View source for Astronomy:Procyon

{{short description|Star in the constellation Canis Minor}}
{{Starbox begin}}
{{Starbox image
 | image   = [[Image:Position Alpha Cmi.png|250px]]
 | caption = The position of Procyon
}}
{{Starbox observe
 | epoch     = J2000
 | constell  = [[Astronomy:Canis Minor|Canis Minor]]
 | pronounce = {{IPAc-en|ˈ|p|r|oʊ|s|i|.|ɒ|n}} {{respell|PROH|see|on}}<ref>{{OED|Procyon}}</ref>
 | ra        = {{RA|07|39|18.11950}}<ref name=aaa474_2_653/>
 | dec       = {{DEC|+05|13|29.9552}}<ref name=aaa474_2_653/>
 | appmag_v  = 0.34<ref name=aaa413/> (A) / 10.7<ref name="ApJ119_2"/> (B)
}}
{{Starbox character
 | class = F5 IV–V<ref name=aaa413/> + DQZ<ref name=Provencal2002/>
 | b-v   = +0.42<ref name=eggen/>
 | u-b   = +0.00<ref name=eggen>{{cite journal|bibcode=1986EgUBV........0M|title=Compilation of Eggen's UBV data, transformed to UBV (unpublished)|journal=Catalogue of Eggen's UBV Data|last1=Mermilliod|first1=J.-C|year=1986}}</ref> |
  variable=suspected<ref name=gcvs>{{cite journal|bibcode=2009yCat....102025S|title=VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007–2013)|journal=VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S|volume=1|pages=02025|last1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009|display-authors=0}}</ref> (A)
}}
{{Starbox astrometry
 | radial_v    = −3.2<ref name=rv>{{cite journal|bibcode=1953GCRV..C......0W|title=General catalogue of stellar radial velocities|journal=Washington|last1=Wilson|first1=Ralph Elmer|year=1953}}</ref>
 | prop_mo_ra  = −714.590<ref name=aaa474_2_653/>
 | prop_mo_dec = −1036.80<ref name=aaa474_2_653/>
 | parallax    = 284.56
 | p_error     = 1.26
 | parallax_footnote =<ref name=aaa474_2_653/>
 | absmag_v    = 2.66/13.0<ref name="ApJ119_2"/>
}}
{{Starbox detail
 | component1 = Procyon A
 | mass     = {{val|1.499|0.031}}<ref name=Liebert2013/>
 | radius   = {{val|2.048|0.025}}<ref name=aaa413/>
 | luminosity  = 6.93<ref name=aaa413/>
 | temperature = {{val|6530|50|fmt=commas}}<ref name=aaa413/>
 | metal_fe = {{val|−0.05|0.03}}<ref name=aaa413/>
 | gravity  = 3.96<ref name=aaa413/>
 | rotational_velocity = {{val|3.16|0.50}}<ref name=aaa413/>
 | rotation = 23&nbsp;days<ref name=mnras374_1_220/>
 | age_gyr  = {{val|1.87|0.13}}<ref name=Liebert2013/>
 | component2 = Procyon B
 | mass2    = {{val|0.602|0.015}}<ref name="Provencal2002"/>
 | radius2  = {{val|0.01234|0.00032}}<ref name="Provencal2002"/>
 | luminosity2  = 0.00049<ref name="ApJS199_2_29"/>
 | temperature2 = {{val|7740|50|fmt=commas}}<ref name="Provencal2002"/>
 | age_gyr2 = 1.37<ref name="ApJS199_2_29"/>
 | gravity2 = 8.0<ref name="Provencal2002"/>
}}
{{Starbox visbin
 | reference  =<ref name=ApJ2015/>
 | name       = Procyon B
 | period     = 40.840 ± 0.022
 | axis       = 4.3075 ± 0.0016
 | eccentricity = 0.39785 ± 0.00025
 | inclination  = 31.408 ± 0.050
 | node       = 100.683 ± 0.095
 | periastron = 1,968.076 ± 0.023
 | periarg    = 89.23 ± 0.11
}}<!--
-->{{Starbox catalog
 | names = {{odlist | name=Elgomaisa<ref>{{cite book
 | last =von Littrow
 | first =Karl
 | title =J. J. von Littrow's Atlas des gestirnten Himmels für Freunde der Astronomie
 | publisher =Gustav Weise
 | date =1866
 | location =Stuttgart
 | pages =9
 | language =German }}</ref> | B=α&nbsp;Canis Minoris | F=10 Canis Minoris | BD=+05°1739 | GJ=280 | HD=61421 | HIP=37279 | HR=2943 | SAO=115756 | GCTP=1805.00 | LHS=233 }}<ref name=SIMBAD/>
}}
{{Starbox reference
 | Simbad  = HR+2943|sn=The system
 | Simbad2 = *+alf+CMi+A|sn2=A
 | Simbad3 = *+alf+CMi+B|sn3=B
}}
{{Starbox end}}

