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	Prominences and Plages
		Prominences and plages are structures that occur above the photosphere of the Sun.
		Quiescent prominences are extremely stable features and remain suspended in the corona where they slowly evolve and become more elongated over the course of several solar rotations (a timescale of a few months).
		Prominences are usually associated with regions of sunspot activity, and are clearly associated with the Sun's magnetic field.
	csep10.phys.utk.edu /astr162/lect/sun/prominences.html (360 words)

	Laboratory simulation of solar prominences
		Solar prominences are large arch-shaped structures observable in the solar corona.
		The physics of solar prominence instability is believed to be governed by magnetic forces and magnetic helicity issues.
		This laboratory simulation of solar prominences is based on the premise that the physics of erupting solar prominences is analogous to the physics of the formation of laboratory spheromaks.
	ve4xm.caltech.edu /Bellan_plasma_page/laborato.htm (206 words)

	Sun
		Prominences are immense clouds of glowing gas that erupt from the upper chromosphere.
		In this photograph, the solar poles are distinguished by a relative absence of supergranulation network, and a much darker tone than the central portions of the disk.
		This image of the solar corona was acquired on 23 December 1996 by the LASCO instrument on the SOHO spacecraft.
	www.solarviews.com /eng/sun.htm (1238 words)

	Brainboost - What are prominences
		Prominences are loops or sheets of glowing gas ejected from an active region on the solar surface.
		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.
		Solar prominences can be as small as a sunspot, about the size of Earth, or extend to nearly the diameter of the sun itself.
	www.brainboost.com /search.asp?Q=What+are+prominences&lfmq=1 (364 words)

	NASA - Sun-Earth Day - Technology Through Time - #53: Solar Prominences
		Solar physicists still do not understand exactly how the gases enter and leave solar prominences, but the basic details of prominences seem to be pretty well understood after more than 100 years of telescopic and mathematical study.
		Solar prominences can be as small as a sunspot, about the size of Earth, or extend to nearly the diameter of the sun itself.
		Although the cool gases within the prominence itself may not be hot enough to emit x-rays, it is often the case that at the two foot points of the prominence near the solar surface, copious amounts of hot gases may exist.
	sunearthday.nasa.gov /2007/locations/ttt_prominences.php (723 words)

	Space Weather Center
		Prominences are dark structures when seen against the bright solar disk, but appear bright when seen over the solar limb.
		Solar flares are marked by a sudden brightening near a Sunspot or prominence.
		Solar flares and CMEs often occur together, but what connections may exist between them is a matter of debate.
	www.spaceweathercenter.org /glossary/001/01.html (1941 words)

	* Solar prominences - (Astronomy): Definition
		Solar prominences are visible as part of the corona during a total solar eclipse.
		Solar prominences are usually only detectable by specialized instruments but can be visible during a total solar eclipse.
		Lyot (1931) for the purpose of observing the corona of the sun and solar prominences occurring in the chromosphere.
	en.mimi.hu /astronomy/solar_prominences.html (274 words)

	Howstuffworks "How the Sun Works"
		In this cycle, the sun undergoes a period of activity (solar maximum) followed by a period of quiet (solar minimum).
		Solar flares are thought to be caused by sudden magnetic field changes in areas where the sun's magnetic field is concentrated.
		Solar flares are accompanied by the release of gas, electrons, visible light, ultraviolet light and X-rays.
	science.howstuffworks.com /sun4.htm (738 words)

	Untitled
		Solar flares are spectacular discharges of magnetic energy from the corona.
		Solar winds are the result of gas expansion in the corona.
		Solar prominences are storms of gas which erupt from the surface in the form of columns which either shoot outward into space or twist and loop back to the Sun's surface.
	home.megapass.co.kr /~hwj804/sun.htm (651 words)

	petrolpump.co.in : energy sources, solar,Structure of the sun, Magnetic Field, Calculating the position of the Sun, ...
		To obtain an uninterrupted view of the Sun, the European Space Agency and NASA cooperatively launched the Solar and Heliospheric Observatory (SOHO) on December 2, 1995.
		A solar wind sample return mission, Genesis, was designed to allow astronomers to directly measure the composition of solar material.
		It returned to Earth in 2004 and is undergoing analysis, but it was damaged by crash-landing when its parachute failed to deploy on reentry to atmosphere.
	www.petrolpump.co.in /energy-sources/solar.htm (1126 words)

