Procyon#Oscillations

File:Hubble_heic0206j.jpg (top right) and Sirius (bottom) form the Winter Triangle. Orion is to the right. Viewed from Northern Hemisphere]]

Procyon is usually the eighth-brightest star in the night sky, culminating at midnight on 14 January.{{sfn|Schaaf|2008|p=257}} It forms one of the three vertices of the Winter Triangle asterism, in combination with Sirius and Betelgeuse.{{sfn|Schaaf|2008|p=166}} The prime period for evening viewing of Procyon is in late winter in the Northern Hemisphere.{{sfn|Schaaf|2008|p=257}}

It has a color index of 0.42, and its hue has been described as having a faint yellow tinge to it.{{sfn|Schaaf|2008|p=166}}

Procyon is a binary star system with a bright primary component, Procyon A, having an apparent magnitude of 0.34, and a faint companion, Procyon B, at magnitude 10.7. The pair orbit each other with a period of 40.84 years along an elliptical orbit with an eccentricity of 0.4, more eccentric than Mercury's. The plane of their orbit is inclined at an angle of 31.1° to the line of sight with the Earth. The average separation of the two components is {{val|15.0|ul=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.

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 hydrogen core into helium, after which it will expand as the nuclear reactions move outside the core. 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.{{sfn|Schaaf|2008|p=168}}

The effective temperature of the stellar atmosphere is an estimated {{val|6582|ul=K|fmt=commas}}, giving Procyon A a white hue. It is 1.5 times the solar mass ({{Solar mass|link=y}}), twice the solar radius ({{Solar radius|link=y}}), and has seven times the Sun's luminosity ({{Solar luminosity|link=y}}). Both the core and the envelope of this star are convective; the two regions being separated by a wide radiation zone.

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. However, others argued that the non-detection was consistent with published ground-based radial velocity observations of solar-like oscillations. Subsequent observations in radial velocity have confirmed that Procyon is indeed oscillating.{{cite journal |display-authors=1 |bibcode=2008ApJ...687.1180A | doi=10.1086/592040 | volume=687 | title=A Multisite Campaign to Measure Solar-like Oscillations in Procyon. I. Observations, Data Reduction, and Slow Variations | year=2008 | journal=The Astrophysical Journal | pages=1180–1190 | last1 = Arentoft | first1 = Torben | last2 = Kjeldsen | first2 = Hans | last3 = Bedding | first3 = Timothy R. | last4 = Bazot | first4 = Michaël | last5 = Christensen-Dalsgaard | first5 = Jørgen | last6 = Dall | first6 = Thomas H. | last7 = Karoff | first7 = Christoffer | last8 = Carrier | first8 = Fabien | last9 = Eggenberger | first9 = Patrick | last10 = Sosnowska | first10 = Danuta | last11 = Wittenmyer | first11 = Robert A. | last12 = Endl | first12 = Michael | last13 = Metcalfe | first13 = Travis S. | last14 = Hekker | first14 = Saskia | last15 = Reffert | first15 = Sabine | last16 = Butler | first16 = R. Paul | last17 = Bruntt | first17 = Hans | last18 = Kiss | first18 = László L. | last19 = O'Toole | first19 = Simon J. | last20 = Kambe | first20 = Eiji | last21 = Ando | first21 = Hiroyasu | last22 = Izumiura | first22 = Hideyuki | last23 = Sato | first23 = Bun'Ei | last24 = Hartmann | first24 = Michael | last25 = Hatzes | first25 = Artie | last26 = Bouchy | first26 = Francois | last27 = Mosser | first27 = Benoit | last28 = Appourchaux | first28 = Thierry | last29 = Barban | first29 = Caroline | last30 = Berthomieu | first30 = Gabrielle | last31 = Garcia | first31 = Rafael A. | last32 = Michel | first32 = Eric | last33 = Provost | first33 = Janine | last34 = Turck-Chièze | first34 = Sylvaine | last35 = Martić | first35 = Milena | last36 = Lebrun | first36 = Jean-Claude | last37 = Schmitt | first37 = Jerome | last38 = Bertaux | first38 = Jean-Loup | last39 = Bonanno | first39 = Alfio | last40 = Benatti | first40 = Serena | last41 = Claudi | first41 = Riccardo U. | last42 = Cosentino | first42 = Rosario | last43 = Leccia | first43 = Silvio | last44 = Frandsen | first44 = Søren | last45 = Brogaard | first45 = Karsten | last46 = Glowienka | first46 = Lars | last47 = Grundahl | first47 = Frank | last48 = Stempels | first48 = Eric| issue=2 | arxiv=0807.3794 | hdl = 2152/34819 | s2cid=15693672 | hdl-access = free }}{{cite journal | display-authors=1 |bibcode=2010ApJ...713..935B | doi=10.1088/0004-637X/713/2/935 | volume=713 | year=2010 | journal=The Astrophysical Journal | pages=935–949 | last1 = Bedding | first1 = Timothy R. | last2 = Kjeldsen | first2 = Hans | last3 = Campante | first3 = Tiago L. | last4 = Appourchaux | first4 = Thierry | last5 = Bonanno | first5 = Alfio | last6 = Chaplin | first6 = William J. | last7 = Garcia | first7 = Rafael A. | last8 = Martić | first8 = Milena | last9 = Mosser | first9 = Benoit | last10 = Butler | first10 = R. 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Ii. Mode Frequencies | issue=2 | arxiv=1003.0052 | hdl = 2152/34818 | s2cid=118470468 | hdl-access = free }}