'''Procyon''' ({{IPAc-en|ˈ|p|r|oʊ|s|i|.|ɒ|n}})<ref name=Kunitzsch>{{cite book
 |last1=Kunitzsch |first1=Paul
 |last2=Smart |first2=Tim
 |date = 2006 |edition = 2nd rev.
 |title = A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations
 |publisher = Sky Pub |location = Cambridge, Massachusetts
 |isbn = 978-1-931559-44-7
}}</ref> is the brightest [[Astronomy:Star|star]] in the [[Astronomy:Constellation|constellation]] of [[Astronomy:Canis Minor|Canis Minor]] and usually the [[Astronomy:List of brightest stars|eighth-brightest star]] in the [[Astronomy:Night sky|night sky]], with an [[Astronomy:Apparent visual magnitude|apparent visual magnitude]] of 0.34.<ref name=aaa413/> It has the [[Astronomy:Bayer designation|Bayer designation]] '''α Canis Minoris''', which is [[Social:Latinisation of names|Latinized]] to '''Alpha Canis Minoris''', and abbreviated '''α CMi''' or '''Alpha CMi''', respectively. As determined by the [[Organization:European Space Agency|European Space Agency]] ''[[Astronomy:Hipparcos|Hipparcos]]'' astrometry satellite,<ref name=GSM/> this system lies at a distance of just {{Convert|11.46|ly|pc|abbr=off|lk=on}},<ref name=aaa474_2_653/> and is therefore one of Earth's [[Astronomy:List of nearest stars and brown dwarfs|nearest stellar neighbors]].

A [[Astronomy:Binary star|binary star]] system, Procyon consists of a white-hued main-sequence star of spectral type F5&nbsp;IV–V, designated component A, in orbit with a faint [[Astronomy:White dwarf|white dwarf]] companion of spectral type DQZ,<ref name=Provencal2002/> named Procyon B. The pair orbit each other with a [[Astronomy:Orbital period|period]] of 40.84&nbsp;years and an [[Astronomy:Orbital eccentricity|eccentricity]] of 0.4.

==Observation==
[[File:Hubble_heic0206j.jpg|left|thumb|Procyon (''top left''), Betelgeuse (''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<!-- Procyon can be surpassed in brightness by Betelgeuse --> in the night sky, [[Astronomy:Culmination|culminating]] at midnight on 14 January.{{sfn|Schaaf|2008|p=257}} It forms one of the three [[Vertex (geometry)|vertices]] of the Winter Triangle [[Astronomy:Asterism|asterism]], in combination with [[Astronomy:Sirius|Sirius]] and [[Astronomy:Betelgeuse|Betelgeuse]].{{sfn|Schaaf|2008|p=166}} The prime period for evening viewing of Procyon is in late winter in the [[Earth:Northern Hemisphere|Northern Hemisphere]].{{sfn|Schaaf|2008|p=257}}

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

==Stellar system==
Procyon is a [[Astronomy:Binary star|binary star]] system with a bright primary component, Procyon A, having an apparent magnitude of 0.34,<ref name=aaa413/> and a faint companion, Procyon B, at magnitude 10.7.<ref name="ApJ119_2"/> The pair orbit each other with a [[Astronomy:Orbital period|period]] of 40.84&nbsp;years along an elliptical orbit with an [[Astronomy:Orbital eccentricity|eccentricity]] of 0.4,<ref name=ApJ2015/> more eccentric than [[Astronomy:Mercury (planet)|Mercury]]'s. The [[Astronomy:Orbital plane|plane]] of their orbit is inclined at an angle of 31.1° to the line of sight with the Earth.<ref name=aj119_5/> The average separation of the two components is {{val|15.0|ul=AU}}, a little less than the distance between [[Astronomy:Uranus|Uranus]] and the [[Astronomy:Sun|Sun]], though the eccentric orbit carries them as close as 8.9&nbsp;AU and as far as 21.0&nbsp;AU.<ref name=Kaler2011/>

