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Ara (constellation)

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Ara
Constellation
Ara
List of stars in Ara
AbbreviationAra[1]
GenitiveArae[1]
Pronunciation/ˈɛərə/, genitive /ˈɛəriː/[a]
Symbolismthe Altar[1]
Right ascension16h 34m 16.9497s–18h 10m 41.3407s[2]
Declination−45.4859734°–−67.6905823°[2]
Area237 sq. deg. (63rd)
Main stars8[1]
Bayer/Flamsteed
stars		17
Stars with planets7
Stars brighter than 3.00m2
Stars within 10.00 pc (32.62 ly)3
Brightest starβ Ara (2.84m)
Messier objects0
Meteor showers0
Bordering
constellations
Visible at latitudes between +25° and −90°.
Best visible at 21:00 (9 p.m.) during the month of July.

Ara (Latin for "the Altar") is a southern constellation between Scorpius, Telescopium, Triangulum Australe, and Norma. It was (as Βωμός, Bōmǒs) one of the Greek bulk (namely 48) described by the 2nd-century astronomer Ptolemy, and it remains one of the 88 modern constellations designated by the International Astronomical Union.

The orange supergiant Beta Arae, to us its brightest star measured with near-constant apparent magnitude of 2.85, is marginally brighter than blue-white Alpha Arae. Seven star systems are known to host planets. Sunlike Mu Arae hosts four known planets. Gliese 676 is a (gravity-paired) binary red dwarf system with four known planets.

The Milky Way crosses the northwestern part of Ara. Within the constellation is Westerlund 1, a super star cluster that contains the red supergiant Westerlund 1-26, one of the largest stars known.

History

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In ancient Greek mythology, Ara was identified as the altar where the gods first made offerings and formed an alliance before defeating the Titans.[1] One of the southernmost constellations depicted by Ptolemy,[3] it had been recorded by Aratus in 270 BC as lying close to the horizon, and the Almagest portrays stars as far south as Gamma Arae. Professor Bradley Schaefer proposes such Ancients must have been able to see as far south as Zeta Arae, for a pattern that looked like an altar.[4]

Johann Elert Bode's illustration of Ara, from his Uranographia (1801)

In illustrations, Ara is usually depicted as compact classical altar with its smoke 'rising' southward.[5] However, depictions often vary. In the early days of printing, a 1482 woodcut of Gaius Julius Hyginus's classic Poeticon Astronomicon depicts the altar as surrounded by demons.[6] Johann Bayer in 1603 depicted Ara as an altar with burning incense. Indeed, frankincense burners were common throughout the Levant especially in the Yemen, where they are known as Mabkhara. This required live coals or burning embers called Jamra', in order to burn the incense. Willem Blaeu, a Dutch uranographer of the 16th and 17th centuries, drew Ara as an altar for sacrifices, with a burning animal offering unusually whose smoke rises northward, represented by Alpha Arae.

The Castle of Knowledge by Robert Record of 1556 lists the constellation stating that "Under the Scorpions tayle, standeth the Altar.";[7] a decade later a translation of a fairly recent mainly astrological work by Marcellus Palingenius of 1565, by Barnabe Googe states "Here mayst thou both the Altar, and the myghty Cup beholde."[8]

Equivalents

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In Chinese astronomy, the stars of the constellation Ara lie within The Azure Dragon of the East (東方青龍, Dōng Fāng Qīng Lóng).[9] Five stars of Ara formed Guī (龜), a tortoise, while another three formed Chǔ (杵), a pestle.

The Wardaman people of the Northern Territory in Australia saw the stars of Ara and the neighbouring constellation Pavo as flying foxes.[10]

Characteristics

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Covering 237.1 square degrees and hence 0.575% of the sky, Ara ranks 63rd of the 88 modern constellations by area.[11] Its position in the Southern Celestial Hemisphere means that the whole constellation is visible to observers south of 22°N.[11][b] Scorpius runs along the length of its northern border, while Norma and Triangulum Australe border it to the west, Apus to the south, and Pavo and Telescopium to the east respectively. The three-letter abbreviation for the constellation, as adopted by the International Astronomical Union, is "Ara".[12] The official constellation boundaries, as set by Belgian astronomer Eugène Delporte in 1930,[c] are defined by a polygon of twelve segments. In the equatorial coordinate system, the right ascension coordinates of these borders lie between 16h 36.1m and 18h 10.4m , while the declination coordinates are between −45.49° and −67.69°.[2]

