Phoenix (constellation)

Coordinates: Sky map 00h 00m 00s, −50° 00′ 00″
Source: Wikipedia, the free encyclopedia.

Phoenix
Constellation
Phoenix
List of stars in Phoenix
AbbreviationPhe
GenitivePhoenicis
Pronunciation
Symbolismthe
37th)
Main stars4
Bayer/Flamsteed
stars		25
Stars with planets10
Stars brighter than 3.00m1
Stars within 10.00 pc (32.62 ly)1
Brightest starα Phe (Ankaa) (2.40m)
Messier objects0
Meteor showersPhoenicids
Bordering
constellations
Visible at latitudes between +32° and −80°.
Best visible at 21:00 (9 p.m.) during the month of November.

Phoenix is a minor

Nicolas Louis de Lacaille charted the brighter stars and gave their Bayer designations in 1756. The constellation stretches from roughly −39° to −57° declination, and from 23.5h to 2.5h of right ascension. The constellations Phoenix, Grus, Pavo and Tucana
, are known as the Southern Birds.

The brightest star,

visible universe. Phoenix is the radiant of two annual meteor showers: the Phoenicids
in December, and the July Phoenicids.

History

The constellation Phoenix as depicted in Johann Gabriel Doppelmayr's Atlas Coelestis, ca. 1742
The "southern birds", as depicted in Johann Bayer's Uranometria. Phoenix is on the lower left.

Phoenix was the largest of the 12 constellations established by

Arabic: العنقاء, romanized: al-‘anqā’, lit. 'the phoenix', and was coined sometime after 1800 in relation to the constellation.[5]

Celestial historian Richard Allen noted that unlike the other constellations introduced by Plancius and

La Caille, Phoenix has actual precedent in ancient astronomy, as the Arabs saw this formation as representing young ostriches, Al Ri'āl, or as a griffin or eagle.[6] In addition, the same group of stars was sometimes imagined by the Arabs as a boat, Al Zaurak, on the nearby river Eridanus.[7] He observed, "the introduction of a Phoenix into modern astronomy was, in a measure, by adoption rather than by invention."[6]

The Chinese incorporated Phoenix's brightest star, Ankaa (Alpha Phoenicis), and stars from the adjacent constellation Sculptor to depict Bakui, a net for catching birds.[4] Phoenix and the neighbouring constellation of Grus together were seen by Julius Schiller as portraying Aaron the High Priest.[6] These two constellations, along with nearby Pavo and Tucana, are called the Southern Birds.[8]

Characteristics

Phoenix is a small constellation bordered by Fornax and Sculptor to the north, Grus to the west, Tucana to the south, touching on the corner of Hydrus to the south, and Eridanus to the east and southeast. The bright star Achernar is nearby.[9] The three-letter abbreviation for the constellation, as adopted by the International Astronomical Union in 1922, is "Phe".[10] The official constellation boundaries, as set by Belgian astronomer Eugène Delporte in 1930, are defined by a polygon of 10 segments. In the equatorial coordinate system, the right ascension coordinates of these borders lie between 23h 26.5m and 02h 25.0m , while the declination coordinates are between −39.31° and −57.84°.[1] This means it remains below the horizon to anyone living north of the 40th parallel in the Northern Hemisphere, and remains low in the sky for anyone living north of the equator. It is most visible from locations such as Australia and South Africa during late Southern Hemisphere spring.[7] Most of the constellation lies within, and can be located by, forming a triangle of the bright stars Achernar, Fomalhaut and Beta Ceti—Ankaa lies roughly in the centre of this.[11]

Features

The constellation Phoenix as it can be seen by the naked eye

Stars

Further information: List of stars in Phoenix

A curved line of stars comprising Alpha,

Nicolas Louis de Lacaille charted and designated 27 stars with the Bayer designations Alpha through to Omega in 1756. Of these, he labelled two stars close together Lambda, and assigned Omicron, Psi and Omega to three stars, which subsequent astronomers such as Benjamin Gould felt were too dim to warrant their letters. A different star was subsequently labelled Psi Phoenicis, while the other two designations fell out of use.[12]

