Astronomy:Triangulum

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Short description: Constellation in the northern celestial hemisphere


Triangulum
Constellation
Triangulum
AbbreviationTri
GenitiveTrianguli
Pronunciation/traɪˈæŋɡjʊləm/,
genitive /traɪˈæŋɡjʊlaɪ/
SymbolismThe Triangle
Right ascension 01h 31.3m to  02h 50.4m[1]
Declination25.60° to 37.35°[1]
QuadrantNQ1
Area132 sq. deg. (78th)
Main stars3
Bayer/Flamsteed
stars		14
Stars with planets3
Stars brighter than 3.00m0
Stars within 10.00 pc (32.62 ly)0
Brightest starβ Tri (3.00m)
Messier objects1
Bordering
constellations		Andromeda
Pisces
Aries
Perseus
Visible at latitudes between +90° and −60°.
Best visible at 21:00 (9 p.m.) during the month of December.

Triangulum is a small constellation in the northern sky. Its name is Latin for "triangle", derived from its three brightest stars, which form a long and narrow triangle. Known to the ancient Babylonians and Greeks, Triangulum was one of the 48 constellations listed by the 2nd century astronomer Ptolemy. The celestial cartographers Johann Bayer and John Flamsteed catalogued the constellation's stars, giving six of them Bayer designations.

The white stars Beta and Gamma Trianguli, of apparent magnitudes 3.00 and 4.00, respectively, form the base of the triangle and the yellow-white Alpha Trianguli, of magnitude 3.41, the apex. Iota Trianguli is a notable double star system, and there are three star systems with known planets located in Triangulum. The constellation contains several galaxies, the brightest and nearest of which is the Triangulum Galaxy or Messier 33—a member of the Local Group. The first quasar ever observed, 3C 48, also lies within the boundaries of Triangulum.

History and mythology

In the Babylonian star catalogues, Triangulum, together with Gamma Andromedae, formed the constellation known as MULAPIN (𒀯𒀳) "The Plough". It is notable as the first constellation presented on (and giving its name to) a pair of tablets containing canonical star lists that were compiled around 1000 BC, the MUL.APIN. The Plough was the first constellation of the "Way of Enlil"—that is, the northernmost quarter of the Sun's path, which corresponds to the 45 days on either side of summer solstice. Its first appearance in the pre-dawn sky (heliacal rising) in February marked the time to begin spring ploughing in Mesopotamia.[2]

The Ancient Greeks called Triangulum Deltoton (Δελτωτόν), as the constellation resembled an upper-case Greek letter delta (Δ). It was transliterated by Roman writers, then later Latinised as Deltotum.[3] Eratosthenes linked it with the Nile Delta, while the Roman writer Hyginus associated it with the triangular island of Sicily, formerly known as Trinacria due to its shape.[4] It was also called Sicilia, because the Romans believed Ceres, patron goddess of Sicily, begged Jupiter to place the island in the heavens.[3] Greek astronomers such as Hipparchos and Ptolemy called it Trigonon (Τρίγωνον), and later, it was Romanized as Trigonum. Other names referring to its shape include Tricuspis and Triquetrum.[3] Alpha and Beta Trianguli were called Al Mīzān, which is Arabic for "The Scale Beam".[5] In Chinese astronomy, Gamma Andromedae and neighbouring stars including Beta, Gamma and Delta Trianguli were called Teen Ta Tseang Keun (天大将军, "Heaven's great general"), representing honour in astrology and a great general in mythology.[4][6]

Later, the 17th-century German celestial cartographer Johann Bayer called the constellation Triplicitas and Orbis terrarum tripertitus, for the three regions Europe, Asia, and Africa. Triangulus Septentrionalis was a name used to distinguish it from Triangulum Australe, the Southern Triangle.[3] Polish astronomer Johannes Hevelius excised three faint stars—ι, 10 and 12 Trianguli—to form the new constellation of Triangulum Minus in his 1690 Firmamentum Sobiescianum, renaming the original as Triangulum Majus.[7] The smaller constellation was not recognised by the International Astronomical Union (IAU) when the constellations were established in the 1920s.[5]