Features

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

Stars

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See also: List of stars in Ara

Bayer gave eight stars Bayer designations, labelling them Alpha through to Theta, though he had never seen the constellation directly as it never rises above the horizon in Germany. After charting the southern constellations, French astronomer Nicolas-Louis de Lacaille recharted the stars of Ara from Alpha through to Sigma, including three pairs of stars next to each other as Epsilon, Kappa and Nu.[14]

Ara contains part of the Milky Way to the south of Scorpius and thus has rich star fields.[1] Within the constellation's borders, there are 71 stars brighter than or equal to apparent magnitude 6.5.[d][11]

Beta Arae, apparent magnitude 2.85, is the brightest star in the constellation, about 0.1 mag brighter than Alpha Arae although the difference in brightness between the two is undetectable by the unaided eye.[16] Beta is an orange-hued star of spectral type K3Ib-IIa that has been classified as a supergiant or bright giant,[17] and lies around 650 light-years from Earth.[18] It is over 8 times as massive and 5,636 times as luminous as the Sun.[19] Close to Beta Arae is Gamma Arae, a blue-hued supergiant of spectral type B1Ib. Of apparent magnitude 3.3, it is 1110 ± 60 light-years from Earth.[18] It has been estimated to be between 12.5 and 25 times as massive as the Sun,[20][21] and have around 120,000 times its luminosity.[21]

Alpha Arae is a blue-white main sequence star of magnitude 2.95, that is 270 ± 20 light-years from Earth.[18] This star is around 9.6 times as massive as the Sun,[22] and has an average of 4.5 times its radius.[23] It is 5,800 times as luminous as the Sun,[22] its energy emitted from its outer envelope at an effective temperature of 18,044 K.[23] A Be star, Alpha Arae is surrounded by a dense equatorial disk of material in Keplerian (rather than uniform) rotation. The star is losing mass by a polar stellar wind with a terminal velocity of approximately 1,000 km/s.[22][24]

The third brightest star in Ara at magnitude 3.13 is Zeta Arae,[25] an orange giant of spectral type K3III that is located 490 ± 10 light-years from Earth.[18] Around 7–8 times as massive as the Sun, it has swollen to a diameter around 114 times that of the Sun and is 3800 times as luminous.[26] Were it not dimmer by intervening interstellar dust, it would be significantly brighter at magnitude 2.11.[25]

Delta Arae is a blue-white main sequence star of spectral type B8Vn and magnitude 3.6, 198 ± 4 light-years from Earth.[18] It is around 3.56 times as massive as the Sun.[27]

Epsilon1 Arae is an orange giant of apparent magnitude 4.1, 360 ± 10 light-years distant from Earth.[18] It is around 74% more massive than the Sun. At an age of about 1.7 billion years, the outer envelope of the star has expanded to almost 34 times the Sun's radius.[28]

Eta Arae is an orange giant of apparent magnitude 3.76, located 299 ± 5 light-years distant from Earth.[18] Estimated to be around five billion years old, it has reached the giant star stage of its evolution. With 1.12 times the mass of the Sun, it has an outer envelope that has expanded to 40 times the Sun's radius.[29] The star is now spinning so slowly that it takes more than eleven years to complete a single rotation.[30]

GX 339-4 (V821 Arae) is a moderately strong variable galactic low-mass X-ray binary (LMXB) source[31][32] and black-hole candidate that flares from time to time. From spectroscopic measurements, the mass of the black-hole was found to be at least of 5.8 solar masses.[33]

Exoplanets have been discovered in seven star systems in the constellation.[34] Mu Arae (Cervantes[35]) is a sunlike star that hosts four planets.[36] HD 152079 is a sunlike star with a jupiter-like planet with an orbital period of 2097 ± 930 days.[37] HD 154672 is an ageing sunlike star with a Hot Jupiter. HD 154857 is a sunlike star with one confirmed and one suspected planet. HD 156411 is a star hotter and larger than the sun with a gas giant planet in orbit. Gliese 674 is a nearby red dwarf star with a planet. Gliese 676 is a binary star system composed of two red dwarves with four planets.

