Procyon

Procyon A/B

The position of Procyon
Observation data
Epoch J2000      Equinox J2000
Constellation Canis Minor
Pronunciation /ˈproʊsi.ɒn/
Right ascension 07h 39m 18.11950s[1][2]
Declination +05° 13′ 29.9552″[1][2]
Apparent magnitude (V) 0.34[3] (A) / 10.7[4] (B)
Characteristics
Evolutionary stage Main sequence
Spectral type F5 IV–V[3] + DQZ[5]
U−B color index −0.01
B−V color index 0.40/0.0
Variable type suspected[6] (A)
Astrometry
Radial velocity (Rv)−3.2 km/s
Proper motion (μ) RA: −714.590[1][2] mas/yr
Dec.: −1036.80[1][2] mas/yr
Parallax (π)284.56 ± 1.26[1][2] mas
Distance11.46 ± 0.05 ly
(3.51 ± 0.02 pc)
Absolute magnitude (MV)2.66/13.0[4]
Details
Procyon A
Mass1.499±0.031[7] M☉
Radius2.048±0.025[3] R☉
Luminosity6.93[3] L☉
Surface gravity (log g)3.96[3] cgs
Temperature6,530±50[3] K
Metallicity [Fe/H]−0.05±0.03[3] dex
Rotation23 days[8]
Rotational velocity (v sin i)3.16±0.50[3] km/s
Age1.87±0.13[7] Gyr
Procyon B
Mass0.602±0.015[5] M☉
Radius0.01234±0.00032[5] R☉
Luminosity0.00049[9] L☉
Surface gravity (log g)8.0[5] cgs
Temperature7,740±50[5] K
Age1.37[9] Gyr
Orbit[10]
CompanionProcyon B
Period (P)40.82 yr
Semi-major axis (a)4.3″
Eccentricity (e)0.407
Inclination (i)31.1°
Longitude of the node (Ω)97.3°
Periastron epoch (T)1967.97
Argument of periastron (ω)
(secondary)		92.2°
Other designations
Elgomaisa, Algomeysa, Antecanis, α Canis Minoris, 10 Canis Minoris, GCTP 1805.00, HR 2943, BD+05°1739, HD 61421, LHS 233, GJ 280, HIP 37279, SAO 115756.[11]
Database references
SIMBADThe system
A
B

Procyon (BrE /ˈproʊsi.ɒn/;[12] PRO-see-on), also designated Alpha Canis Minoris (α Canis Minoris, abbreviated Alpha CMi, α CMi), is the brightest star in the constellation of Canis Minor. To the naked eye, it appears to be a single star, the eighth-brightest in the night sky with a visual apparent magnitude of 0.34.[3] It is a binary star system, consisting of a white main-sequence star of spectral type F5 IV–V, named Procyon A, and a faint white dwarf companion of spectral type DQZ,[5] named Procyon B.

As determined by the European Space Agency Hipparcos astrometry satellite,[1][13] it lies at a distance of just 11.46 light-years (3.51 parsecs),[2] and is therefore one of Earth's nearest stellar neighbours. Its closest neighboring star is Luyten's Star, about 1.12 ly (0.34 pc) away, and the latter would appear as a visual magnitude 2.7 star in the night sky of a hypothetical planet orbiting Procyon.[14]

Visibility

Procyon is the eighth-brightest star in the night sky, culminating at midnight on January 14.[15] It forms one of the three vertices of the Winter Triangle asterism, in combination with Sirius and Betelgeuse.[16] The prime period for evening viewing of Procyon is in late winter.[15]

It has a color index of 0.42, and its hue has been described as having a faint yellow tinge to it.[16]

System

Procyon is a binary star system with a bright primary component, Procyon A, having an apparent magnitude of 0.34,[3] and a faint companion, Procyon B, at magnitude 10.7.[4] The pair orbit each other with a period of 40.82 years along an elliptical orbit with an eccentricity of 0.407. The plane of their orbit is inclined at an angle of 31.1° to the line of sight with the Earth.[10] The average separation of the two components is 15.0 AU, a little less than the distance between Uranus and the Sun, though the eccentric orbit carries them as close as 8.9 AU and as far as 21.0 AU.[17]