	On-Line Glossary of Solar-Terrestrial Terms
		A solar PROMINENCE that becomes activa- ted and is seen to ascend from the sun.
		Solar flares that occur repetitively in the same ACTIVE REGION, with essentially the same position and with a common pattern of development.
		Of the white-light CORONA (that is, the corona seen by the eye at a total solar eclipse), that portion which is caused by sunlight scattered by electrons in the hot outer atmosphere of the sun.
	sec.noaa.gov /info/glossary.html (3279 words)

	Hermit Eclipse: Science: The Sun
		Since prominences are denser, and hence heavier, than the surrounding coronal gas, there must be something holding them up; although the explanation for this is not fully understood, it is almost certainly to do with the complex magnetic fields of the Sun.
		Unlike solar prominences, flares always occur in active regions of the Sun, and are extremely rapid events; a typical flare is over in a few minutes, although the larger flares can last for an hour.
		In order for the chromosphere, corona and solar prominences to become visible, we need the photosphere to be totally blocked out; that means that the Moon needs to be big and/or near enough to cover it completely.
	www.hermit.org /Eclipse/why_sun.html (1145 words)

	Prominences
		Stannyan first described prominences in a letter to Flamsteed following the eclipse of 1706, but the first detailed descriptions of them were by the Swedish astronomer Vassinius at the eclipse of 1733 (although he incorrectly believed them to be lunar in origin).
		Prominences may be relatively quiescent, persisting for many weeks without significant change, or they may be violently active, erupting outward as far as three million kilometers (two million miles) from the sun’s surface.
		The more active prominences will exhibit changes from minute to minute; noting any movement or change is a worthy undertaking.
	www.math.nus.edu.sg /aslaksen/gem-projects/hm/0304-1-08-eclipse/Prominences.htm (177 words)

	The Sun
		Solar flares are spectacular discharges of magnetic energy from the corona.
		Solar winds are the result of gas expansion in the corona.
		Solar prominences are storms of gas which erupt from the surface in the form of columns which either shoot outward into space or twist and loop back to the Sun's surface.
	library.thinkquest.org /C0110277/solar_system/sun/sun.htm (473 words)

	Solar Flares, Prominences, and the Solar Wind - Enchanted Learning Software
		A solar flare is a magnetic storm on the Sun which appears to be a very bright spot and a gaseous surface eruption.
		The solar wind is a continuous stream of ions (electrically charged particles) that are given off by magnetic anomalies on the Sun.
		A solar prominence (also known as a filament) is an arc of gas that erupts from the surface of the Sun.
	www.allaboutspace.com /subjects/astronomy/sun/prominences.shtml (580 words)

	Solar Wind
		Within a region about 0.3 solar radii from the center of the Sun, the temperature and density are high enough (~10^7 K and 100 g/cm^3) to promote fusion of protons into helium nuclei.
		Because of solar rotation, the point where the open field line is anchored to the Sun moves and as a result the interplanetary magnetic field has the form of a spiral (This spiral pattern is not unlike the one seen for water emanating from a rotating garden sprinkler).
		As the solar wind expands, its density decreases as the inverse of the square of its distance from the Sun.
	fusedweb.pppl.gov /CPEP/Chart_Pages/5.Plasmas/SolarWind.html (1088 words)

	chromosphere. The Columbia Encyclopedia, Sixth Edition. 2001-05
		This spectrum is obtained before a solar eclipse reaches totality and is formed from the thin arc of the sun disappearing behind the moon’s disk.
		Most spectacular of the solar features are the streams of hot gas, called prominences, that shoot out thousands or even hundreds of thousands of miles from the sun’s surface at velocities as great as 250 mi per sec (400 km per sec).
		Another phenomenon occurring in the chromosphere is the solar flare, a sudden and intense brightening in a plage that rises to great brilliance in a few minutes, then fades dramatically in a half hour to several hours.
	www.bartelby.com /65/ch/chromosp.html (673 words)

