Astronomy:Solar prominence

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Short description: Structure extending off of the Sun's surface
False-color image of a solar prominence captured in 304 Å (30.4 nm) radiation emitted by He II

A prominence, sometimes referred to as a filament,[lower-alpha 1] 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 photosphere, and extend outwards into the solar corona. While the corona consists of extremely hot plasma, prominences contain much cooler plasma, similar in composition to that of the chromosphere.

Prominences form over timescales of about a day and may persist in the corona for several weeks or months, looping hundreds of thousands of kilometers into space. Some prominences may give rise to coronal mass ejections. Scientists are currently researching how and why prominences are formed.

A typical prominence extends over many thousands of kilometers; the largest on record was estimated at over 800,000 km (500,000 mi) long,[2] roughly a solar radius.

History

Solar prominences can sometimes be visible in red around the edges of the Sun during a total solar eclipse.

The first detailed description of a solar prominence was in 14th-century Laurentian Codex, describing the solar eclipse of May 1, 1185. They were described as "flame-like tongues of live embers".[3][4][5]

Prominences were first photographed during the solar eclipse of July 18, 1860, by Angelo Secchi. From these photographs, altitude, emissivity, and many other important parameters were able to be derived for the first time.[6]

During the solar eclipse of August 18, 1868, spectroscopes were for the first time able to detect the presence of emission lines from prominences. The detection of a hydrogen line confirmed that prominences were gaseous in nature. Pierre Janssen was also able to detect an emission line corresponding to an at the time unknown element now known as helium. The following day, Janssen confirmed his measurements by recording the emission lines from the now unobstructed Sun, a task that had never been done before. Using his new techniques, astronomers were able to study prominences daily.[7]

Classification

H-alpha image of the solar disk showing quiescent filaments (QF), intermediate filaments (IF), and active region filaments (ARF).

There are a number of different prominence classification schemes in use today. One of the most widely used and basic schemes classifies prominences based on the magnetic environment in which they had formed. There are three classes:

  • Active region prominences, or active region filaments, form within the relatively strong magnetic fields at the centers of active regions. Active region prominences have lifetimes ranging from hours to days and erupt more often than prominences belonging to the other classes.[8] As a consequence of being located within active regions, active region prominences are usually found in low heliographic latitudes.[9][10]
  • Intermediate prominences, or intermediate filaments, form between a weak unipolar plage regions and active regions.
  • Quiescent prominences, or quiescent filaments, form in the weak background magnetic field far from any active regions.[11] Unlike active region prominences, quiescent prominences are relatively stable and can have lifetimes ranging from weeks to months, hence the name quiescent.[8] Quiescent prominences are typically located at high latitudes around what is referred to as the polar crown.[9][10] Additionally, quiescent prominences generally reach much greater heights in the corona than active region prominences.

Active region and quiescent prominences can also be differentiated by their emitted spectra. The spectra of active region prominences is identical to that of the upper chromosphere having strong He II lines but very weak ionized metal lines. On the other hand, the spectra of quiescent prominences is identical to the spectra measured at 1,500 km (930 mi) in the chromosphere with strong H, He I, and ionized metal lines, but weak He II lines.[12]

Morphology

Filament channels

Prominences form in magnetic structures known as filament channels where they are thermally shielded from the surrounding corona and supported against gravity. These channels are found in the chromosphere and lower corona above divisions between regions of opposite photospheric magnetic polarity known as polarity inversion lines (PIL).[lower-alpha 2] The presence of a filament channel is a necessary condition for the formation of a prominence, but a filament channel can exist without containing a prominence. Multiple prominences may form and erupt from within one filament channel over the channel's lifetime. The magnetic field making up the filament channel is predominantly horizontal, pointing in the same direction on both sides of the PIL (see § Chirality).[13][14][15]

Prominence material does not occupy the entire width of the filament channel; a tunnel-like region less dense than the corona, known as a coronal cavity, occupies the volume between the prominence and the overlying magnetic arcade.[7]

