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 width under one Angstrom 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 (Zirin) is somewhat useful in categorizing
CLASS 1: QUIESCENT FILAMENTS/PROMINENCES (long lived, fairly static)
a. QRF (Quiet Region Filament) ie: hedgerow, curtains, floating arches, arcs, fans, etc.
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 (netural line filaments).
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).
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 be 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 darker 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 losses of the lower chromosphere. In addition, filaments
often have a lighter "filament channel" beneath them where the usual
dark mottled appearance of quiet regions in the Chromosphere is weak or
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.
Region Filaments (ARF's) (best seen on the solar disk) tend to be
smaller, darker, and narrower 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 in an active
region under- going 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.
are short-lived features associated with solar flares and other violent
events. Limb Flares can appear on the solar limb as elevated bright
blobs. Occasionally, a small ARF in which a flare begins will rise and
expand into a majestic Eruptive Prominence, often in the form of a
twisting loop, while intense emission appears on the surface. Flares
sometimes produce a SURGE Prominence, visible near the limb as a well
defined jet of bright gas, and which can occasionally be seen in
emission on the solar disk. 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.
active prominence type, usually resulting from the 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). Often, the filament involved becomes slightly 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
Two other types of flare-associated active prominences are the Flare Loops, and Coronal Rain. FLARE LOOPS are large thin circular or elliptical vertical loops of gas which appear in the later stages of, 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.