Arcturus

For other uses, see Arcturus (disambiguation).
Arcturus

Arcturus in the constellation of Boötes.
Observation data
Epoch J2000      Equinox J2000
Constellation Boötes
Pronunciation /ɑːrkˈtjʊərəs/
Right ascension 14h 15m 39.7s[1]
Declination +19° 10′ 56″[1]
Apparent magnitude (V) −0.05[2]
Characteristics
Spectral type K0 III[3]
Apparent magnitude (J) −2.25[2]
U−B color index +1.28[2]
B−V color index +1.23[2]
R−I color index +0.65[2]
Note (category: variability): H and K emission vary.
Astrometry
Radial velocity (Rv)−5.19[4] km/s
Proper motion (μ) RA: −1093.45[5] mas/yr
Dec.: −1999.40[5] mas/yr
Parallax (π)88.83 ± 0.54[1] mas
Distance36.7 ± 0.2 ly
(11.26 ± 0.07 pc)
Absolute magnitude (MV)−0.30±0.02[6]
Details
Mass1.08±0.06[7] M☉
Radius25.4±0.2[7] R☉
Luminosity170[8] L☉
Surface gravity (log g)1.66±0.05[7] cgs
Temperature4286±30[7] K
Metallicity [Fe/H]−0.52±0.04[7] dex
Rotational velocity (v sin i)2.4±1.0[6] km/s
Age7.1+1.5
−1.2[7] Gyr
Other designations
Alramech, Abramech, α Boötis, 16 Boötes, BD+19°2777, GCTP 3242.00, GJ 541, HD 124897, HIP 69673, HR 5340, LHS 48, SAO 100944.
Database references
SIMBADdata
Data sources:
Hipparcos Catalogue,
CCDM (2002),
Bright Star Catalogue (5th rev. ed.),
VizieR catalog entry

Arcturus (/ɑːrkˈtjʊərəs/; α Boo, α Boötis, Alpha Boötis) of the constellation Boötes is the brightest star in the northern celestial hemisphere. With a visual magnitude of −0.05, it is the fourth brightest star in the night sky, after −1.46 magnitude Sirius, −0.86 magnitude Canopus, and −0.27 magnitude Alpha Centauri. It is a relatively close star at only 36.7 light-years from Earth, and, together with Vega and Sirius, one of the most luminous stars in the Sun's neighborhood.

Arcturus is a type K0 III orange giant star, with an absolute magnitude of −0.30. It has likely exhausted its hydrogen from its core and is now in its active hydrogen shell burning phase. It will continue to expand before entering horizontal branch stage of its life cycle.

Observational history

As one of the brightest stars in the sky, Arcturus has been significant to observers since antiquity. In Mesopotamia, it was linked to the god Enlil, and also known as Shudun, "yoke",[9] or SHU-PA of unknown derivation in the Three Stars Each Babylonian star catalogues and later MUL.APIN around 1100 BC.[10]

Ptolemy described Arcturus as subrufa "slightly red", and it has a B-V color index of +1.23, roughly midway between Pollux (B-V +1.00) and Aldebaran (B-V +1.54).[11]

Prehistoric Polynesian navigators knew Arcturus as Hōkūleʻa, the "Star of Joy". Arcturus is the zenith star of the Hawaiian Islands. Using Hōkūleʻa and other stars, the Polynesians launched their double-hulled canoes from Tahiti and the Marquesas Islands. Traveling east and north they eventually crossed the equator and reached the latitude at which Arcturus would appear directly overhead in the summer night sky. Knowing they had arrived at the exact latitude of the island chain, they sailed due west on the trade winds to landfall. If Hōkūleʻa could be kept directly overhead, they landed on the southeastern shores of the Big Island of Hawaiʻi. For a return trip to Tahiti the navigators could use Sirius, the zenith star of that island. Since 1976, the Polynesian Voyaging Society's Hōkūle‘a has crossed the Pacific Ocean many times under navigators who have incorporated this wayfinding technique in their non-instrument navigation.