Ankaa is the brightest star in the constellation. It is an orange giant of

apparent visual magnitude 2.37 and spectral type K0.5IIIb,[13] 77 light years distant from Earth and orbited by a secondary object about which little is known.[14] Lying close by Ankaa is Kappa Phoenicis, a main sequence star of spectral type A5IVn and apparent magnitude 3.90.[15] Located centrally in the asterism,[7] Beta Phoenicis is the second brightest star in the constellation and another binary star. Together the stars, both yellow giants of spectral type G8, shine with an apparent magnitude of 3.31, though the components are of individual apparent magnitudes of 4.0 and 4.1 and orbit each other every 168 years.[16] Zeta Phoenicis or Wurren[17] is an Algol-type eclipsing binary, with an apparent magnitude fluctuating between 3.9 and 4.4 with a period of around 1.7 days (40 hours); its dimming results from the component two blue-white B-type stars, which orbit and block out each other from Earth. The two stars are 0.05 AU from each other, while a third star is around 600 AU away from the pair, and has an orbital period exceeding 5000 years.[18] The system is around 300 light years distant.[19] In 1976, researchers Clausen, Gyldenkerne, and Grønbech calculated that a nearby 8th magnitude star is a fourth member of the system.[20]

AI Phe is an eclipsing binary star identified in 1972. Its long mutual eclipses and combination of spectroscopic and astrometric data allows precise measurement of the masses and radii of the stars[21] which is viewed as a potential cross-check on stellar properties and distances independent on Ceiphid Variables and such techniques. The long eclipse events require space-based observations to avoid Solar interference. Gamma Phoenicis is a

astroseismology.[30] Rho is spectral type F2III,[31] and ranges between magnitudes 5.20 and 5.26 over a period of 2.85 hours.[32] BD is of spectral type A1V,[33] and ranges between magnitudes 5.90 and 5.94.[34]

Earth's.[40]

Ten stars have been found to have planets to date, and four planetary systems have been discovered with the

SuperWASP project. HD 142 is a yellow giant that has an apparent magnitude of 5.7, and has a planet (HD 142 b) 1.36 times the mass of Jupiter which orbits every 328 days.[41] HD 2039 is a yellow subgiant with an apparent magnitude of 9.0 around 330 light years away which has a planet (HD 2039 b) six times the mass of Jupiter. WASP-18 is a star of magnitude 9.29 which was discovered to have a hot Jupiter-like planet (WASP-18b) taking less than a day to orbit the star.[42] The planet is suspected to be causing WASP-18 to appear older than it really is.[43] WASP-4 and WASP-5 are solar-type yellow stars around 1000 light years distant and of 13th magnitude, each with a single planet larger than Jupiter.[44] WASP-29 is an orange dwarf of spectral type K4V and visual magnitude 11.3, which has a planetary companion of similar size and mass to Saturn. The planet completes an orbit every 3.9 days.[45]

WISE J003231.09-494651.4 and WISE J001505.87-461517.6 are two brown dwarfs discovered by the Wide-field Infrared Survey Explorer, and are 63 and 49 light years away respectively.[46] Initially hypothesised before they were belatedly discovered,[47] brown dwarfs are objects more massive than planets, but which are of insufficient mass for hydrogen fusion characteristic of stars to occur. Many are being found by sky surveys.[48]

Phoenix contains

HE0107-5240, possibly one of the oldest stars yet discovered. It has around 1/200,000 the metallicity that the Sun has and hence must have formed very early in the history of the universe.[49] With a visual magnitude of 15.17,[50] it is around 10,000 times dimmer than the faintest stars visible to the naked eye and is 36,000 light years distant.[49]