Spines and barbs

Typical prominences have a narrow structure oriented along the filament channel known as a spine. The spine defines the upper main body of a prominence and is generally in the form of a vertical sheet that diverges towards the photosphere at both ends. Many prominences also have smaller structures referred to as barbs that similarly diverge from the spine towards the chromosphere and photosphere. Spines and barbs are both composed of thin threads that trace the magnetic field similar to chromospheric fibrils.[14]

The cool prominence material that makes up spines and barbs—the prominence core—is surrounded by a prominence-corona transition region (PCTR) where there is a steep temperature gradient. The PCTR is responsible for most of the optical emission of prominences.[7]

H-alpha image of an active region filament showing a spine, two barbs, and chromospheric fibrils oriented parallel to the PIL[13]

Overlying structures

Main page: Astronomy:Helmet streamer

Above filament channels lie overarching magnetic arcades which can extend from 50,000 to 70,000 km (31,000 to 43,000 mi) into the corona. Above these arcades, the closed coronal magnetic field may extend radially outward, forming what is known as a helmet streamer.[16] These streamers may reach a solar radius or more above the Sun's surface.[7]

Chirality

Filament channels and their prominence, if present, exhibit chirality. When observed from the side of the filament channel with positive magnetic polarity, the channel is said to be dextral if the horizontal magnetic field is oriented rightward and sinistral if it is oriented leftward. Dextral channels have been found more frequently in the Sun's northern hemisphere and sinistral channels more frequently in the southern hemisphere.

The horizontally oriented magnetic field causes chromospheric fibrils along the filament channel to lie nearly parallel to the PIL and anti-parallel to one another on opposite sides of the PIL. The directions that these fibrils are oriented depend on the chirality of the channel. On the side of the PIL with positive magnetic polarity, dextral channels have fibrils which stream to the right and barbs which bear to the right, whereas sinistral channels have fibrils which stream to the left and barbs which bear to the left. Additionally, the overlying magnetic arcades of dextral channels are left-skewed, and those of sinistral channels are right-skewed.[7]

Formation

The exact mechanism which leads to the formation of solar prominences is not currently known. Models must be able to explain the formation of the filament channel and its hemisphere-dependent chirality, as well as the origin of the dense plasma that makes up the prominence core.[7]

Eruption

File:Solar prominence.ogv Some prominences are ejected from the Sun in what is known as a prominence eruption. These eruptions can have speeds ranging from 600 km/s to more than 1000 km/s.[1] At least 70% of prominence eruptions are associated with an ejection of coronal material into the solar wind known as a coronal mass ejection.[17]

See also

Explanatory notes

  1. ↑ When viewed against the background of space (off-limb), they are referred to as prominences; when viewed against the Sun's surface (on-disk), they are referred to as filaments.[1]
  2. ↑ Divisions between regions of opposite photospheric magnetic polarity are variously referred to as polarity inversion lines (PIL), polarity reversal boundaries (PRB), or neutral lines.