Primary star

The primary has a stellar classification of F5IV–V, indicating that it is a late-stage F-type main-sequence star. Procyon A is bright for its spectral class, suggesting that it is evolving into a subgiant that has nearly fused its core hydrogen into helium, after which it will expand as "burning" moves outside the core.[3] As it continues to expand, the star will eventually swell to about 80 to 150 times its current diameter and become a red or orange color. This will probably happen within 10 to 100 million years.[18]

The effective temperature of the stellar atmosphere is an estimated 6,530 K,[3] giving Procyon A a white hue. It is 1.5 times the solar mass (M☉), twice the solar radius (R☉), and has 6.9 times the Sun's luminosity (L☉).[3][19] Both the core and the envelope of this star are convective; the two regions being separated by a wide radiation zone.[7]

Oscillations

In late June 2004, Canada's orbital MOST satellite telescope carried out a 32-day survey of Procyon A. The continuous optical monitoring was intended to confirm solar-like oscillations in its brightness observed from Earth and to permit asteroseismology. No oscillations were detected and the authors concluded that the theory of stellar oscillations may need to be reconsidered.[20] However, others argued that the non-detection was consistent with published ground-based radial velocity observations of solar-like oscillations.[21][22]

Photometric measurements from the NASA Wide Field Infrared Explorer (WIRE) satellite from 1999 and 2000 showed evidence of granulation (convection near the surface of the star) and solar-like oscillations.[23] Unlike the MOST result, the variation seen in the WIRE photometry was in agreement with radial velocity measurements from the ground.

White dwarf companion

Like Sirius B, Procyon's companion is a white dwarf that was inferred from astrometric data long before it was observed. Its existence had been postulated by Friedrich Bessel as early as 1844, and, although its orbital elements had been calculated by Arthur Auwers in 1862 as part of his thesis,[24] Procyon B was not visually confirmed until 1896 when John Martin Schaeberle observed it at the predicted position using the 36-inch refractor at Lick Observatory.[25] It is more difficult to observe from Earth than Sirius B, due to a greater apparent magnitude difference and smaller angular separation from its primary.[17]

At 0.6 M☉, Procyon B is considerably less massive than Sirius B; however, the peculiarities of degenerate matter ensure that it is larger than its more famous neighbor, with an estimated radius of 8,600 km, versus 5,800 km for Sirius B.[5][26] The radius agrees with white dwarf models that assume a carbon core.[5] It has a stellar classification of DQZ,[5] having a helium-dominated atmosphere with traces of heavy elements. For reasons that remain unclear, the mass of Procyon B is unusually low for a white dwarf star of its type.[7] With a surface temperature of 7,740 K, it is also much cooler than Sirius B; this is a testament to its lesser mass and greater age. The mass of the progenitor star for Procyon B was about 2.59+0.22
−0.18 M☉ and it came to the end of its life some 1.19±0.11 Gyr ago, after a main-sequence lifetime of 680±170 Myr.[7]

X-ray emission

Attempts to detect X-ray emission from Procyon with nonimaging, soft X-ray–sensitive detectors prior to 1975 failed.[27][27] Extensive observations of Procyon were carried out with the Copernicus and TD-1A satellites in the late 1970s.[28] The X-ray source associated with Procyon A/B was observed on April 1, 1979, with the Einstein Observatory high-resolution imager (HRI).[29] The HRI X-ray pointlike source location is ~4" south of Procyon A, on the edge of the 90% confidence error circle, indicating identification with Procyon A rather than Procyon B which was located about 5" north of Procyon A (about 9" from the X-ray source location).[28]

Etymology and cultural significance

α Canis Minoris (Latinised to Alpha Canis Minoris) is the star's Bayer designation.

The name Procyon comes from the Ancient Greek Προκύων (Prokyon), meaning "before the dog", since it precedes the "Dog Star" Sirius as it travels across the sky due to Earth's rotation. (Although Procyon has a greater right ascension, it also has a more northerly declination, which means it will rise above the horizon earlier than Sirius from most northerly latitudes.) In Greek mythology, Procyon is associated with Maera, a hound belonging to Erigone, daughter of Icarius of Athens.[30] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[31] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[32] included a table of the first two batches of names approved by the WGSN; which included Procyon for this star.