The French mathematician and astronomer Jean-Baptiste Morin observed Arcturus in the daytime with a telescope (a first for any star other than the Sun and supernovae) in 1635, and Arcturus has been seen at or just before sunset with the naked eye.[11]

Based upon an annual parallax shift of 88.83 milliarcseconds as measured by the Hipparcos satellite,[1] Arcturus is 36.7 light-years (11.26 parsecs) from Earth—relatively close in astronomical terms. The margin of error is 0.54 milliarcseconds, translating to a margin of error of ±2.3 light-years (0.7 parsecs).[1]

Together with Spica and Denebola (or Regulus, depending on the source), Arcturus is part of the Spring Triangle asterism, and by extension, also of the Great Diamond after factoring in Cor Caroli.

Visibility

Arcturus has a visual magnitude of −0.05, making it the brightest star north of the celestial equator, and the fourth brightest star in the night sky.[12] However, Alpha Centauri is a bright binary star, whose unresolved components to the naked eye are both fainter than Arcturus. This makes Arcturus the third brightest individual star, just ahead of Alpha Centauri A (α Cen A), whose visual magnitude is −0.01.[11]

Arcturus is visible from both Earth's hemispheres as it is located 19° north of the celestial equator. The star culminates at midnight on 27 April, and at 9PM on June 10 being visible during the late northern spring or the southern autumn.[13] From the northern hemisphere, an easy way to find Arcturus is to follow the arc of the handle of the Big Dipper. By continuing in this path, one can find Spica, "Arc to Arcturus, then spike to Spica".

Eta Boötis, or Muphrid, is only 3.3 light-years distant from Arcturus, and would have a visual magnitude −2.5, whereas an observer on the former system would find Arcturus as bright as Venus as seen from Earth.[11]

Properties

Optical image of Arcturus (DSS2 / MAST / STScI / NASA)

Arcturus is a type K0 III red giant star. It is about 110 times brighter than the Sun in visible light wavelengths, but this underestimates its strength as much of the light it gives off is in the infrared; total (bolometric) power output is about 180 times that of the Sun. The lower output in visible light is due to a lower efficacy as the star has a lower surface temperature than the Sun. With a near-infrared J band magnitude of −2.2, only Betelgeuse (−2.9) and R Doradus (−2.6) are brighter.

As the brightest K-type giant in the sky, it was the subject of an atlas of its visible spectrum, made from photographic spectra taken with the coudé spectrograph of the Mt. Wilson 2.5m telescope published in 1968,[14] a key reference work for stellar spectroscopy. Subsequent spectral atlases [15] [16] [17] with greater wavelength coverage and superior signal-to-noise ratio made with digital detectors have supplanted the older work, but the Arcturus spectrum remains an important standard for stellar spectroscopy.

As a single star, the mass of Arcturus cannot be measured directly, but models suggest it is slightly larger than that of the Sun. Evolutionary matching to the observed physical parameters gives a mass of 1.08 ± 0.06 M☉,[7] while the oxygen isotope ratio for a first Dredge-up star gives a mass of 1.2 M☉.[18] Arcturus has been estimated to be around 6 billion to 8.5 billion years old, and is ascending the red giant branch until it accumulates a large enough degenerate helium core to ignite the helium flash.[7]

Oscillations

As one of the brightest stars in the sky, Arcturus has been the subject of a number of studies in the emerging field of asteroseismology. Belmonte and colleagues carried out a radial velocity (Doppler shift of spectral lines) study of the star in April and May 1988, which showed variability with a frequency of the order of a few microhertz, the highest peak corresponding to 4.3 μHz (2.7 days) with an amplitude of 60 ms−1, with a frequency separation of ~5 μHz. They suggested that the most plausible explanation for the variability of Arcturus is stellar oscillations.[19]

Asteroseismological measurements allow direct calculation of the mass and radius, giving values of 0.8 ± 0.2 M☉ and 27.9 ± 3.4 R☉. This form of modelling is still relatively inaccurate, but a useful check on others models.[20]

Element abundance

Astronomers term "metals" those elements with higher atomic numbers than helium. Arcturus has an enrichment of alpha elements relative to iron but only about a third of solar metallicity, Arcturus is possibly a Population II star.[11]

