalloped in form.
Motion of material in QRFs is usually slow and small in scale, leaving the overall prominence shape unchanged, but minor changes can occasionally be seen in as little as 10 minutes. When viewed on the solar disk, QRFs tend to lose some of their fine detail, becoming faint irregular dark patches or large gently curving arcs of dark matter. Prominences are darker on the disk because they absorb light from below and then re-emit it in all directions. Some low-level filaments will often show a brighter base due to a "blanketing" effect they have which reduces the emission looses of the lower chromosphere.
Large Quiescents are not always stable, and if they exceed a height of 50,000 km above the surface (0.07 solar radii), they will usually break loose from the sun within 48 hours in an eruption known as a "Disparition Brusque" (sudden vanishing). Disparition Brusque eruptions usually last less than one or two hours. They vary in form from a simple fading away of the quiescent, to a spectacular "lifting off", where the prominence rises up and drifts away from the sun, slowly breaking up in the process.
Mild surface brightening can also occasionally occur. Sometimes, a vanished quiescent will even reform a few hours or days later near its previous location. In a few large eruptions, a Dispartition Brusque can produce a Coronal Mass Ejection. Some prominences do rotate slowly, and a few even look and act like tornadoes, especially Disparition Brusque debris.
Active Region Filaments(ARF's)(best seen on the solar disk)tend to be smaller than their giant cousins, the QRFs. They are present in or near active regions and sometimes wind around or even through large sunspot groups. The Neutral Line Filament is an active region undergoing the shearing of local magnetic fields is an example of an ARF. Arch Filament System "filaments" between forming sunspots are really fibrils, tending to be small and fairly short-lived unless flux emergence goes on for very long. They can be particularly dark when a spot is emerging, and often show Doppler shifts from material flowing in the fibrils.
These jets sometimes take the form of fine closely-spaced spines which may be visible up to a solar radii from the limb. Surges can also be seen as bright-based narrow dark features on the disk of the sun (sometimes blue-shifted). Surges usually happen when a small satellite spot of opposite magnetic polarity comes up in or very close to the penumbra of a big regular sunspot. A small flare then occurs, resulting in an outward ejection of gas which is confined into a narrow stream by the dominant spot's field.
The surge ejecta's velocity (50-200 km/sec) isn't enough to leave the sun, and the gas will follow magnetic field lines as it falls or draws back, sometimes creating a "splash" of brightening near the point of origin. Much smaller non-flare surges can often be seen in active and occasionally in Ephemeral regions on the solar disk as tiny blue-shifted "smoke stack" or "puff" filaments, which resemble a smoke plume. Smoke stack surges usually last only a few minutes, and can occasionally occur in the middle of a fairly quiet area, especially in the early stages of an emerging flux region.
Another active promincence type, usually resulting from most violent flares, is the Spray, a spectacular uncollimated expansion of disrupted ARF material, sending debris flying off in many directions at speeds of 200-300 km/sec or more (up to 2000 km/sec for some of the largest flares). Usually, the filament involved is somewhat elevated initially, then it explodes outward in the spray. Motion of spray material can often be seen in only a few minutes time, and occasionally, material can be seen leaving the sun entirely (Coronal Mass Ejection).
Two other types of flare-associated active prominences are the Flare Loops, and Coronal Rain. Flare Loops are large think circular or elliptical vertical loops of gas which appear in the later stages or after a major flare. They tend to be brighter at the top and at their bases, and often show a nested structure of many very thin loops (Arcades), all with nearby endpoints. These loops are where flare ejecta or other gas has encountered the new magnetic field lines set up by the reconnection which occurs during the flare.
Motion of material can often be seen down both sides of the loop towards the surface. The first loops form fairly low, while succeeding loops form higher and higher above the surface. Flare loops are sometimes not seen after some explosive flares or with small flares. They usually last only a matter of hours, and should not be confused with the quiescent "Floating Arches" prominences, which are thick or irregular in form, and are much longer lived. Coronal Rain is the diffuse faint patchy emission from gas descending back towards the surface as it encounters magnetic field lines. It can often be seen often as material "raining" down into post-flare loops or active regions.
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