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. Unlike the MOST result, the variation seen in the WIRE photometry was in agreement with radial velocity measurements from the ground. Additional observations with MOST taken in 2007 were able to detect oscillations.{{Cite journal |display-authors=1 |bibcode=2011ApJ...731...94H |title=Solar-like Oscillations and Activity in Procyon: A Comparison of the 2007 MOST and Ground-based Radial Velocity Campaigns |last1= Huber |first1= Daniel |last2= Bedding |first2= Timothy R. |last3= Arentoft |first3= Torben |last4= Gruberbauer |first4= Michael |last5= Guenther |first5= David B. |last6= Houdek |first6= Günter |last7= Kallinger |first7= Thomas |last8= Kjeldsen |first8= Hans |last9= Matthews |first9= Jaymie M. |last10= Stello |first10= Dennis |last11= Weiss |first11= Werner W. |journal=The Astrophysical Journal |year=2011 |volume=731 |issue=2 |page=94 |doi=10.1088/0004-637X/731/2/94 |arxiv=1102.2894 |s2cid=56123076}}

File:Procyonorbitillustration.jpg

Like Sirius B, Procyon B is a white dwarf that was inferred from astrometric data long before it was observed. Its existence had been postulated by German astronomer Friedrich Bessel as early as 1844, and, although its orbital elements had been calculated by his countryman Arthur Auwers in 1862 as part of his thesis, 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. 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.

At {{Solar mass|0.6|link=y}}, 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. The radius agrees with white dwarf models that assume a carbon core. It has a stellar classification of DQZ, 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. With a surface temperature of {{val|fmt=commas|7740|ul=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 {{val|2.59|+0.22|-0.18|u=solar mass}} and it came to the end of its life some {{val|1.19|0.11}} billion years ago, after a main-sequence lifetime of {{val|680|170}} million years.

Attempts to detect X-ray emission from Procyon with nonimaging, soft X-ray-sensitive detectors prior to 1975 failed. Extensive observations of Procyon were carried out with the Copernicus and TD-1A satellites in the late 1970s. The X-ray source associated with Procyon AB was observed on 1 April 1979, with the Einstein Observatory high-resolution imager (HRI). 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).

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

The name Procyon comes from the Ancient Greek {{lang|grc|Προκύων}} ({{Transliteration|grc|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. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN){{cite web | url=https://www.iau.org/science/scientific_bodies/working_groups/280/ | title=IAU Working Group on Star Names (WGSN)|access-date=22 May 2016}} to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016{{cite web | url=http://www.pas.rochester.edu/~emamajek/WGSN/WGSN_bulletin1.pdf | title=Bulletin of the IAU Working Group on Star Names, No. 1 |access-date=28 July 2016}} included a table of the first two batches of names approved by the WGSN; which included Procyon for the star α Canis Minoris A.

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 organizing the celestial sky.{{cite book|author=Kelley, David H.|author2=Milone, Eugene F.|author3=Aveni, A. F. |title=Exploring Ancient Skies: A Survey of Ancient and Cultural Astronomy|publisher=Springer|location=New York City|date=2011|pages=217|isbn=978-1441976239|url=https://books.google.com/books?id=ILBuYcGASxcC&pg=PA217}}

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.{{cite journal|title=Macedonian Folk Constellations |author=Cenev, Gjore |journal=Publications of the Astronomical Observatory of Belgrade|volume= 85|pages=97–109|bibcode=2008POBeo..85...97C|year=2008 }}

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.{{Cite journal | last1 = Gingerich | first1 = O.| doi = 10.1111/j.1749-6632.1987.tb37197.x | title = Zoomorphic Astrolabes and the Introduction of Arabic Star Names into Europe | journal = Annals of the New York Academy of Sciences | volume = 500 | issue = 1| pages = 89–104 | year = 1987 |bibcode = 1987NYASA.500...89G | s2cid = 84102853}} Al Shira derives from {{lang|ar|الشعرى الشامية}} {{Transliteration|ar|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 {{lang|ar|الغميصاء}} {{Transliteration|ar|al-ghumaisa’}} "the bleary-eyed (woman)", in contrast to {{lang|ar|العبور}} "the teary-eyed (woman)", which is Sirius. (See Gomeisa.)