The two dog stars are referred to in the most ancient literature and were venerated by the Babylonians and the Egyptians, In Babylonian mythology, Procyon was known as Nangar (the Carpenter), an aspect of Marduk, involved in constructing and organising the celestial sky.[33]

The constellations in Macedonian folklore represented agricultural items and animals, reflecting their village way of life. To them, Procyon and Sirius were Volci "the wolves", circling hungrily around Orion which depicted a plough with oxen.[34]

Rarer names are the Latin translation of Procyon, Antecanis, and the Arabic-derived names Al Shira and Elgomaisa. Medieval astrolabes of England and Western Europe used a variant of this, Algomeiza/Algomeyza.[35] Al Shira derives from الشعرى الشامية aš-ši‘ra aš-šamiyah, "the Syrian sign" (the other sign being Sirius; "Syria" is supposedly a reference to its northern location relative to Sirius); Elgomaisa. derives from الغميصاء al-ghumaisa’ "the bleary-eyed (woman)", in contrast to العبور "the teary-eyed (woman)", which is Sirius. (See Gomeisa.) At the same time this name is synonymous with the Turkish name "Rumeysa", and it is a commonly used name in Turkey. The modern Arabic name for Procyon is غموص ghumūṣ. It is known as 南河三 (Mandarin nánhésān, the "Third Star in the South of the River") in Chinese, and it is part of the Vermilion Bird.

The Hawaiians saw Procyon as part of an asterism Ke ka o Makali'i ("the canoe bailer of Makali'i") that helped them navigate at sea. Called Puana "blossom", it formed this asterism with Capella, Sirius, Castor, and Pollux.[36] In Tahitian lore, Procyon was one of the pillars propping up the sky, known as Anâ-tahu'a-vahine-o-toa-te-manava ("star-the-priestess-of-brave-heart"), the pillar for elocution.[37] The Maori knew the star as Puangahori.[38]

Procyon appears on the flag of Brazil, symbolising the state of Amazonas.[39] The Kalapalo people of Mato Grosso state in Brazil called Procyon and Canopus Kofongo "Duck", with Castor and Pollux representing his hands. The asterism's appearance signified the coming of the rainy season and increase in food staple manioc, used at feasts to feed guests.[40]

Known as Sikuliarsiujuittuq to the Inuit, Procyon was quite significant in their astronomy and mythology. Its eponymous name means "the one who never goes onto the newly formed sea-ice", and refers to a man who stole food from his village's hunters because he was too obese to hunt on ice. He was killed by the other hunters who convinced him to go on the sea ice. Procyon received this designation because it typically appears red (though sometimes slightly greenish) as it rises during the Arctic winter; this red color was associated with Sikuliarsiujuittuq's bloody end.[41]

View from this System

Were the Sun to be observed from this star system, it would appear to be a magnitude 2.55 star in the constellation Aquila with the exact opposite coordinates at RA: 19h 39m 18.11950s, Dec.: -05° 13' 29.9552". It would be as bright as Beta Scorpii is in our sky. Given its large distance, β Canis Minoris would be in a similar part of the sky, reducing Canis Minor to one star.

While the night sky would be very similar to that of Earth, the nearby stars would be in unfamiliar positions; Sirius, which is almost twice as close as it is to the Sun, would be far brighter and would be in the southern constellation of Grus and Alpha Centauri would be located in the "Teapot" of Sagittarius in the Zodiac. Consequently, Canis Minor, Canis Major, and Centaurus would all be missing their brightest stars.