Characteristics

A small constellation, Triangulum is bordered by Andromeda to the north and west, Pisces to the west and south, Aries to the south, and Perseus to the east. The centre of the constellation lies halfway between Gamma Andromedae and Alpha Arietis.[8] The three-letter abbreviation for the constellation, as adopted by the IAU in 1922, is "Tri".[9] The official constellation boundaries, as set by Belgian astronomer Eugène Delporte in 1930, are defined as a polygon of 14 segments. In the equatorial coordinate system, the right ascension coordinates of these borders lie between  01h 31.3m and  02h 50.4m, while the declination coordinates are between 25.60° and 37.35°.[1] Covering 132 square degrees and 0.320% of the night sky, Triangulum ranks 78th of the 88 constellations in size.[10]

Features

Bayer catalogued five stars in the constellation, giving them the Bayer designations Alpha to Epsilon. John Flamsteed added Eta, Iota and four Roman letters; of these, only Iota is still used as the others were dropped in subsequent catalogues and star charts.[11] Flamsteed gave 16 stars Flamsteed designations, of which numbers 1 and 16 are not used—1's coordinates were in error as there was no star present at the location that corresponds to any star in his Catalogus Britannicus; Baily presumed that the coordinates were mistranscribed 32s in error by Flamsteed and in fact referred to 7.4 magnitude HD 10407. Baily also noted that 16 Trianguli was closer to Aries and included it in the latter constellation.[11]

The constellation Triangulum as it can be seen by the naked eye.

Stars

Three stars make up the long narrow triangle that gives the constellation its name. The brightest member is the white giant star Beta Trianguli of apparent magnitude 3.00,[5] lying 127 light-years distant from Earth.[12] It is actually a spectroscopic binary system; the primary is a white star of spectral type A5IV with 3.5 times the mass of the Sun that is beginning to expand and evolve off the main sequence. The secondary is poorly known, but calculated to be a yellow-white F-type main-sequence star around 1.4 solar masses. The two orbit around a common centre of gravity every 31 days, and are surrounded by a ring of dust that extends from 50 to 400 AU away from the stars.[13]

The second-brightest star, the yellow-white subgiant star Alpha Trianguli (3.41m) with a close dimmer companion, is also known as Caput Trianguli or Ras al Muthallath, and is at the apex of the triangle. It lies around 7 degrees north-northwest of Alpha Arietis.[14] Making up the triangle is Gamma Trianguli, a white main sequence star of spectral type A1Vnn of apparent magnitude 4.00 about 112 light-years from Earth.[15] It is around double the size of and around 33 times as luminous as the sun and rotates rapidly. Like Beta, it is surrounded by a dusty debris disk, which has a radius 80 times the distance of the Earth from the Sun.[16] Lying near Gamma and forming an optical triple system with it are Delta and 7 Trianguli. Delta is a spectroscopic binary system composed of two yellow main sequence stars of similar dimensions to the Sun that lies 35 light-years from Earth. The two stars orbit each other every ten days and are a mere 0.1 AU apart.[17] This system is the closest in the constellation to the Earth.[10] Only of magnitude 5.25, 7 Trianguli is much further away at around 280 light-years distant from Earth.[18]

Iota Trianguli is a double star whose components can be separated by medium-sized telescopes into a strong yellow and a contrasting pale blue star. Both of these are themselves close binaries.[19] X Trianguli is an eclipsing binary system that ranges between magnitudes 8.5 and 11.2 over a period of 0.97 days.[20] RW Trianguli is a cataclysmic variable star system composed of a white dwarf primary and an orange main sequence star of spectral type K7 V. The former is drawing off matter from the latter, forming a prominent accretion disc. The system is around 1075 light-years distant.[21]

R Trianguli is a long period (Mira) variable that ranges from magnitude 6.2 to 11.7 over a period of 267 days.[20] It is a red giant of spectral type M3.5-8e, lying around 960 light-years away.[22] HD 12545, also known as XX Trianguli, is an orange giant of spectral type K0III around 520 light-years distant with a visual magnitude of 8.42.[23] A huge starspot larger than the diameter of the Sun was detected on its surface in 1999 by astronomers using Doppler imaging.[24]