	Solar Flares, Prominences, and the Solar Wind - Enchanted Learning Software
		A solar flare is a magnetic storm on the Sun which appears to be a very bright spot and a gaseous surface eruption.
		The solar wind is a continuous stream of ions (electrically charged particles) that are given off by magnetic anomalies on the Sun.
		A solar prominence (also known as a filament) is an arc of gas that erupts from the surface of the Sun.
	www.littleexplorers.com /subjects/astronomy/sun/prominences.shtml (580 words)

	Solar Physics: 0 to 1599
		It is far too faint to be seen against the blinding brightness of the solar disk itself, but becomes visible, and spectacularly so, at times of total solar eclipses when the solar disk is obscured by the Moon.
		Prominences are large accumulation of (relatively) cold gas held suspended high in the solar atmosphere by the Sun's magnetic field (see Slide 6 and sun_pictorialIntro/slide7.html">Slide 7 of the HAO slide set).
		Large prominences are often visible at times of solar eclipses, in the form of small reddish filaments or blobs in the lower corona.
	www.hao.ucar.edu /Public/education/Timeline.B.html (952 words)

	Astrophotography by Anthony Ayiomamitis
		The sun's outermost "shell", the chromosphere, is a region measuring approximately 2000 km deep and is the source of some incredibly dynamic activity and temperatures reaching 400,000 °C at its furthest distance from the photosphere and is not visible to the naked eye or telescope filtered with typical mylar white-light material.
		Violent explosions and outbursts involving the hydrogen gases and the process of nuclear fusion of hydrogen to helium lead to the development of filaments, flares and prominences.
		Filaments and prominences are typically characterized as Class I ("Quiescent Filaments and Prominences") or Class II ("Active Filaments and Prominences").
	www.perseus.gr /Astro-Solar-Prominences.htm (200 words)

	Solar & Eclipse
		Solar observing and imaging are one of the few astronomical activities that one can do during the daytime.
		Among the more interesting things to observe on the Sun are sunspots and solar prominences, both with their respective appropriate filters.
		The Total Solar Eclipse of August 11, 1999 in Europe was a great opportunity for anyone interested in solar photography.
	www.luminous-landscape.com /reviews/solar_eclipse.shtml (734 words)

	Solar Filters
		Basic to the understanding of the observed solar spectrums from the various parts of the layers about the sun is the concept of absorption and radiation of photons from atomic gasses.
		In addition to the constant boiling of the solar surface there are much greater spurts of material that are ejected from the surface of the sun which return in gigantic arcs.
		The granularity, the chromosphere and the solar prominences are so dim compared to the photosphere that they cannot be observed except during a solar eclipse or with very special telescopes and filters.
	www.mailbag.com /users/ragreiner/solarfilter.html (1940 words)

	Schmidt Cassegrain telescope advice - solar observing equipment & accessories
		Narrow-bandpass H-alpha filters (0.8 Å or less) may not display prominences as well, but they will show them and in addition they show the convection-current-driven granularity of the sun’s surface, much better than a 1.5 Å prominence filter is able to do.
		For example, in the case of the the Solar Max the front cell houses a narrow-band Fabry Perot etalon which is tuned to H-alpha and an energy rejection filter, while the rear cell holds a secondary interference filter that serves to block the peaks adjacent to H-alpha.
		But the Solar Max does not include that mounting plate for the front-cell components, and Coronado’s price for a mounting plate for an 8” scope is “$350 and up”, which must be added to the $995 for the rest of the H-alpha filter assembly.
	sctscopes.net /SCT_Tips/Nice_to_Have/Solar_Observing/solar_observing.html (1995 words)