===Procyon A===
The primary has a [[Astronomy:Stellar classification|stellar classification]] of F5IV–V, indicating that it is a late-stage [[Astronomy:F-type main-sequence star|F-type main-sequence star]]. Procyon A is bright for its spectral class, suggesting that it is evolving into a [[Astronomy:Subgiant|subgiant]] that has nearly [[Physics:Nuclear fusion|fused]] its [[Chemistry:Hydrogen|hydrogen]] core into [[Chemistry:Helium|helium]], after which it will expand as the nuclear reactions move outside the core.<ref name=aaa413/> 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 [[Astronomy:Effective temperature|effective temperature]] of the [[Astronomy:Stellar atmosphere|stellar atmosphere]] is an estimated {{val|6530|ul=K|fmt=commas}},<ref name=aaa413/> giving Procyon A a white hue. It is 1.5 times the [[Astronomy:Solar mass|solar mass]] ({{Solar mass|link=y}}), twice the [[Astronomy:Solar radius|solar radius]] ({{Solar radius|link=y}}), and has seven times the Sun's luminosity ({{Solar luminosity|link=y}}).<ref name=aaa413/><ref name=aj131/> Both the core and the envelope of this star are [[Astronomy:Convection zone|convective]]; the two regions being separated by a wide [[Astronomy:Radiation zone|radiation zone]].<ref name=Liebert2013/>

====Oscillations====
In late June 2004, Canada's orbital MOST satellite telescope carried out a 32-day survey of Procyon&nbsp;A. The continuous optical monitoring was intended to confirm [[Astronomy:Solar-like oscillations|solar-like oscillations]] in its brightness observed from Earth and to permit [[Astronomy:Asteroseismology|asteroseismology]]. No [[Oscillation|oscillation]]s were detected and the authors concluded that the theory of stellar oscillations may need to be reconsidered.<ref name=nature430_921/> However, others argued that the non-detection was consistent with published ground-based [[Astronomy:Radial velocity|radial velocity]] observations of solar-like oscillations.<ref name=nature432_7015/><ref name=aaa432/> Subsequent observations in radial velocity have confirmed that Procyon is indeed oscillating.<ref>{{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 }}</ref><ref>{{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. Paul | last11 = Bruntt | first11 = Hans | last12 = Kiss | first12 = László L. | last13 = O'Toole | first13 = Simon J. | last14 = Kambe | first14 = Eiji | last15 = Ando | first15 = Hiroyasu | last16 = Izumiura | first16 = Hideyuki | last17 = Sato | first17 = Bun'Ei | last18 = Hartmann | first18 = Michael | last19 = Hatzes | first19 = Artie | last20 = Barban | first20 = Caroline | last21 = Berthomieu | first21 = Gabrielle | last22 = Michel | first22 = Eric | last23 = Provost | first23 = Janine | last24 = Turck-Chièze | first24 = Sylvaine | last25 = Lebrun | first25 = Jean-Claude | last26 = Schmitt | first26 = Jerome | last27 = Bertaux | first27 = Jean-Loup | last28 = Benatti | first28 = Serena | last29 = Claudi | first29 = Riccardo U. | last30 = Cosentino | first30 = Rosario | last31 = Leccia | first31 = Silvio | last32 = Frandsen | first32 = Søren | last33 = Brogaard | first33 = Karsten | last34 = Glowienka | first34 = Lars | last35 = Grundahl | first35 = Frank | last36 = Stempels | first36 = Eric | last37 = Arentoft | first37 = Torben | last38 = Bazot | first38 = Michaël | last39 = Christensen-Dalsgaard | first39 = Jørgen | last40 = Dall | first40 = Thomas H. | last41 = Karoff | first41 = Christoffer | last42 = Lundgreen-Nielsen | first42 = Jens | last43 = Carrier | first43 = Fabien | last44 = Eggenberger | first44 = Patrick | last45 = Sosnowska | first45 = Danuta | last46 = Wittenmyer | first46 = Robert A. | last47 = Endl | first47 = Michael | last48 = Metcalfe | first48 = Travis S. | last49 = Hekker | first49 = Saskia | last50 = Reffert | first50 = Sabine| title=A Multi-Site Campaign to Measure Solar-Like Oscillations in Procyon. Ii. Mode Frequencies | issue=2 | arxiv=1003.0052 | hdl = 2152/34818 | s2cid=118470468 | hdl-access = free }}</ref>

[[Astronomy:Photometry|Photometric]] measurements from the [[Organization:NASA|NASA]] [[Astronomy:Wide Field Infrared Explorer|Wide Field Infrared Explorer]] (WIRE) satellite from 1999 and 2000 showed evidence of granulation ([[Astronomy:Convection|convection]] near the surface of the [[Astronomy:Star|star]]) and [[Astronomy:Solar-like oscillations|solar-like oscillations]].<ref name=apj633/> Unlike the MOST result, the variation seen in the WIRE photometry was in agreement with [[Astronomy:Radial velocity|radial velocity]] measurements from the ground. Additional observations with MOST taken in 2007 were able to detect oscillations.<ref>{{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}}</ref>