Deep-sky objects

The constellation does not lie on the

light-years) in diameter and about 12.9 billion years old.[52] Robert's Quartet (composed of the irregular galaxy NGC 87, and three spiral galaxies NGC 88, NGC 89 and NGC 92) is a group of four galaxies located around 160 million light-years away which are in the process of colliding and merging. They are within a circle of radius of 1.6 arcmin, corresponding to about 75,000 light-years.[53] Located in the galaxy ESO 243-49 is HLX-1, an intermediate-mass black hole—the first one of its kind identified. It is thought to be a remnant of a dwarf galaxy that was absorbed in a collision with ESO 243-49.[citation needed] Before its discovery, this class of black hole was only hypothesized.[54]

Lying within the bounds of the constellation is the gigantic

Phoenix cluster, which is around 7.3 million light years wide and 5.7 billion light years away, making it one of the most massive galaxy clusters. It was first discovered in 2010, and the central galaxy is producing an estimated 740 new stars a year.[55] Larger still is El Gordo, or officially ACT-CL J0102-4915, whose discovery was announced in 2012.[56] Located around 7.2 billion light years away, it is composed of two subclusters in the process of colliding, resulting in the spewing out of hot gas, seen in X-rays and infrared images.[57]

Meteor showers

Phoenix is the

short-period comet 289P/Blanpain. It peaks around 4–5 December, though is not seen every year.[58] A very minor meteor shower peaks around July 14 with around one meteor an hour, though meteors can be seen anytime from July 3 to 18; this shower is referred to as the July Phoenicids.[59]