Kinematics

Arcturus is notable for its high proper motion, two arc seconds a year, greater than any first magnitude star other than α Centauri. It is moving rapidly (122 km/s) relative to the Solar System, and is now almost at its closest point to the Sun. Closest approach will happen in about 4,000 years, when the star will be a few hundredths of a light year closer to Earth than it is today. Arcturus is thought to be an old disk star, and appears to be moving with a group of 52 other such stars, known as the Arcturus stream.[21]

In antiquity, Arcturus was closer to the centre of the constellation.[9]

Possible planetary system

Hipparcos also suggested that Arcturus is a binary star, with the companion about twenty times dimmer than the primary and orbiting close enough to be at the very limits of our current ability to make it out. Recent results remain inconclusive, but do support the marginal Hipparcos detection of a binary companion.[22]

In 1993, radial velocity measurements of Aldebaran, Arcturus and Pollux showed that Arcturus exhibited a long-period radial velocity oscillation, which could be interpreted as a substellar companion. This substellar object would be nearly 12 times the mass of Jupiter and be located roughly at the same orbital distance from Arcturus as the Earth is from the Sun, at 1.1 Astronomical Units. However, all three stars surveyed showed similar oscillations yielding similar companion masses, and the authors concluded that the variation was likely to be intrinsic to the star rather than due to the gravitational effect of a companion. So far no substellar companion has been confirmed.[23]

Names and cultural significance

Comparison between Arcturus, red supergiant Antares, and the Sun. The black circle is the size of the orbit of Mars.

The name of the star derives from Ancient Greek Ἀρκτοῦρος (Arktouros) and means "Guardian of the Bear",[24] ultimately from ἄρκτος (arktos), "bear"[25] and οὖρος (ouros), "watcher, guardian".[26] It has been known by this name since at least the time of Hesiod.[9] This is a reference to its being the brightest star in the constellation Boötes (of which it forms the left foot), which is next to the Greater and Lesser Bears, Ursa Major and Ursa Minor.

In Ancient Rome, the star's celestial activity was supposed to portend tempestuous weather, and a personification of the star acts as narrator of the prologue to Plautus' comedy Rudens (circa 211 BC).[27][28]

In the Middle Ages, Arcturus was considered a Behenian fixed star[29] and attributed to the stone Jasper and the plantain herb. Cornelius Agrippa listed its kabbalistic sign under the alternate name Alchameth.

In Arabic

In Arabic, Arcturus is one of two stars called al-simāk ("the uplifted one"); the other is Spica. Arcturus is specified as السماك الرامح as-simāk ar-rāmiħ "the uplifted one of the lancer". The term Al Simak Al Ramih has appeared in Al Achsasi Al Mouakket catalogue (translated into Latin as Al Simak Lanceator).[30]

This has been variously romanized in the past, leading to obsolete variants such as Aramec and Azimech. For example, the name Alramih is used in Geoffrey Chaucer's Treatise on the Astrolabe (1391). Another Arabic name is Haris-el-sema, from حارس السماء ħāris al-samā’ "the keeper of heaven".[31][32][33] or حارس ألشمل ħāris al-shamāl’ "the keeper of north".[34]

In the Hebrew scriptures Arcturus is referred to in Job 38:32.[35]

Arcturus was once again called by its classical name from the Renaissance onwards.[36]

Aboriginal Australians

The Wotjobaluk Koori people of southeastern Australia knew Arcturus as Marpean-kurrk, mother of Djuit (Antares) and another star in Bootes, Weet-kurrk[37] (Muphrid).[38] Its appearance in the north signified the arrival of the larvae of the wood ant (a food item) in spring. The beginning of summer was marked by the star's setting with the Sun in the west and the disappearance of the larvae.[37] The people of Milingimbi Island in Arnhem Land saw Arcturus and Muphrid as man and woman, and took the appearance of Arcturus at sunrise as a sign to go and harvest rakia or spikerush.[39]:24,69,112 The Wailwun of northern New South Wales knew Arcturus as Guembila "red".[39]:84

China

In Chinese astronomy, Arcturus is called Da Jiao (Chinese: 大角; pinyin: Dàjiǎo; literally: "great horn"), because it is the brightest star in the Chinese constellation called Jiao Xiu (Chinese: 角宿; pinyin: Jiǎo Xiǔ; literally: "horn star"). Later it become a part of another constellation Kang Xiu (Chinese: 亢宿; pinyin: Kàng Xiǔ).