===Procyon B===
[[File:Procyonorbitillustration.jpg|thumb|left|Orbit of Procyon B seen from above its plane]]
Like Sirius B, Procyon B is a [[Astronomy:White dwarf|white dwarf]] that was inferred from [[Astronomy:Astrometry|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,<ref name=auwers/> Procyon&nbsp;B was not visually confirmed until 1896 when John Martin Schaeberle observed it at the predicted position using the 36-inch refractor at [[Organization:Lick Observatory|Lick Observatory]].<ref name=burnham78/> It is more difficult to observe from Earth than Sirius&nbsp;B, due to a greater [[Astronomy:Apparent magnitude|apparent magnitude]] difference and smaller angular separation from its primary.<ref name=Kaler2011/>

At {{Solar mass|0.6|link=y}}, Procyon&nbsp;B is considerably less massive than Sirius&nbsp;B; however, the peculiarities of [[Astronomy:Degenerate matter|degenerate matter]] ensure that it is larger than its more famous neighbor, with an estimated radius of 8,600&nbsp;km, versus 5,800&nbsp;km for Sirius&nbsp;B.<ref name="Provencal2002"/><ref name=apj497/> The radius agrees with white dwarf models that assume a carbon core.<ref name="Provencal2002"/> It has a [[Astronomy:Stellar classification|stellar classification]] of DQZ,<ref name=Provencal2002/> having a helium-dominated atmosphere with traces of heavy elements. For reasons that remain unclear, the mass of Procyon&nbsp;B is unusually low for a white dwarf star of its type.<ref name=Liebert2013/> With a surface temperature of {{val|7740|ul=K}}, it is also much cooler than Sirius&nbsp;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}}&nbsp;billion years ago, after a main-sequence lifetime of {{val|680|170}}&nbsp;million years.<ref name=Liebert2013/>

===X-ray emission===
Attempts to detect X-ray emission from Procyon with nonimaging, soft X-ray-sensitive detectors prior to 1975 failed.<ref name=apj202/> Extensive observations of Procyon were carried out with the [[Astronomy:Orbiting Astronomical Observatory#OAO-3 (Copernicus)|''Copernicus'']] and [[Astronomy:TD-1A|TD-1A]] satellites in the late 1970s.<ref name=apj228_1/> The X-ray source associated with Procyon AB was observed on 1&nbsp;April 1979, with the [[Astronomy:Einstein Observatory|Einstein Observatory]] high-resolution imager (HRI).<ref name=apj540/> 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&nbsp;A (about 9″ from the X-ray source location).<ref name=apj228_1/>
<!--
===Possibility of life===
Life is unlikely around Procyon, because the habitable zone around 2.7&nbsp;AU from the primary may not contain stable orbits, due to the white dwarf companion with a periastron of 8.9 AU.{{or|date=July 2015}} Also the white dwarf companion to Procyon would have stressed life severely during its red-giant phase. Procyon emits more of its light in the [[Physics:Ultraviolet|ultraviolet]] spectrum, which may be damaging to life. Still, life cannot be ruled out for other stars of the spectral type of Procyon, but such life would have a relatively short time to evolve and would face heavy bombardment from [[Astronomy:Comet|comet]]s and [[Astronomy:Meteorite|meteorite]]s as happened in the first few million years of the Earth's existence. Shortly after the phase of heavy bombardment has ended for a planet orbiting a star like Procyon the star is likely to leave the [[Astronomy:Main sequence|main sequence]] preventing further development of life.<ref name=exoplaneten/>
-->

==Etymology and cultural significance==
''α Canis Minoris'' ([[Social:Latinisation of names|Latinized]] to ''Alpha Canis Minoris'') is the [[Astronomy:Star|star]]'s [[Astronomy:Bayer designation|Bayer designation]].

The name ''Procyon'' comes from the [[Social:Ancient Greek|Ancient Greek]] {{lang|grc|Προκύων}} (''{{transl|grc|Prokyon}}''), meaning "before the dog", since it precedes the "Dog Star" [[Astronomy:Sirius|Sirius]] as it travels across the sky due to [[Earth's rotation]]. (Although Procyon has a greater [[Right ascension|right ascension]], it also has a more northerly [[Declination|declination]], which means it will rise above the [[Horizon|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.<ref name=mw1999/> In 2016, the [[Organization:International Astronomical Union|International Astronomical Union]] organized a Working Group on Star Names (WGSN)<ref name="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}}</ref> to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016<ref name="WGSN1">{{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}}</ref> 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 [[Religion:Marduk|Marduk]], involved in constructing and organizing the celestial sky.<ref name="kelley11">{{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}}</ref>