See also

References

  1. 1 2 3 4 5 6 Perryman, M. A. C.; Lindegren, L.; Kovalevsky, J.; et al. (July 1997), "The Hipparcos Catalogue", Astronomy and Astrophysics, 323: L49–L52, Bibcode:1997A&A...323L..49P
  2. 1 2 3 4 5 6 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, Bibcode:2007A&A...474..653V, arXiv:0708.1752 Freely accessible, doi:10.1051/0004-6361:20078357
  3. 1 2 3 4 5 6 7 8 9 10 11 12 13 Kervella, P.; et al. (January 2004), "The diameter and evolutionary state of Procyon A. Multi-technique modeling using asteroseismic and interferometric constraints", Astronomy and Astrophysics, 413 (1): 251–256, Bibcode:2004A&A...413..251K, arXiv:astro-ph/0309148 Freely accessible, doi:10.1051/0004-6361:20031527
  4. 1 2 3 Schroeder, Daniel J.; Golimowski, David A.; Brukardt, Ryan A.; Burrows, Christopher J.; Caldwell, John J.; Fastie, William G.; Ford, Holland C.; Hesman, Brigette; Kletskin, Ilona; Krist, John E.; Royle, Patricia; Zubrowski, Richard. A. (February 2000), "A Search for Faint Companions to Nearby Stars Using the Wide Field Planetary Camera 2", The Astronomical Journal, 119 (2): 906–922, Bibcode:2000aj....119..906s, doi:10.1086/301227
  5. 1 2 3 4 5 6 7 8 9 Provencal, J. L.; et al. (2002), "Procyon B: Outside the Iron Box", The Astrophysical Journal, 568 (1): 324–334, Bibcode:2002ApJ...568..324P, doi:10.1086/338769
  6. ↑ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007–2013)". VizieR On-line Data Catalog: B/gcvs. Originally published in: 2009yCat....102025S. 1: 02025. Bibcode:2009yCat....102025S.
  7. 1 2 3 4 5 Liebert, James; et al. (May 2013), "The Age and Stellar Parameters of the Procyon Binary System", The Astrophysical Journal, 769 (1): 10, Bibcode:2013ApJ...769....7L, arXiv:1305.0587 Freely accessible, doi:10.1088/0004-637X/769/1/7, 7
  8. ↑ Koncewicz, R.; Jordan, C. (January 2007), "OI line emission in cool stars: calculations using partial redistribution", Monthly Notices of the Royal Astronomical Society, 374 (1): 220–231, Bibcode:2007MNRAS.374..220K, doi:10.1111/j.1365-2966.2006.11130.x
  9. 1 2 Giammichele, N.; Bergeron, P.; Dufour, P. (April 2012), "Know Your Neighborhood: A Detailed Model Atmosphere Analysis of Nearby White Dwarfs", The Astrophysical Journal Supplement, 199 (2): 29, Bibcode:2012ApJS..199...29G, arXiv:1202.5581 Freely accessible, doi:10.1088/0067-0049/199/2/29 Age is for the white dwarf stage.
  10. 1 2 Girard, T. M.; et al. (May 2000), "A Redetermination of the Mass of Procyon", The Astronomical Journal, 119 (5): 2428–2436, Bibcode:2000AJ....119.2428G, doi:10.1086/301353
  11. ↑ "PROCYON AB -- Spectroscopic binary", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2011-11-23
  12. ↑ "Procyon". Oxford English Dictionary (3rd ed.). Oxford University Press. September 2005. (Subscription or UK public library membership required.)
  13. ↑ Perryman, Michael (2010), "The Making of History's Greatest Star Map", The Making of History's Greatest Star Map:, Astronomers’ Universe, Heidelberg: Springer-Verlag, Bibcode:2010mhgs.book.....P, ISBN 978-3-642-11601-8, doi:10.1007/978-3-642-11602-5
  14. ↑ "Annotations on LHS 33 object", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2010-04-21
  15. 1 2 Schaaf, Fred (2008), "The Brightest Stars: Discovering the Universe through the Sky's Most Brilliant Stars", The Astrophysical Journal, John Wiley & Sons, 113: 257, Bibcode:1951ApJ...113....1S, ISBN 047024917X, doi:10.1086/145373, retrieved 2014-12-28
  16. 1 2 Schaaf 2008, p. 166.
  17. 1 2 Kaler, James B., "Procyon", Stars, University of Illinois, retrieved 2011-11-23
  18. ↑ Schaaf 2008, p. 168.
  19. ↑ Gatewood, G.; Han, I. (February 2006), "An Astrometric Study of Procyon", Astronomical Journal, 131 (2): 1015–1021, Bibcode:2006AJ....131.1015G, doi:10.1086/498894