Deep-sky objects

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IC 4653 galaxy taken by Hubble.[38]

The northwest corner of Ara is crossed by the galactic plane of the Milky Way and contains several open clusters (notably NGC 6200) and diffuse nebulae (including the bright cluster/nebula pair NGC 6188 and NGC 6193). The brightest of the globular clusters, sixth magnitude NGC 6397, lies at a distance of just 6,500 light-years (6.1×1016 km), making it one of the closest globular clusters to the Solar System.[39]

Ara also contains Westerlund 1, a super star cluster containing itself the possible red supergiant Westerlund 1-237 and the red supergiant Westerlund 1-26. The latter is one of the largest stars known with an estimate varying between 1,168 R☉[40] and 2,519 R☉.[41]

Although Ara lies close to the heart of the Milky Way, two spiral galaxies (NGC 6215 and NGC 6221) are visible near star Eta Arae.[39]

Open clusters

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Globular clusters

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  • NGC 6352
  • NGC 6362
  • NGC 6397 is a globular cluster with an overall magnitude of 6.0; it is visible to the naked eye under exceptionally dark skies and is normally visible in binoculars. It is a fairly close globular cluster, at a distance of 10,500 light-years.[1]

Planetary Nebulae

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  • The Stingray Nebula (Hen 3–1357), the youngest known planetary nebula as of 2010, formed in Ara; the light from its formation was first observable around 1987.
  • NGC 6326. A planetary nebula that might have a binary system at its center.

Notes

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  1. ^ Random House Dictionary
  2. ^ Although parts of the constellation technically rise above the horizon to observers between the 22°N and 44°N, stars within a few degrees of the horizon are to all intents and purposes unobservable.[11]
  3. ^ Delporte had proposed standardising the constellation boundaries to the International Astronomical Union, who had agreed and gave him the lead role[13]
  4. ^ Objects of magnitude 6.5 are among the faintest visible to the unaided eye in suburban-rural transition night skies.[15]