India

In Indian Astrology or Vedic Astrology or Sidereal Astrology, Arcturus is called 'Swati' which is a word meaning "very beneficent" derived from the language Sanskrit. It is the eponymous star of one of the nakshatras (lunar mansions) of Hindu astrology.

Inuit

In Inuit astronomy, Arcturus is called the Old Man (Uttuqalualuk in Inuit) and The First Ones (Sivulliik in Inuit).

The Mi'kmaq of eastern Canada saw Arcturus as Kookoogwéss, the owl.[40]

Indonesia

In Indonesia, Arcturus is called Bintang Biduk (star of boat).

Polynesia

Arcturus had several names that described its significance to indigenous Polynesians. In the Society Islands, Arcturus, called Ana-tahua-taata-metua-te-tupu-mavae ("a pillar to stand by"), was one of the ten "pillars of the sky", bright stars that represented the ten heavens of the Tahitian afterlife.[41] In Hawaii, the pattern of Boötes was called Hoku-iwa, meaning "stars of the frigate bird". This constellation marked the path for Hawaiiloa on his return to Hawaii from the South Pacific Ocean.[42] The Hawaiians called Arcturus Hoku-leʻa.[43] It was equated to the Tuamotuan constellation Te Kiva, meaning "frigate-bird", which could either represent the figure of Boötes or just Arcturus.[44] However, Arcturus may instead be the Tuamotuan star called Turu.[45] The Hawaiian name for Arcturus as a single star was likely Hoku-leʻa, which means "star of gladness", or "clear star".[46] In the Marquesas Islands, Arcturus was probably called Tau-tou and was the star that ruled the month approximating January. The Maori and Moriori called it Tautoru, a variant of the Marquesan name and a name shared with Orion's Belt.[47]

Japan

In Japan, Arcturus is called Mugi-boshi (麦星), meaning star of wheat.

1933 World's Fair

Arcturus achieved fame when its light was rumored to be the mechanism used to open the 1933 Chicago World's Fair. The star was chosen as it was thought that light from Arcturus had started its journey at about the time of the previous Chicago World's Fair in 1893. The star is 36.7 light-years from Earth, and the light started its journey in 1896.[48]