In Chinese, {{lang|zh|南河}} ({{lang|zh-Latn|Nán Hé}}), meaning South River, refers to an asterism consisting of Procyon, ε Canis Minoris and β Canis Minoris.{{in lang|zh}} 中國星座神話, written by 陳久金. Published by 台灣書房出版有限公司, 2005, {{ISBN|978-986-7332-25-7}}. Consequently, Procyon itself is known as {{lang|zh|南河三}} ({{lang|zh-Latn|Nán Hé sān}}, the Third Star of South River).{{in lang|zh}} [http://www.lcsd.gov.hk/CE/Museum/Space/Research/StarName/c_research_chinengstars_e_g.htm 香港太空館 – 研究資源 – 亮星中英對照表] {{webarchive|url=https://web.archive.org/web/20110130063007/http://www.lcsd.gov.hk/CE/Museum/Space/Research/StarName/c_research_chinengstars_e_g.htm |date=30 January 2011}}, Hong Kong Space Museum. Accessed on line 23 November 2010. It is part of the Vermilion Bird.

The Hawaiians see Procyon as part of an asterism Ke ka o Makali'i ("the canoe bailer of Makali'i") that helps them navigate at sea.{{Cite web|title=Hawaiian Star Lines|url=http://archive.hokulea.com/ike/hookele/hawaiian_star_lines.html#ke_ka_o_makalii|access-date=2020-10-21|website=archive.hokulea.com}} In Hawaiian language, this star is called Puana ("blossom"), which is a new Hawaiian name based on the Māori name Puangahori. It forms this asterism (Ke ka o Makali'i) with the Pleiades (Makali'i), Auriga, Orion, Capella, Sirius, Castor and Pollux.{{Cite book | last=Brosch | first=Noah | title=Sirius Matters | date=2008 | publisher=Springer | isbn=978-1-4020-8318-1 | page= 46 |url = https://books.google.com/books?id=ricStR4SE-UC&pg=PA46}} 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.{{cite journal|last=Henry|first=Teuira |author-link=Teuira Henry |date=1907|title=Tahitian Astronomy: Birth of Heavenly Bodies|journal=The Journal of the Polynesian Society |volume=16|issue=2|pages=101–04|jstor=20700813}} Māori astronomers know the star as Puangahori ("False Puanga") which distinguishes it from its pair Puanga or Puanga-rua ("Blossom-cluster") which refers to a star of great importance to Māori culture and calendar, known by its western name Rigel.{{cite book|last=Best|first=Elsdon|title=Astronomical Knowledge of the Maori: Genuine and Empirical|publisher=Dominion Museum|location=Wellington, New Zealand|date=1922|page=33|url=http://nzetc.victoria.ac.nz/tm/scholarly/tei-BesAstro-t1-body-d1-d6-d4.html}}

Procyon appears on the flag of Brazil, symbolizing the state of Amazonas.

The Kalapalo people of Mato Grosso state in Brazil call 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.{{cite book|last=Basso|first=Ellen B. |title=In Favor of Deceit: A Study of Tricksters in an Amazonian Society|publisher=University of Arizona Press|location=Tucson, Arizona|date=1987|pages=[https://archive.org/details/infavorofdeceits0000bass/page/360 360]|isbn=978-0-8165-1022-1|url=https://archive.org/details/infavorofdeceits0000bass|url-access=registration}}

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.{{cite book |title = The Arctic sky: Inuit astronomy, star lore, and legend |url = https://archive.org/details/arcticskyinuitas0000macd |url-access = registration |last = MacDonald |first = John |publisher = Royal Ontario Museum/Nunavut Research Institute|location=Toronto, Ontario/Iqaluit, NWT |date = 1998 |isbn = 9780888544278|pages=[https://archive.org/details/arcticskyinuitas0000macd/page/72 72], 231–33}}

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 right ascension {{RA|19|39|18.11950}}, declination {{DEC|-05|13|29.9552}}. It would be as bright as β Scorpii is in our sky.

Procyon's closest neighboring star is Luyten's Star, about {{Convert|1.12|ly|pc|abbr=off}} away. Procyon would be the brightest star in the night sky of an exoplanet orbiting Luyten's Star, with an apparent magnitude of -4.68.{{efn|1=The absolute magnitude M_v of Procyon is 2.66, so the apparent magnitude m is given by 2.66 − 5 + (5*log₁₀(0.34)) = -4.68.{{cite book |first=Roger John |last=Tayler |date=1994 |title=The Stars: Their Structure and Evolution |url=https://archive.org/details/starstheirstruct00tayl_311 |url-access=limited |publisher=Cambridge University Press |page=[https://archive.org/details/starstheirstruct00tayl_311/page/n24 16] |isbn=978-0-521-45885-6}}}} Luyten's Star would also be visible from Procyon, at an apparent magnitude of 4.61, unlike any red dwarfs from Earth.

• Procyon in astrology

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}}

{{Sky|07|39|18.1|+|05|13|29|11}}

{{Nearest systems|2}}

{{Stars of Canis Minor}}

{{Portal bar|Astronomy|Stars|Outer space}}

{{DEFAULTSORT:Procyon}}

Category:F-type main-sequence stars

Category:F-type subgiants

Category:White dwarfs

Category:Binary stars

Category:Local Bubble

Category:Canis Minor

Canis Minoris, Alpha

2943

BD+05 1739

Canis Minoris, 10

0280

061421

037279

Category:Astronomical objects known since antiquity

Category:TIC objects

Procyon