References

[edit]
  1. ^ a b c d e f g h Ridpath & Tirion 2001, pp. 82–83.
  2. ^ a b c "Ara, constellation boundary". The Constellations. Retrieved 14 February 2014.
  3. ^ Barentine, John C. (23 November 2015). "Officina Typographica". The Lost Constellations. Springer. p. 13. ISBN 978-3-319-22794-8.
  4. ^ Schaefer, Bradley E. (2002). "The latitude and epoch for the formation of the southern Greek constellations". Journal for the History of Astronomy. 4. 33 (113): 313–50. Bibcode:2002JHA....33..313S. doi:10.1177/002182860203300401. ISSN 0021-8286. S2CID 122459258.
  5. ^ Ridpath, Star Tales Ara.
  6. ^ Kanas, Nick (2012). History, Artistry, and Cartography (Second ed.). Chichester, U.K.: Praxis Publishing. p. 136. doi:10.1007/978-1-4614-0917-5. ISBN 978-1-4614-0916-8. S2CID 239353025.
  7. ^ The Castle of Knowledge containing the Explication of the Sphere both Celestiall and Materiall, etc., 1st edition, 1556; Robert Record, London; R. Wolfe (printer) STC 20796
  8. ^ The zodiake of life written by the godly and zealous poet Marcellus Palingenius Stellatus, wherein are conteyned twelve bookes, new edition, 1565 (1 vol.); Barnabe Googe, London; Henry Denham (printer), for Rafe Newberye dwelling in Fleete streate, Anno. 1565. Aprilis. 18; STC 1915
  9. ^ AEEA 2006.
  10. ^ Harney, Bill Yidumduma; Cairns, Hugh C. (2004) [2003]. Dark Sparklers (Revised ed.). Merimbula, New South Wales: Hugh C. Cairns. p. 201. ISBN 978-0-9750908-0-0.
  11. ^ a b c d Ridpath, Ian. "Constellations: Andromeda–Indus". Star Tales. self-published. Retrieved 18 September 2016.
  12. ^ Russell, Henry Norris (1922). "The New International Symbols for the Constellations". Popular Astronomy. 30: 469. Bibcode:1922PA.....30..469R.
  13. ^ Ridpath, Ian. "Constellation boundaries: How the modern constellation outlines came to be". Star Tales. self-published. Retrieved 18 September 2016.
  14. ^ Wagman 2003, pp. 42–43.
  15. ^ Bortle, John E. (February 2001). "The Bortle Dark-Sky Scale". Sky & Telescope. Retrieved 26 August 2015.
  16. ^ Kaler, James B. "BETA ARA (Beta Arae)". Stars. University of Illinois. Retrieved 17 September 2016.
  17. ^ De Medeiros, J. R.; Udry, S.; Burki, G.; Mayor, M. (November 2002). "A catalog of rotational and radial velocities for evolved stars. II. Ib supergiant stars" (PDF). Astronomy and Astrophysics. 395: 97–98. Bibcode:2002A&A...395...97D. doi:10.1051/0004-6361:20021214. Archived (PDF) from the original on 2022-10-09.
  18. ^ a b c d e f g van Leeuwen, F. (November 2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–64. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600.
  19. ^ Heiter, U.; Jofré, P.; Gustafsson, B.; Korn, A. J.; Soubiran, C.; Thévenin, F. (2015). "Gaia FGK benchmark stars: Effective temperatures and surface gravities". Astronomy & Astrophysics. 582: A49. arXiv:1506.06095. Bibcode:2015A&A...582A..49H. doi:10.1051/0004-6361/201526319. S2CID 53391939.
  20. ^ Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (2011). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society. 410 (1): 190–200. arXiv:1007.4883. Bibcode:2011MNRAS.410..190T. doi:10.1111/j.1365-2966.2010.17434.x. S2CID 118629873.
  21. ^ a b Lefever, K.; Puls, J.; Aerts, C. (March 2007). "Statistical properties of a sample of periodically variable B-type supergiants. Evidence for opacity-driven gravity-mode oscillations". Astronomy and Astrophysics. 463 (3): 1093–1109. arXiv:astro-ph/0611484. Bibcode:2007A&A...463.1093L. doi:10.1051/0004-6361:20066038. S2CID 8783008.
  22. ^ a b c Meilland, A.; et al. (March 2007). "First direct detection of a Keplerian rotating disk around the Be star α Arae using AMBER/VLTI". Astronomy and Astrophysics. 464 (1): 59–71. arXiv:astro-ph/0606404. Bibcode:2007A&A...464...59M. doi:10.1051/0004-6361:20064848. S2CID 55225830.. See Tables 1 and 4 for parameters of the star, circumstellar disk, and polar winds.
  23. ^ a b Meilland, A.; Stee, Ph.; Chesneau, O.; Jones, C. (2009). "VLTI/MIDI observations of 7 classical Be stars". Astronomy and Astrophysics. 505 (2): 687–93. arXiv:0908.1239. Bibcode:2009A&A...505..687M. doi:10.1051/0004-6361/200911960. S2CID 12694072.
  24. ^ Chesneau, O.; Meilland, A.; Rivinius, T.; Stee, Ph.; Jankov, S.; Domiciano de Souza, A.; Graser, U.; Herbst, T.; Janot-Pacheco, E.; Koehler, R.; Leinert, C.; Morel, S.; Paresce, F.; Richichi, A.; Robbe-Dubois, S. (2005). "First VLTI/MIDI observations of a Be star: Alpha Arae". Astronomy and Astrophysics. 435 (1): 275–287. arXiv:astro-ph/0501162. Bibcode:2005A&A...435..275C. doi:10.1051/0004-6361:20041954. S2CID 16747094.