See also

References

  1. 1 2 3 4 5 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.
  2. 1 2 3 4 5 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues 2237: 0. Bibcode:2002yCat.2237....0D.
  3. ↑ Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Robinson, P. E. (2003). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 Parsecs: The Northern Sample. I". The Astronomical Journal 126 (4): 2048. arXiv:astro-ph/0308182. Bibcode:2003AJ....126.2048G. doi:10.1086/378365.
  4. ↑ Massarotti, Alessandro; Latham, David W.; Stefanik, Robert P.; Fogel, Jeffrey (2008). "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity". The Astronomical Journal 135: 209. Bibcode:2008AJ....135..209M. doi:10.1088/0004-6256/135/1/209.
  5. 1 2 Perryman; et al. (1997). "HIP 69673". The Hipparcos and Tycho Catalogues.
  6. 1 2 Carney, Bruce W.; et al. (March 2008). "Rotation and Macroturbulence in Metal-Poor Field Red Giant and Red Horizontal Branch Stars". The Astronomical Journal 135 (3): 892–906. arXiv:0711.4984. Bibcode:2008AJ....135..892C. doi:10.1088/0004-6256/135/3/892.
  7. 1 2 3 4 5 6 7 8 I. Ramírez; C. Allende Prieto (December 2011). "Fundamental Parameters and Chemical Composition of Arcturus". The Astrophysical Journal 743 (2): 135. arXiv:1109.4425. Bibcode:2011ApJ...743..135R. doi:10.1088/0004-637X/743/2/135.
  8. ↑ Schröder, K.-P.; Cuntz, M. (April 2007). "A critical test of empirical mass loss formulas applied to individual giants and supergiants". Astronomy and Astrophysics 465 (2): 593–601. arXiv:astro-ph/0702172. Bibcode:2007A&A...465..593S. doi:10.1051/0004-6361:20066633.
  9. 1 2 3 Rogers, John H. (1998). "Origins of the Ancient Constellations: II. The Mediterranean Traditions". Journal of the British Astronomical Association 108 (2): 79–89. Bibcode:1998JBAA..108...79R.
  10. ↑ Rogers, John H. (1998). "Origins of the Ancient Constellations: I. The Mesopotamian Traditions". Journal of the British Astronomical Association 108 (1): 9–28. Bibcode:1998JBAA..108....9R.
  11. 1 2 3 4 5 Schaaf, Fred (2008). The Brightest Stars: Discovering the Universe Through the Sky's Most Brilliant Stars. Hoboken, New Jersey: John Wiley and Sons. pp. 126–36. ISBN 978-0-471-70410-2.
  12. ↑ Kaler, James B. (2002). The Hundred Greatest Stars. New York, New York: Copernicus Books. p. 21. ISBN 0-387-95436-8.
  13. ↑ Schaaf, p. 257.
  14. ↑ Griffin, R. E.; Griffin, R. (1968). A photometric atlas of the spectrum of Arcturus, λλ3600-8825Å. Cambridge: Cambridge Philosophical Society. Bibcode:1968pmas.book.....G.
  15. ↑ Hinkle, Kenneth; Wallace, Lloyd; Valenti, Jeff; Harmer, Dianne (2000). Visible and Near Infrared Atlas of the Arcturus Spectrum 3727-9300 Å. San Francisco: Astronomical Society of the Pacific. Bibcode:2000vnia.book.....H. ISBN 1-58381-037-4.
  16. ↑ Hinkle, Kenneth; Wallace, Lloyd; Livingston, William Charles (1995). Infrared atlas of the Arcturus spectrum, 0.9-5.3 microns. San Francisco: Astronomical Society of the Pacific. Bibcode:1995iaas.book.....H.
  17. ↑ Hinkle, Kenneth; Wallace, Lloyd; Valenti, Jeff; Ayres, Thomas (2005). Ultraviolet Atlas of the Arcturus Spectrum, 1150-3800 Å. San Francisco: Astronomical Society of the Pacific. Bibcode:2005uaas.book.....H.
  18. ↑ Abia, C.; Palmerini, S.; Busso, M.; Cristallo, S. (2012). "Carbon and oxygen isotopic ratios in Arcturus and Aldebaran. Constraining the parameters for non-convective mixing on the red giant branch". Astronomy & Astrophysics 548: A55. arXiv:1210.1160. Bibcode:2012A&A...548A..55A. doi:10.1051/0004-6361/201220148.
  19. ↑ Belmonte, J. A.; Jones, A. R.; Palle, P. L.; Roca Cortes, T. (1990). "Acoustic oscillations in the K2 III star Arcturus". Astrophysics and Space Science 169 (1–2): 77–84. Bibcode:1990Ap&SS.169...77B. doi:10.1007/BF00640689. ISSN 0004-640X.