Two star systems appear to have planets. HD 9446 is a Sun-like star around 171 light-years distant that has two planets of masses 0.7 and 1.8 times that of Jupiter, with orbital periods of 30 and 193 days respectively.[25] HD 13189 is an orange giant of spectral type K2II about 2–7 times as massive as the Sun with a planetary or brown dwarf companion between 8 and 20 times as massive as Jupiter, which takes 472 days to complete an orbit. It is one of the largest stars discovered to have a planetary companion.[26]

Deep-sky objects

The peculiar asymmetry of NGC 949.[27]

The Triangulum Galaxy, also known as Messier 33, was discovered by Giovanni Battista Hodierna in the 17th century.[28] A distant member of the Local Group, it is about 2.3 million light-years away, and at magnitude 5.8 it is bright enough to be seen by the naked eye under dark skies. Being a diffuse object, it is challenging to see under light-polluted skies, even with a small telescope or binoculars, and low power is required to view it. It is a spiral galaxy with a diameter of 46,000 light-years and is thus smaller than both the Andromeda Galaxy and the Milky Way. A distance of less than 300 kiloparsecs between it and Andromeda supports the hypothesis that it is a satellite of the larger galaxy.[29] It is believed to have been interacting with it from their velocities.[30] Within the constellation, it lies near the border of Pisces, 3.5 degrees west-northwest of Alpha Trianguli and 7 degrees southwest of Beta Andromedae.[14] Within the galaxy, NGC 604 is an H II region where star formation takes place.[31][32]

IC 1727 and UGC 1249.[33]

In addition to M33, there are several NGC galaxies of visual magnitudes 12 to 14.[5] The largest of these include the 10 arcminute long magnitude 12 NGC 925 spiral galaxy and the 5 arcminute long magnitude 11.6 NGC 672 barred spiral galaxy. The latter is close by and appears to be interacting with IC 1727. The two are 88,000 light-years apart and lie around 18 million light-years away.[34] These two plus another four nearby dwarf irregular galaxies constitute the NGC 672 group, and all six appear to have had a burst of star formation in the last ten million years. The group is thought connected to another group of six galaxies known as the NGC 784 group, named for its principal galaxy, the barred spiral NGC 784. Together with two isolated dwarf galaxies, these fourteen appear to be moving in a common direction and constitute a group possibly located on a dark matter filament.[35] 3C 48 was the first quasar ever to be observed, although its true identity was not uncovered until after that of 3C 273 in 1963.[36] It has an apparent magnitude of 16.2 and is located about 5 degrees northwest of Alpha Trianguli.[14]

See also

  • Triangulum (Chinese astronomy)