See also

References

  1. ^ a b c "Phoenix, constellation boundary". The Constellations. International Astronomical Union. Retrieved 23 August 2012.
  2. ^ Ridpath, Ian. "Bayer's Southern Star Chart". self-published. Retrieved August 15, 2013.
  3. ^ Ridpath, Ian. "Frederick de Houtman's catalogue". self-published. Retrieved August 15, 2013.
  4. ^ a b Ridpath, Ian. "Phoenix – the Phoenix". self-published. Retrieved August 18, 2013.
  5. ISBN 978-1-931559-44-7
    .
  6. ^
    ISBN 978-0-486-21079-7. star names meaning phoenix.[permanent dead link
    ]
  7. ^
    ISBN 978-1-85410-088-7
    .
  8. ISBN 978-0521793902
    .
  9. ^
    ISBN 978-0-600-00893-4
    .
  10. Bibcode:1922PA.....30..469R
    .
  11. ISBN 978-1139461382
    .
  12. ISBN 978-0-939923-78-6
    .
  13. ^ "Alpha Phoenicis". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 25 August 2012.
  14. ^ Kaler, Jim. "Ankaa". Stars. University of Illinois. Retrieved 24 August 2012.
  15. ^ "Kappa Phoenicis". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 25 August 2012.
  16. ^ Kaler, Jim. "Beta Phoenicis". Stars. University of Illinois. Retrieved 24 August 2012.
  17. ^ "Naming Stars". IAU.org. Retrieved 16 December 2017.
  18. ^ Kaler, Jim. "Zeta Phoenicis". Stars. University of Illinois. Retrieved 18 June 2013.
  19. ^ "Zeta Phoenicis – Eclipsing binary of Algol type (detached)". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 4 September 2013.
  20. Bibcode:1976A&A....46..205C
    .
  21. S2CID 214605785
    .
  22. ^ "Gamma Phoenicis". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 25 August 2012.
  23. ^ Kaler, Jim. "Gamma Phoenicis". Stars. University of Illinois. Retrieved 23 August 2012.
  24. ^ a b "Psi Phoenicis – Semi-regular pulsating Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 12 May 2013.
  25. ^
    ISBN 978-1-4614-0830-7
    .
  26. S2CID 1586125
    .
  27. ^ "W Phe". International Variable Star Index. American Association of Variable Star Observers. 4 January 2010. Retrieved 19 June 2013.
  28. ISBN 978-0-486-24065-7
    .
  29. S2CID 122809222
    .
  30. ^ Templeton, Matthew (16 July 2010). "Delta Scuti and the Delta Scuti Variables". Variable Star of the Season. AAVSO (American Association of Variable Star Observers). Retrieved 19 June 2013.
  31. ^ "V* rho Phe – Variable Star of delta Sct type". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 26 August 2012.
  32. ^ "Rho Phe". International Variable Star Index. AAVSO. 4 January 2010. Retrieved 18 June 2013.
  33. ^ "V* BD Phe – Variable Star of delta Sct type". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 18 June 2013.
  34. ^ "BD Phe". International Variable Star Index. AAVSO. 4 January 2010. Retrieved 18 June 2013.
  35. ^ "LHS 1220 – High proper-motion Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 11 May 2013.
  36. S2CID 53694238
    .
  37. S2CID 46328823
    .
  38. ^ "GJ 915 – White Dwarf". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 26 August 2012.
  39. ^ Johnson, J. (2007). "Extreme Stars: White Dwarfs & Neutron Stars". Lecture notes, Astronomy 162. Ohio State University. Retrieved 17 August 2013.
  40. S2CID 14696597
    .
  41. ^ Kaler, Jim. "HR 6 Phoenicis". Stars. University of Illinois. Retrieved 24 August 2012.
  42. S2CID 205217669
    .
  43. ^ "NASA's Chandra X-ray Observatory Finds Planet That Makes Star Act Deceptively Old". Chandra X-ray Observatory. Retrieved 20 September 2014.
  44. S2CID 53606165. Archived from the original
    on 2010-04-08.
  45. S2CID 64119308
    .
  46. S2CID 119279752
    .
  47. ^ Jameson, R.F.; Hodgkin, S.T. (1997). "Brown Dwarfs and Low Mass Stars". Brown Dwarfs. Leicester, United Kingdom: University of Leicester. Archived from the original on 2 June 2013. Retrieved 16 August 2013.
  48. ^ "Science: Brown Dwarfs". Wide-field Infrared Survey Explorer. NASA. 31 August 2011. Retrieved 16 August 2013.
  49. ^ a b Christlieb, Norbert (30 October 2002). "A Glimpse of the Young Milky Way: VLT UVES Observes Most Metal-Deficient Star Known". European Southern Observatory. Retrieved 26 July 2013.
  50. ^ "2MASS J01092916-5224341 – Carbon Star". SIMBAD Astronomical Database. Centre de Données astronomiques de Strasbourg. Retrieved 17 August 2013.
  51. ISBN 978-0-521-19876-9
    .
  52. ^ "NED results for NGC 37". NED via University of California. Retrieved 19 August 2013.
  53. ^ Boffin, Henri (4 November 2005). "eso0535 — Photo Release: Cosmic Portrait of a Perturbed Family". European Southern Observatory. Archived from the original on 11 October 2008. Retrieved 24 August 2012.
  54. ^ "Astronomers spot the very first intermediate-mass black hole". The Bunsen Burner. T.E. Holdings LLC. 9 July 2012. Archived from the original on 3 December 2013. Retrieved 15 August 2013.
  55. ^ Chu, Jennifer (15 August 2012). "Most massive and luminous galaxy cluster identified". MIT News. Cambridge, Massachusetts: Massachusetts Institute of Technology. Retrieved 25 August 2012.
  56. ^ Perrotto, Trent J.; Anderson, Janet; Watzke, Megan (10 January 2012). "NASA's Chandra Finds Largest Galaxy Cluster in Early Universe". NASA. Archived from the original on 1 May 2017. Retrieved 2 September 2013.
  57. ^ Chandra X-ray Observatory (10 January 2012). "El Gordo: NASA's Chandra Finds Largest Galaxy Cluster in Early Universe". NASA. Retrieved 2 September 2013.
  58. ISBN 978-0-521-85349-1
    .
  59. ISBN 978-0-521-69691-3
    .

External links

Media related to Phoenix (constellation) at Wikimedia Commons


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