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.<ref>{{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 }}</ref>

Rarer names are the Latin translation of Procyon, ''Antecanis'', and the [[Social:Arabic|Arabic]]-derived names ''Al&nbsp;Shira'' and ''Elgomaisa''. Medieval [[Astronomy:Astrolabe|astrolabe]]s of England and Western Europe used a variant of this, ''Algomeiza/Algomeyza''.<ref>{{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}}</ref> ''Al&nbsp;Shira'' derives from {{lang|ar|الشعرى الشامية}} ''{{transl|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}} ''{{transl|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 ''[[Astronomy:Well (Chinese constellation)|South River]]'', refers to an [[Astronomy:Asterism|asterism]] consisting of Procyon, ε Canis Minoris and β Canis Minoris.<ref>{{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}}.</ref> Consequently, Procyon itself is known as {{lang|zh|南河三}} ({{lang|zh-Latn|Nán Hé sān}}, ''the Third Star of South River'').<ref>{{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.</ref> It is part of the [[Astronomy:Vermilion Bird|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.<ref>{{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}}</ref> In [[Social:Hawaiian language|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, [[Astronomy:Capella|Capella]], Sirius, [[Astronomy:Castor (star)|Castor]] and [[Astronomy:Pollux (star)|Pollux]].<ref name=brosch>{{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}}</ref> 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.<ref name=henry1907>{{cite journal|last=Henry|first=Teuira |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}}</ref> 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.<ref name="Best22">{{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}}</ref>

Procyon appears on the flag of Brazil, symbolizing the state of Amazonas.<ref name=fotw/>
The Kalapalo people of Mato Grosso state in Brazil call Procyon and [[Astronomy:Canopus|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.<ref name="basso87">{{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}}</ref>

Known as ''Sikuliarsiujuittuq'' to the [[Unsolved:Inuit astronomy|Inuit]], Procyon was quite significant in their astronomy and mythology. Its eponymous name means "the one who never goes onto the newly formed [[Earth:Sea ice|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.<ref>{{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}}</ref>

==View from this system==
{{importance section|date=November 2023}}
Were [[Astronomy:Sun|Sol]] to be observed from this [[Astronomy:Star system|star system]], it would appear to be a [[Astronomy:Apparent magnitude|magnitude]] 2.55 star in the constellation [[Astronomy:Aquila (constellation)|Aquila]] with the exact opposite coordinates at [[Right ascension|right ascension]] {{RA|19|39|18.11950}}, [[Declination|declination]] {{DEC|-05|13|29.9552}}. It would be as bright as β Scorpii is in our sky. [[Astronomy:Canis Minor|Canis Minor]] would obviously be missing its brightest star.

Procyon's closest neighboring star is [[Astronomy:Luyten's Star|Luyten's Star]], about {{Convert|1.12|ly|pc|abbr=off}} away.<ref name=Annot/> 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<sub>v</sub>'' of Procyon is 2.66, so the apparent magnitude ''m'' is given by 2.66 − 5 + (5*log<sub>10</sub>(0.34)) = -4.68.<ref>{{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}}</ref>}}

==See also==
* [[Astronomy:Stars in astrology#Procyon|Procyon in astrology]]
* Procyon in fiction

==Notes==
{{notelist}}

==References==
{{Reflist|30em|refs=

<ref name="aaa474_2_653">{{citation | last1=van Leeuwen | first1=F. | title=Validation of the new Hipparcos reduction | journal=Astronomy and Astrophysics | volume=474 | issue=2 |date=November 2007 | pages=653–664 | doi=10.1051/0004-6361:20078357 | bibcode=2007A&A...474..653V | arxiv=0708.1752 | s2cid=18759600 }}</ref>

<ref name="GSM">{{citation | last=Perryman | first=Michael | title=The Making of History's Greatest Star Map | location=Heidelberg | publisher=Springer-Verlag | date=2010 | doi=10.1007/978-3-642-11602-5| series=Astronomers’ Universe | isbn=978-3-642-11601-8 | bibcode=2010mhgs.book.....P | url=https://cds.cern.ch/record/1338896/files/978-3-642-11602-5_BookTOC.pdf }}</ref>