  20. ↑ Kallinger, T.; Weiss, W. W.; Barban, C.; Baudin, F.; Cameron, C.; Carrier, F.; De Ridder, J.; Goupil, M.-J.; Gruberbauer, M.; Hatzes, A.; Hekker, S.; Samadi, R.; Deleuil, M. (2010). "Oscillating red giants in the CoRoT exofield: Asteroseismic mass and radius determination". Astronomy and Astrophysics 509: A77. Bibcode:2010A&A...509A..77K. doi:10.1051/0004-6361/200811437.
  21. ↑ Ramya, P.; Reddy, Bacham E.; Lambert, David L. (2012). "Chemical compositions of stars in two stellar streams from the Galactic thick disc". Monthly Notices of the Royal Astronomical Society 425 (4): 3188. arXiv:1207.0767. Bibcode:2012MNRAS.425.3188R. doi:10.1111/j.1365-2966.2012.21677.x.
  22. ↑ Verhoelst, T.; Bordé, P. J.; Perrin, G.; Decin, L.; et al. (2005). "Is Arcturus a well-understood K giant?". Astronomy & Astrophysics 435: 289. arXiv:astro-ph/0501669. Bibcode:2005A&A...435..289V. doi:10.1051/0004-6361:20042356., and see references therein.
  23. ↑ Hatzes, A.; Cochran, W. (August 1993). "Long-period radial velocity variations in three K giants". The Astrophysical Journal 413 (1): 339–348. Bibcode:1993ApJ...413..339H. doi:10.1086/173002.
  24. ↑ Ἀρκτοῦρος, Henry George Liddell, Robert Scott, A Greek-English Lexicon, on Perseus
  25. ↑ ἄρκτος, Henry George Liddell, Robert Scott, A Greek-English Lexicon, on Perseus
  26. ↑ οὖρος, Henry George Liddell, Robert Scott, A Greek-English Lexicon, on Perseus
  27. ↑ Plautus. "Rudens". p. prol. 71.
  28. ↑ Lewis and Short. "Arcturus". Latin Dictionary.
  29. ↑ Tyson, Donald; Freake, James (1993), Three Books of Occult Philosophy, Llewellyn Worldwide, ISBN 0-87542-832-0
  30. ↑ Knobel, E. B. (June 1895). "Al Achsasi Al Mouakket, on a catalogue of stars in the Calendarium of Mohammad Al Achsasi Al Mouakket". Monthly Notices of the Royal Astronomical Society 55: 429. Bibcode:1895MNRAS..55..429K. doi:10.1093/mnras/55.8.429.
  31. ↑ "List of the 25 brightest stars". Jordanian Astronomical Society. Retrieved March 28, 2007.
  32. ↑ Allen, Richard Hinckley (1936). Star-names and their meanings. pp. 100–101.
  33. ↑ Wehr, Hans (1994). Cowan, J. Milton, ed. A dictionary of modern written Arabic.
  34. ↑ Davis Jr., G. A. (October 3, 1944). "The Pronunciations, Derivations, and Meanings of a Selected List of Star Names". Popular Astronomy LII: 13. Bibcode:1944PA.....52....8D.
  35. ↑ "Job 38:32". Bible Hub.
  36. ↑ Kunitzsch, Paul; Smart, Tim (2006). A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.). Cambridge, MA: Sky Pub. p. 19. ISBN 978-1-931559-44-7.
  37. 1 2 Mudrooroo (1994). Aboriginal mythology : an A-Z spanning the history of aboriginal mythology from the earliest legends to the present day. London: HarperCollins. p. 5. ISBN 1-85538-306-3.
  38. ↑ Hamacher, Duane W.; Frew, David J. (2010). "An Aboriginal Australian Record of the Great Eruption of Eta Carinae" (PDF). Journal of Astronomical History & Heritage 13 (3): 220–34. arXiv:1010.4610. Bibcode:2010JAHH...13..220H.
  39. 1 2 Johnson, Diane (1998). Night skies of aboriginal Australia: a noctuary. Darlington, New South Wales: University of Sydney. pp. 24, 69, 84, 112. ISBN 1-86451-356-X.
  40. ↑ Hagar, Stansbury (1900). "The Celestial Bear". The Journal of American Folklore 13 (49): 92–103. doi:10.2307/533799. JSTOR 533799.
  41. ↑ Makemson 1941, p. 199.
  42. ↑ Makemson 1941, p. 209.
  43. ↑ Makemson 1941, p. 280.
  44. ↑ Makemson 1941, p. 221.
  45. ↑ Makemson 1941, p. 264.
  46. ↑ Makemson 1941, p. 210.
  47. ↑ Makemson 1941, p. 260.
  48. ↑ "Century of Progress World's Fair, 1933-1934". University of Illinois-Chicago. January 2008. Retrieved 2009-09-06.

Cited texts

Notes

    External links

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    Coordinates: 14h 15m 39.7s, 19° 10′ 56″

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