References

  1. ↑ 1.0 1.1 "About Filaments and Prominences". solar.physics.montana.edu. http://solar.physics.montana.edu/ypop/Program/hfilament.html. 
  2. ↑ Atkinson, Nancy (6 August 2012). "Huge Solar Filament Stretches Across the Sun". Universe Today. http://www.universetoday.com/96649/huge-solar-filament-stretches-across-the-sun/. 
  3. ↑ "1185: The first description of solar prominences". High Altitude Observatory. 2008. https://www2.hao.ucar.edu/Education/solar-physics-historical-timeline-0-1599#1185. 
  4. ↑ "1185: The first description of solar prominences". Université de Montréal. 2008. http://www.astro.umontreal.ca/~paulchar/grps/histoire/newsite/sp/great_moments_e.html. 
  5. ↑ Poitevin, Patrick; Edmonds, Joanne (2003). "Solar Eclipse Newsletter". http://eclipse.gsfc.nasa.gov/SENL/SENL200305.pdf. 
  6. ↑ Secchi, Angelo (1870). Le Soleil, Part 1. Paris: Gauthier-Villars. p. 378. https://play.google.com/store/books/details?id=V-gRAAAAYAAJ&rdid=book-V-gRAAAAYAAJ&rdot=1. 
  7. ↑ 7.0 7.1 7.2 7.3 7.4 7.5 Vial, Jean-Claude; Engvold, Oddbjørn (2015). Solar Prominences. Springer. ISBN 978-3-319-10415-7. 
  8. ↑ 8.0 8.1 Mackay, D. H.; Karpen, J. T.; Ballester, J. L.; Schmieder, B.; Aulanier, G. (April 2010). "Physics of Solar Prominences: II—Magnetic Structure and Dynamics". Space Science Reviews 151 (4): 333–399. doi:10.1007/s11214-010-9628-0. Bibcode: 2010SSRv..151..333M. 
  9. ↑ 9.0 9.1 Menzel, Donald H.; Jones, F. Shirley (December 1962). "Solar Prominence Activity, 1944-1954". Journal of the Royal Astronomical Society of Canada 56: 193. Bibcode: 1962JRASC..56..193M. https://apps.dtic.mil/sti/citations/AD0402858. 
  10. ↑ 10.0 10.1 Minarovjech, M.; Rybanský, M.; Rušin, V. (1998). "Time-Latitude Prominence and the Green Corona Distribution over the Solar Activity Cycle". International Astronomical Union Colloquium 167: 484–487. doi:10.1017/S0252921100048132. 
  11. ↑ Engvold, Oddbjørn (1998). "Observations of Filament Structure and Dynamics". International Astronomical Union Colloquium 167: 22–31. doi:10.1017/S0252921100047229. 
  12. ↑ Zirin, Harold; Tandberg-Hanssen, Einar (1960). "Physical Conditions in Limb Flares and Active Prominences. IV. Comparison of Active and Quiescent Prominences". The Astrophysical Journal 131: 717–724. doi:10.1086/146884. Bibcode: 1960ApJ...131..717Z. http://adsabs.harvard.edu/pdf/1960ApJ...131..717Z. 
  13. ↑ 13.0 13.1 Parenti, Susanna (2014). "Solar Prominences: Observations". Living Reviews in Solar Physics 11 (1): 1. doi:10.12942/lrsp-2014-1. Bibcode: 2014LRSP...11....1P. https://link.springer.com/content/pdf/10.12942/lrsp-2014-1.pdf. Retrieved 29 January 2022. 
  14. ↑ 14.0 14.1 Gibson, Sarah E. (December 2018). "Solar prominences: theory and models: Fleshing out the magnetic skeleton". Living Reviews in Solar Physics 15 (1): 7. doi:10.1007/s41116-018-0016-2. PMID 30872983. PMC 6390890. Bibcode: 2018LRSP...15....7G. https://link.springer.com/content/pdf/10.1007/s41116-018-0016-2.pdf. Retrieved 29 January 2022. 
  15. ↑ Gaizauskas, V. (1998). "Filament Channels: Essential Ingredients for Filament Formation" (in en). International Astronomical Union Colloquium 167: 257–264. doi:10.1017/S0252921100047709. ISSN 0252-9211. 
  16. ↑ Guo, W. P.; Wu, S. T. (10 February 1998). "A Magnetohydrodynamic Description of Coronal Helmet Streamers Containing a Cavity". The Astrophysical Journal 494 (1): 419–429. doi:10.1086/305196. Bibcode: 1998ApJ...494..419G. 
  17. ↑ Gopalswamy, N.; Shimojo, M.; Lu, W.; Yashiro, S.; Shibasaki, K.; Howard, R. A. (20 March 2003). "Prominence Eruptions and Coronal Mass Ejection: A Statistical Study Using Microwave Observations". The Astrophysical Journal 586 (1): 562–578. doi:10.1086/367614. Bibcode: 2003ApJ...586..562G. 

Further reading

External links



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