<ref name="aaa413">{{citation | display-authors=1 | last1=Kervella | first1=P. | last2=Thévenin | first2=F. | last3=Morel | first3=P. | last4=Berthomieu | first4=G. | last5=Bordé | first5=P. | last6=Provost | first6=J. | title=The diameter and evolutionary state of Procyon A. Multi-technique modeling using asteroseismic and interferometric constraints | journal=Astronomy and Astrophysics | volume=413 | issue=1 | pages=251–256 |date=January 2004 | doi=10.1051/0004-6361:20031527 | bibcode=2004A&A...413..251K |arxiv = astro-ph/0309148 | s2cid=8840932 }}</ref>

<ref name="Provencal2002">{{citation | display-authors=1 | last1=Provencal | first1=J. L. | last2=Shipman | first2=H. L. | last3=Koester | first3=Detlev | last4=Wesemael | first4=F. | last5=Bergeron | first5=P. | title=Procyon B: Outside the Iron Box | journal=The Astrophysical Journal | date=2002 | volume=568 | issue=1 | pages=324–334 | bibcode=2002ApJ...568..324P | doi=10.1086/338769 | doi-access=free }}</ref>

<ref name="aj119_5">{{citation | display-authors=1 | last1=Girard | first1=T. M. | last2=Wu | first2=H. | last3=Lee | first3=J. T. | last4=Dyson | first4=S. E. | last5=van Altena | first5=W. F. | last6=Horch | first6=E. P. | last7=Gilliland | first7=R. L. | last8=Schaefer | first8=K. G. | last9=Bond | first9=H. E. | title=A Redetermination of the Mass of Procyon | journal=The Astronomical Journal | volume=119 | issue=5 | pages=2428–2436 |date=May 2000 | doi=10.1086/301353 | bibcode=2000AJ....119.2428G | doi-access=free }}</ref>

<ref name="aj131">{{citation | last1=Gatewood | first1=G. | last2=Han | first2=I. | title=An Astrometric Study of Procyon | journal=Astronomical Journal | volume=131 | issue=2 | pages=1015–1021 |date=February 2006 | doi=10.1086/498894 | bibcode=2006AJ....131.1015G | doi-access=free }}</ref>

<ref name="SIMBAD">{{citation | title=PROCYON AB -- Spectroscopic binary | work=SIMBAD | publisher=Centre de Données astronomiques de Strasbourg | url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=procyon | access-date=23 November 2011 }}</ref>

<ref name="Kaler2011">{{citation | first1=James B. | last1=Kaler | work=Stars | title=Procyon |  publisher=University of Illinois | url=http://stars.astro.illinois.edu/sow/procyon.html | access-date=23 November 2011 }}</ref>

<ref name="apj497">{{citation | display-authors=1 | last1=Holberg | first1=J. B. | last2=Barstow | first2=M. A. | last3=Bruhweiler | first3=F. C. | last4=Cruise | first4=A. M. |last5=Penny | first5=A. J. | title=Sirius B: A New, More Accurate View | journal=The Astrophysical Journal | volume=497 | issue=2 | pages=935–942 | date=2 April 1998| doi=10.1086/305489 | bibcode=1998ApJ...497..935H | doi-access=free }}</ref>

<ref name="burnham78">{{citation | first1=Robert | last1=Burnham Jr. |  title=Burnham's Celestial Handbook | location=New York | publisher=Dover Publications Inc. | date=1978 | page=450 | volume=1 | isbn=0-486-23567-X }}</ref>

<ref name="nature430_921">{{citation | display-authors=1 | last1=Matthews | first1=Jaymie M. | last2=Kuschnig | first2=Rainer | last3=Guenther | first3=David B. | last4=Walker | first4=Gordon A. H. | last5=Moffat | first5=Anthony F. J. | last6=Rucinski | first6=Slavek M. | last7=Sasselov | first7=Dimitar | last8=Weiss | first8=Werner W. | title=No stellar p-mode oscillations in space-based photometry of Procyon | journal=Nature | volume=430 | issue=921 | date=2004 | doi=10.1038/nature02671 | bibcode=2004Natur.430...51M | pmid=15229593 | pages=51–3 | s2cid=4420705 }}</ref>

<ref name="nature432_7015">{{citation | display-authors=1 | last1=Bouchy | first1=François | last2=Maeder | first2=Andreé | last3=Mayor | first3=Michel | last4=Mégevand | first4=Denis | last5=Pepe | first5=Francesco | last6=Sosnowska | first6=Danuta | title=Brief Communications Arising: Oscillations on the star Procyon | journal=Nature | volume=432 | issue=7015 | pages=2 | date=2004 | bibcode=2004Natur.432....2B |doi=10.1038/nature03165| pmid=15568216 |arxiv = astro-ph/0510303 | s2cid=593117 | url=https://hal.archives-ouvertes.fr/hal-00011135 }}</ref>