	Branching of the Helium-to-Balmer emission ratio in solar prominences (Site not responding. Last check: )
		Branching of the Helium-to-Balmer emission ratio in solar prominences
		Whereas the Balmer excitation is almost uniformly distributed over the prominences, the He excitation is enhanced in strutured prominences of low brightness or in outer parts of unstructured bright prominences, where exciting and ionizing EUV radiation can freely penetrate.
		The atmospheric prominence parameters are not yet sufficiently known to allow a reliable determination of the solar He abundance.
	www.uni-sw.gwdg.de /research/preprints/1995/pr1995_23.html?nav_print=1& (148 words)

	Paul Bellan, Work in Progress
		Solar prominences take on their dramatic shapes for pretty much the same reason that a magnet can make iron shavings form an arc on a sheet of paper.
		Since a solar prominence is a natural container of plasma, Bellan's work could lead to a cheaper and easier way to confine plasma in fusion reactors.
		The miniature prominence, formed by a specially designed plasma gun, is about a billion times smaller than actual solar prominences and lasts for a time that is more than a billion times shorter.
	pr.caltech.edu /media/features/bellanwip.html (966 words)

	NASA/Marshall Solar Physics
		Prominences are dense clouds of material suspended above the surface of the Sun by loops of magnetic field.
		Prominences and filaments are actually the same things except that prominences are seen projecting out above the limb, or edge, of the Sun.
		However, as the magnetic loops that support them slowly change, filaments and prominences can erupt and rise off of the Sun over the course of a few minutes or hours (4.0 MB MPEG movie of the "Granddaddy" prominence eruption of 1945).
	solarscience.msfc.nasa.gov /feature2.shtml (327 words)

	California State University \| Public Affairs Department
		Solar prominences - luminous clouds of solar gas erupting from the sun - are unpredictable and spew out huge magnetic fields that travel into interplanetary space and on rare occasions can damage spacecrafts and Earth's electrical power grids.
		Bellan works with a group that has developed a laboratory devise that creates magnetized plasmas known as spheromaks that have the same conditions and dynamics as solar prominences to study the clouds effects on the atmosphere and spacecrafts.
		He will also describe the operation of the lab and present photographs showing an expanding, twisting lab simulation of a solar prominence.
	www.csus.edu /news/040401solar.html (218 words)

	Solar Wind
		In a region of the sun known as the corona, which can extend several solar radii from the edge of the sun, the temperatures range from 1 to 2 X 10^6 K, though it is not a very dense region.
		Although the dimensions of the magnetosphere vary depending on the solar wind speed and direction of the IMF, the typical distance from the earth to the edge of the magnetosphere on the dayside is about 10 Earth radii, while the magnetotail can stretch to distances as great as several hundred Earth radii.
		The magnetopause is the boundary layer formed between the inner magnetosphere and the shocked solar wind plasma of the magnetosheath.
	www.cem.msu.edu /~cem181h/projects/97/solar/index.htm (1444 words)

	Schmidt Cassegrain telescope advice - solar observing equipment & accessories
		Narrow-bandpass H-alpha filters (0.8 Å or less) may not display prominences as well, but they will show them and in addition they show the convection-current-driven granularity of the sun’s surface, much better than a 1.5 Å prominence filter is able to do.
		For example, in the case of the the Solar Max the front cell houses a narrow-band Fabry Perot etalon which is tuned to H-alpha and an energy rejection filter, while the rear cell holds a secondary interference filter that serves to block the peaks adjacent to H-alpha.
		But the Solar Max does not include that mounting plate for the front-cell components, and Coronado’s price for a mounting plate for an 8” scope is “$350 and up”, which must be added to the $995 for the rest of the H-alpha filter assembly.
	www.sctscopes.net /SCT_Tips/Nice_to_Have/Solar_Observing/solar_observing.html (1995 words)

	Sector "SUN"
		Furthermore, V. Dermendjiev was associated lecturer of the solar physics at the Astronomy Department in the faculty of Physics at Sofia University.
		Besides, some of the first solar physic researches were devoted to the behaviour of the green coronal line 5303 A, as well as of the monochromatic solar corona.
		The secondary polar zone of the solar prominences has been established in distribution of the polar prominences, observed in the coronal station Lomnicky Shtit, Slovakia in the period 1976-1990 (Dermendjiev et al., 1994c).
	www.astro.bas.bg /sun/history.html (1551 words)

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