References

  1. ↑ 1.0 1.1 1.2 "Triangulum, Constellation Boundary". The Constellations. International Astronomical Union. https://www.iau.org/public/themes/constellations/#tri. 
  2. ↑ Rogers, John H. (1998). "Origins of the Ancient Constellations: I. The Mesopotamian Traditions". Journal of the British Astronomical Association 108: 9–28. Bibcode: 1998JBAA..108....9R. 
  3. ↑ 3.0 3.1 3.2 3.3 Allen, Richard Hinckley (1963). Star Names: Their Lore and Meaning (Reprint ed.). New York, New York: Dover Publications Inc.. pp. 414–15. ISBN 0-486-21079-0. 
  4. ↑ 4.0 4.1 Ian Ridpath. "Triangulum". self-published. http://www.ianridpath.com/startales/triangulum.html. 
  5. ↑ 5.0 5.1 5.2 5.3 Garfinkle, Robert A. (1997). Star-Hopping: Your Visa to Viewing the Universe. Cambridge, United Kingdom: Cambridge University Press. p. 238. ISBN 0-521-59889-3. https://books.google.com/books?id=40JzBYGREL0C&pg=PA238. 
  6. ↑ Olcott, William Tyler (2004). Star Lore: Myths, Legends, and Facts. Mineola, New York: Courier Dover Publications. pp. 22–23. ISBN 978-0-486-43581-7. 
  7. ↑ Ian Ridpath. "Triangulum Minus". self-published. http://www.ianridpath.com/startales/triangulumminus.html. 
  8. ↑ Simpson, L. Phil (2012). Guidebook to the Constellations: Telescopic Sights, Tales, and Myths. New York, New York: Springer. p. 417. ISBN 978-1-4419-6941-5. https://books.google.com/books?id=7gde2t9ta4QC&q=delta+triangulum&pg=PA417. 
  9. ↑ Russell, Henry Norris (1922). "The New International Symbols for the Constellations". Popular Astronomy 30: 469–71. Bibcode: 1922PA.....30..469R. 
  10. ↑ 10.0 10.1 Bagnall, Philip M. (2012). The Star Atlas Companion: What You Need to Know about the Constellations. New York, New York: Springer. p. 436. ISBN 978-1-4614-0830-7. https://books.google.com/books?id=KcIg02TKW6QC&pg=PA436. 
  11. ↑ 11.0 11.1 Wagman, Morton (2003). Lost Stars: Lost, Missing and Troublesome Stars from the Catalogues of Johannes Bayer, Nicholas Louis de Lacaille, John Flamsteed, and Sundry Others. Blacksburg, Virginia: The McDonald & Woodward Publishing Company. pp. 301–02, 348. ISBN 978-0-939923-78-6. 
  12. ↑ "Beta Trianguli". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Beta+trianguli&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id. 
  13. ↑ Kennedy, G. M.; Wyatt, M. C.; Sibthorpe, B.; Phillips, N. M.; Matthews, B.; Greaves, J. S. (2012). "Coplanar Circumbinary Debris Disks". Monthly Notices of the Royal Astronomical Society 426 (3): 2115–28. doi:10.1111/j.1365-2966.2012.21865.x. Bibcode: 2012MNRAS.426.2115K. 
  14. ↑ 14.0 14.1 14.2 Motz, Lloyd; Nathanson, Carol (1991). The Constellations: An Enthusiast's Guide to the Night Sky. London, United Kingdom: Aurum Press. pp. 310–12. ISBN 1-85410-088-2. 
  15. ↑ "Gamma Trianguli". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Gamma+Trianguli&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id. 
  16. ↑ Rhee, Joseph H.; Song, Inseok; Zuckerman, B.; McElwain, Michael (May 2007), "Characterization of Dusty Debris Disks: The IRAS and Hipparcos Catalogs", The Astrophysical Journal 660 (2): 1556–71, doi:10.1086/509912, Bibcode: 2007ApJ...660.1556R 
  17. ↑ Kaler, Jim. "Delta Trianguli". Stars. University of Illinois. http://stars.astro.illinois.edu/sow/deltatri.html. 
  18. ↑ "7 Trianguli". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=7+Trianguli&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id. 
  19. ↑ Burnham, Robert Jr. (1978). Burnham's Celestial Handbook. New York, New York: Dover Publications. ISBN 0-486-24065-7. https://archive.org/details/burnhamscelestia02robe. 
  20. ↑ 20.0 20.1 Levy, David H. (2005). David Levy's Guide to Variable Stars. Cambridge, United Kingdom: Cambridge University Press. p. 227. ISBN 0-521-60860-0. https://books.google.com/books?id=Df9d8FBagqEC&q=%22X+trianguli%22&pg=PA227. 