<ref name="aaa432">{{citation | display-authors=1 | last1=Bedding | first1=T. R. | author1-link = Tim Bedding | last2=Kjeldsen | first2=H. | last3=Bouchy | first3=F. | last4=Bruntt | first4=H. | last5=Butler | first5=R. P. | last6=Buzasi | first6=D. L. | last7=Christensen-Dalsgaard | first7=J. | author7-link = Jørgen Christensen-Dalsgaard | last8=Frandsen | first8=S. | last9=Lebrun | first9=J.-C. | title=The non-detection of oscillations in Procyon by MOST: Is it really a surprise? | journal=Astronomy and Astrophysics | volume=432
| issue=2 | page=L43 | date=2005 | doi=10.1051/0004-6361:200500019 | bibcode=2005A&A...432L..43B |arxiv = astro-ph/0501662 | s2cid=53350078 }}</ref>

<ref name="apj633">{{citation | display-authors=1 | last1=Bruntt | first1=H. | last2=Kjeldsen | first2=H. | last3=Buzasi | first3=D. L. | last4=Bedding | first4=T. R. | author4-link = Tim Bedding | title=Evidence for Granulation and Oscillations in Procyon from Photometry with the WIRE Satellite | journal=The Astrophysical Journal | volume=633 | issue=1 | pages=440–446 | date=2005 | doi=10.1086/462401 | bibcode=2005ApJ...633..440B |arxiv = astro-ph/0504469 | s2cid=1812152 }}</ref>

<!--<ref name=exoplaneten>{{citation | last1=Kuhlmann | first1=Christoph | last2=Requejo | first2=Xavier Dalmau | title=Spectral Type F - Procyon | work=exoplaneten.de | url=http://www.exoplaneten.de/procyon/english.html | access-date=1 May 2010 }}</ref> -->

<ref name="apj202">{{citation | display-authors=1 | last1=Mewe | first1=R. | last2=Heise | first2=J. | last3=Gronenschild | first3=E. H. B. M. | last4=Brinkman | first4=A. C. | last5=Schrijver | first5=J. | last6=den Boggende | first6=A. J. F. | title=Detection of X-ray emission from stellar coronae with ANS | journal=Astrophysical Journal Letters | volume=202 | date=1 December 1975 | pages=L67–L71 | doi=10.1086/181983 | bibcode=1975ApJ...202L..67M | doi-access=free }}</ref>

<ref name="apj228_1">{{citation | display-authors=1 | last1=Schmitt | first1=J. H. M. M. | last2=Harnden | first2=F. R. Jr. | last3=Rosner | first3=R. | last4=Peres | first4=G. | last5=Serio | first5=S. | title=The X-ray corona of Procyon | journal=Astrophysical Journal, Part 1 | volume=288 | date=15 January 1985 | pages=751–755 | doi=10.1086/162843 | bibcode=1985ApJ...288..751S }}</ref>

<ref name="apj540">{{citation | display-authors=1 | last1=Giacconi | first1=R. | last2=Branduardi | first2=G. | last3=Briel | first3=U. | last4=Epstein | first4=A. | last5=Fabricant | first5=D. | last6=Feigelson | first6=E. | last7=Forman | first7=W. | last8=Gorenstein | first8=P. | last9=Grindlay | first9=J. | title=The Einstein /HEAO 2/ X-ray Observatory | journal=Astrophysical Journal | volume=230 | pages=540–550 | date=1979 | doi=10.1086/157110 | bibcode=1979ApJ...230..540G | s2cid=120943949 | doi-access=free }}</ref>

<ref name="mw1999">{{citation | contribution=Erigone | date=1999 | title=Merriam-Webster's encyclopedia of world religions | page=333 | editor1=Wendy Doniger | publisher=Merriam-Webster | isbn=0-87779-044-2 | url=https://books.google.com/books?id=ZP_f9icf2roC&pg=PA333 }}</ref>

<ref name="fotw">{{citation | first1=Ian | last1=MacDonald | date=9 August 2009 | title=Astronomy of the Brazilian Flag | url=https://www.fotw.info/flags/br_astro.html | publisher=FOTW Flags of the World website | access-date=23 November 2011 | url-status=dead | archive-url=https://web.archive.org/web/20090628101130/https://www.fotw.info/flags/br_astro.html | archive-date=28 June 2009 }}</ref>

<ref name="auwers">{{citation | title=Untersuchungen uber veranderliche eigenbewegungen | journal=Leipzig | last1=Auwers | first1=Arthur | language=de | location=Leipzig | publisher=W. Engelmann | date=1868 | url=https://books.google.com/books?id=F9dDAAAAYAAJ | bibcode=1868uuve.book.....A }}</ref>