  20. ↑ Matthews, Jaymie M.; et al. (2004), "No stellar p-mode oscillations in space-based photometry of Procyon", Nature, 430 (921): 51–3, Bibcode:2004Natur.430...51M, PMID 15229593, doi:10.1038/nature02671
  21. ↑ Bouchy, François; et al. (2004), "Brief Communications Arising: Oscillations on the star Procyon", Nature, 432 (7015): 2, Bibcode:2004Natur.432....2B, PMID 15568216, arXiv:astro-ph/0510303 Freely accessible, doi:10.1038/nature03165
  22. ↑ Bedding, T. R.; et al. (2005), "The non-detection of oscillations in Procyon by MOST: Is it really a surprise?", Astronomy and Astrophysics, 432 (2): L43, Bibcode:2005A&A...432L..43B, arXiv:astro-ph/0501662 Freely accessible, doi:10.1051/0004-6361:200500019
  23. ↑ Bruntt, H.; et al. (2005), "Evidence for Granulation and Oscillations in Procyon from Photometry with the WIRE Satellite", The Astrophysical Journal, 633 (1): 440–446, Bibcode:2005ApJ...633..440B, arXiv:astro-ph/0504469 Freely accessible, doi:10.1086/462401
  24. ↑ Auwers, Arthur (1868), Untersuchungen uber veranderliche eigenbewegungen (in German), Leipzig: W. Engelmann, Bibcode:1868uuve.book.....A
  25. ↑ Burnham Jr., Robert (1978), Burnham's Celestial Handbook, 1, New York: Dover Publications Inc., p. 450, ISBN 0-486-23567-X
  26. ↑ Holberg, J. B.; et al. (1998-04-20), "Sirius B: A New, More Accurate View", The Astrophysical Journal, 497 (2): 935–942, Bibcode:1998ApJ...497..935H, doi:10.1086/305489
  27. 1 2 Mewe, R.; et al. (December 1, 1975), "Detection of X-ray emission from stellar coronae with ANS", Astrophysical Journal Letters, 202: L67–L71, Bibcode:1975ApJ...202L..67M, doi:10.1086/181983
  28. 1 2 Schmitt, J. H. M. M.; et al. (January 15, 1985), "The X-ray corona of Procyon", Astrophysical Journal, Part 1, 288: 751–755, Bibcode:1985ApJ...288..751S, doi:10.1086/162843
  29. ↑ Giacconi, R.; et al. (1979), "The Einstein /HEAO 2/ X-ray Observatory", Astrophysical Journal, 230: 540–550, Bibcode:1979ApJ...230..540G, doi:10.1086/157110
  30. ↑ Wendy Doniger, eds. (1999), "Erigone", Merriam-Webster's encyclopedia of world religions, Merriam-Webster, p. 333, ISBN 0-87779-044-2
  31. ↑ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
  32. ↑ "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
  33. ↑ Kelley, David H.; Milone, Eugene F.; Aveni, A.F. (2011). Exploring Ancient Skies: A Survey of Ancient and Cultural Astronomy. New York, New York: Springer. p. 217. ISBN 144197623X.
  34. ↑ Cenev, Gjore. "Macedonian Folk Constellations". Publications of the Astronomical Observatory of Belgrade. 85: 97–109. Bibcode:2008POBeo..85...97C.
  35. ↑ Gingerich, O. (1987). "Zoomorphic Astrolabes and the Introduction of Arabic Star Names into Europe". Annals of the New York Academy of Sciences. 500: 89–104. Bibcode:1987NYASA.500...89G. doi:10.1111/j.1749-6632.1987.tb37197.x.
  36. ↑ Brosch, Noah (2008). Sirius Matters. Springer. p. 46. ISBN 1-4020-8318-1.
  37. ↑ Henry, Teuira (1907). "Tahitian Astronomy: Birth of Heavenly Bodies". The Journal of the Polynesian Society. 16 (2): 101–04. JSTOR 20700813.
  38. ↑ Best, Elsdon (1922). Astronomical Knowledge of the Maori: Genuine and Empirical. Wellington, New Zealand: Dominion Museum. p. 33.
  39. ↑ MacDonald, Ian (August 9, 2009), Astronomy of the Brazilian Flag, FOTW Flags Of The World website, retrieved 2011-11-23
  40. ↑ Basso, Ellen B. (1987). In Favor of Deceit: A Study of Tricksters in an Amazonian Society. Tucson, Arizona: University of Arizona Press. p. 360. ISBN 0816510229.
  41. ↑ MacDonald, John (1998). The Arctic sky: Inuit astronomy, star lore, and legend. Toronto, Ontario/Iqaluit, NWT: Royal Ontario Museum/Nunavut Research Institute. pp. 72, 231–33. ISBN 9780888544278.

Sources

Coordinates: 07h 39m 18.1s, +05° 13′ 29″

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