  25. ^ a b Kaler, Jim (13 July 2012). "Zeta Arae". Stars. University of Illinois. Retrieved 12 September 2019.
  26. ^ Cruzalèbes, P.; Jorissen, A.; Rabbia, Y.; Sacuto, S.; Chiavassa, A.; Pasquato, E.; Plez, B.; Eriksson, K.; Spang, A.; Chesneau, O. (2013). "Fundamental parameters of 16 late-type stars derived from their angular diameter measured with VLTI/AMBER". Monthly Notices of the Royal Astronomical Society. 434 (1): 437. arXiv:1306.3288. Bibcode:2013MNRAS.434..437C. doi:10.1093/mnras/stt1037. S2CID 49573767.
  27. ^ Shaya, Ed J.; Olling, Rob P. (January 2011). "Very Wide Binaries and Other Comoving Stellar Companions: A Bayesian Analysis of the Hipparcos Catalogue". The Astrophysical Journal Supplement. 192 (1): 2. arXiv:1007.0425. Bibcode:2011ApJS..192....2S. doi:10.1088/0067-0049/192/1/2. S2CID 119226823.
  28. ^ da Silva, L.; Girardi, L.; Pasquini, L.; Setiawan, J.; von der Lühe, O.; de Medeiros, J. R.; Hatzes, A.; Döllinger, M. P.; Weiss, A. (November 2006). "Basic physical parameters of a selected sample of evolved stars". Astronomy and Astrophysics. 458 (2): 609–623. arXiv:astro-ph/0608160. Bibcode:2006A&A...458..609D. doi:10.1051/0004-6361:20065105. S2CID 9341088.
  29. ^ Jofré, E.; Petrucci, R.; Saffe, C.; Saker, L.; de la Villarmois, E. Artur; Chavero, C.; Gómez, M.; Mauas, P. J. D. (2015). "Stellar parameters and chemical abundances of 223 evolved stars with and without planets". Astronomy & Astrophysics. 574: A50. arXiv:1410.6422. Bibcode:2015A&A...574A..50J. doi:10.1051/0004-6361/201424474. S2CID 53666931.
  30. ^ Setiawan, J.; Pasquini, L.; da Silva, L.; Hatzes, A. P.; von der Lühe, O.; Girardi, L.; de Medeiros, J. R.; Guenther, E. (July 2004). "Precise radial velocity measurements of G and K giants. Multiple systems and variability trend along the Red Giant Branch". Astronomy and Astrophysics. 421: 241–254. Bibcode:2004A&A...421..241S. doi:10.1051/0004-6361:20041042-1.
  31. ^ SIMBAD
  32. ^ Bradt, H.V.D., and McClintock, J.E., Annu. Rev. Astron. Astrophys., 21, 13-66 (1983)
  33. ^ Hynes, R. I.; Steeghs, D.; Casares, J.; Charles, P. A.; O'Brien, K. (February 2003). "Dynamical Evidence for a Black Hole in GX 339-4". The Astrophysical Journal. 583 (2, pp. L95–L98): L95–L98. arXiv:astro-ph/0301127. Bibcode:2003ApJ...583L..95H. doi:10.1086/368108. S2CID 16820881.
  34. ^ Bagnall, Philip M. (2012). The Star Atlas Companion : What You Need to Know about the Constellations. New York: Springer. pp. 50–54. ISBN 9781461408307. OCLC 794225463.
  35. ^ "Naming Stars". IAU.org. Retrieved 30 July 2018.
  36. ^ Pepe, F.; Correia, A. C. M.; Mayor, M.; Tamuz, O.; Benz, W.; Bertaux, J. -L.; Bouchy, F.; Couetdic, J.; Laskar, J.; Lovis, C.; Naef, D.; Queloz, D.; Santos, N. C.; Sivan, J. -P.; Sosnowska, D.; Udry, S. (2006). "The HARPS search for southern extra-solar planets. IX. μ Ara, a system with four planets". Astronomy and Astrophysics. 462 (2): 769–776. arXiv:astro-ph/0608396. Bibcode:2007A&A...462..769P. doi:10.1051/0004-6361:20066194. S2CID 119071803.
  37. ^ Arriagada, Pamela; et al. (2010). "Five Long-period Extrasolar Planets in Eccentric orbits from the Magellan Planet Search Program". The Astrophysical Journal. 711 (2): 1229–35. arXiv:1001.4093. Bibcode:2010ApJ...711.1229A. doi:10.1088/0004-637X/711/2/1229. S2CID 118682009.
  38. ^ "A Familiar Sight". www.spacetelescope.org. Retrieved 23 October 2019.
  39. ^ a b Dunlop 2005.
  40. ^ Arévalo, Aura (2019). The Red Supergiants in the Supermassive Stellar Cluster Westerlund 1 (Master's thesis). University of São Paulo. doi:10.11606/D.14.2019.tde-12092018-161841.
  41. ^ Fok, Thomas K. T.; Nakashima, Jun-ichi; Yung, Bosco H. K.; Hsia, Chih-Hao; Deguchi, Shuji (2012). "Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters". The Astrophysical Journal. 760 (1): 65. arXiv:1209.6427. Bibcode:2012ApJ...760...65F. doi:10.1088/0004-637X/760/1/65. S2CID 53393926.

Bibliography

[edit]
  • Dunlop, Storm (2005). Atlas of the Night Sky. Collins. ISBN 978-0-00-717223-8.
  • Ridpath, Ian; Tirion, Wil (2001). Stars and Planets Guide. Princeton University Press. ISBN 978-0-691-08913-3.
  • Ridpath, Ian; Tirion, Wil (2007). Stars and Planets Guide (4th ed.). Princeton University Press. ISBN 978-0-691-13556-4.
  • Staal, Julius D.W. (1988). The New Patterns in the Sky. McDonald and Woodward Publishing Company. ISBN 978-0-939923-04-5.
  • 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, VA: The McDonald & Woodward Publishing Company. ISBN 978-0-939923-78-6.

Online sources

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