  21. ↑ Groot, Paul J.; Rutten, Rene G.M.; van Paradijs, Jan (2004). "A Spectrophotometric Study of RW Trianguli". Astronomy & Astrophysics 417: 283–91. doi:10.1051/0004-6361:20031771. Bibcode: 2004A&A...417..283G. 
  22. ↑ "R Trianguli – Variable Star of Mira Ceti type". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=R+Tri&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id. 
  23. ↑ "XX Trianguli – Variable of RS CVn type". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=HD+12545&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id. 
  24. ↑ Strassmeier, K. G (1999). "Doppler imaging of stellar surface structure. XI. The super starspots on the K0 giant HD 12545: Larger than the entire Sun". Astronomy and Astrophysics 347: 225. Bibcode: 1999A&A...347..225S. 
  25. ↑ Hébrard, Guillaume; Bonfils, Xavier; Ségransan, Damien; Moutou, Claire; Delfosse, Xavier; Bouchy, François; Boisse, Isabelle; Arnold, Luc (2010). "The SOPHIE Search for Northern Extrasolar Planets: II. A Multi-planet System Around HD 9446". Astronomy & Astrophysics 513: A69. doi:10.1051/0004-6361/200913790. Bibcode: 2010A&A...513A..69H. http://www.aanda.org/articles/aa/full_html/2010/05/aa13790-09/aa13790-09.html. 
  26. ↑ Hatzes, A. P.; Guenther, E. W.; Endl, M.; Cochran, W. D.; Döllinger, M. P.; Bedalov, A. (2005). "A giant planet around the massive giant star HD 13189". Astronomy and Astrophysics 437 (2): 743–51. doi:10.1051/0004-6361:20052850. Bibcode: 2005A&A...437..743H. http://www.aanda.org/articles/aa/pdf/2005/26/aa2850-05.pdf. 
  27. ↑ "The peculiar asymmetry of NGC 949". http://www.spacetelescope.org/images/potw1518a/. 
  28. ↑ Fodera-Serio, G.; Indorato, L.; Nastasi, P. (February 1985). "Hodierna's Observations of Nebulae and his Cosmology". Journal for the History of Astronomy 16 (1): 1–36. doi:10.1177/002182868501600101. Bibcode: 1985JHA....16....1F. 
  29. ↑ Pawlowski, Marcel S.; Kroupa, Pavel; Jerjen, Helmut (2013). "Dwarf Galaxy Planes: the Discovery of Symmetric Structures in the Local Group". Monthly Notices of the Royal Astronomical Society 435 (3): 1928. doi:10.1093/mnras/stt1384. Bibcode: 2013MNRAS.435.1928P. 
  30. ↑ Brunthaler, Andreas; Reid, Mark J.; Falcke, Heino; Greenhill, Lincoln J. et al. (2005). "The Geometric Distance and Proper Motion of the Triangulum Galaxy (M33)". Science 307 (5714): 1440–1443. doi:10.1126/science.1108342. PMID 15746420. Bibcode: 2005Sci...307.1440B. 
  31. ↑ Nemiroff, R.; Bonnell, J., eds (16 August 1996). "NGC 604: Giant Stellar Nursery in M33". Astronomy Picture of the Day. NASA. https://apod.nasa.gov/apod/ap960816.html. 
  32. ↑ Ho, Luis C.; Filippenko, Alexei V.; Sargent, Wallace L. W. (October 1997). "A Search for "Dwarf" Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies". Astrophysical Journal Supplement 112 (2): 315–390. doi:10.1086/313041. Bibcode: 1997ApJS..112..315H. 
  33. ↑ "A distorted duo". https://www.spacetelescope.org/images/potw1733a/. 
  34. ↑ Block, Adam (20 October 2003). "NGC 672". National Optical Astronomy Observatory. http://www.noao.edu/outreach/aop/observers/n672.html. 
  35. ↑ Zitrin, Adi; Brosch, Noah (2008). "The NGC 672 and 784 galaxy groups: evidence for galaxy formation and growth along a nearby dark matter filament". Monthly Notices of the Royal Astronomical Society 390 (1): 408–20. doi:10.1111/j.1365-2966.2008.13786.x. Bibcode: 2008MNRAS.390..408Z. 
  36. ↑ Robertson, Peter (1992). Beyond Southern Skies: Radio Astronomy and the Parkes Telescope. Cambridge, United Kingdom: Cambridge University Press. p. 234. ISBN 0-521-41408-3. https://books.google.com/books?id=OBOY2G_3BCgC&q=3C+48&pg=PA234. 

External links

Coordinates: Sky map 02h 00m 00s, +30° 00′ 00″



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