<ref name="mnras374_1_220">{{citation | last1=Koncewicz | first1=R. | last2=Jordan | first2=C. | title=OI line emission in cool stars: calculations using partial redistribution | journal=[[Organization:Monthly Notices of the Royal Astronomical Society|Monthly Notices of the Royal Astronomical Society]] | volume=374 | issue=1 | pages=220–231 |date=January 2007 | doi=10.1111/j.1365-2966.2006.11130.x | bibcode=2007MNRAS.374..220K | doi-access=free }}</ref>

<ref name="Annot">{{citation | title=Annotations on LHS 33 object | work= [[Astronomy:SIMBAD|SIMBAD]] | publisher=Centre de Données astronomiques de Strasbourg | url=http://cdsannotations.u-strasbg.fr/annotations/simbadObject/971564 | access-date=21 April 2010 }}</ref>

<ref name="ApJS199_2_29">{{citation | last1 = Giammichele | first1 = N. | last2 = Bergeron | first2 = P. | last3 = Dufour | first3 = P. | title = Know Your Neighborhood: A Detailed Model Atmosphere Analysis of Nearby White Dwarfs | journal = The Astrophysical Journal Supplement | volume = 199 | issue = 2 | page = 29 | date = April 2012 | arxiv = 1202.5581 | doi = 10.1088/0067-0049/199/2/29 | bibcode = 2012ApJS..199...29G | s2cid = 118304737 }} Age is for the white dwarf stage.</ref>

<ref name="ApJ119_2">{{citation | last1 = Schroeder | first1 = Daniel J. | last2 = Golimowski | first2 = David A. | last3 = Brukardt | first3 = Ryan A. | last4 = Burrows | first4 = Christopher J. | last5 = Caldwell | first5 = John J. | last6 = Fastie | first6 = William G. | last7 = Ford | first7 = Holland C. | last8 = Hesman | first8 = Brigette | last9 = Kletskin | first9 = Ilona | last10 = Krist | first10 = John E. | last11 = Royle | first11 = Patricia | last12 = Zubrowski | first12 = Richard. A. | title = A Search for Faint Companions to Nearby Stars Using the Wide Field Planetary Camera 2 | journal = The Astronomical Journal | volume = 119 | issue = 2 | pages = 906–922 | date = February 2000 | bibcode = 2000AJ....119..906S | doi = 10.1086/301227 | doi-access = free }}</ref>

<ref name="Liebert2013">{{citation | display-authors = 1 | last1 = Liebert | first1 = James | last2 = Fontaine | first2 = Gilles | last3 = Young | first3 = Patrick A. | last4 = Williams | first4 = Kurtis A. | last5 = Arnett | first5 = David | title = The Age and Stellar Parameters of the Procyon Binary System | journal = The Astrophysical Journal | volume = 769 | issue = 1 | id = 7 | pages = 10 | date = May 2013 | doi = 10.1088/0004-637X/769/1/7 | bibcode = 2013ApJ...769....7L | arxiv = 1305.0587 | s2cid = 118473397 }}</ref>

<ref name="ApJ2015">{{ citation | display-authors = 1 | last1 = Bond | first1 = Howard E. | last2 = Gilliland | first2 = Ronald L. | last3 = Schaefer | first3 = Gail H. | last4 = Demarque | first4 = Pierre | last5 = Girard | first5 = Terrence M. | last6 = Holberg | first6 = Jay B. | last7 = Gudehus | first7 = Donald | last8 = Mason | first8 = Brian D. | last9 = Kozhurina-Platais | first9 = Vera | last10 = Burleigh | first10 = Matthew R. | last11 = Barstow | first11 = Martin A. | last12 = Neland | first12 = Edmund P. | title = Hubble Space Telescope Astrometry of the Procyon System | journal = The Astrophysical Journal | volume = 813 | issue = 2 | id = 106 | pages = 19 | date = November 2015 | doi = 10.1088/0004-637X/813/2/106 | bibcode = 2015ApJ...813..106B | arxiv = 1510.00485 | s2cid = 55163606 }}</ref>

}}

==Sources==
* {{cite book |title=The Brightest Stars: Discovering the Universe through the Sky's Most Brilliant Stars |last=Schaaf |first=Fred |date=2008 |publisher=John Wiley & Sons |location=Hoboken, New Jersey |isbn=978-0-471-70410-2 }}

{{Sky|07|39|18.1|+|05|13|29|11}}
{{Nearest systems|3}}
{{Stars of Canis Minor}}

{{DEFAULTSORT:Procyon}}
<!-- Properties -->
[[Category:F-type main-sequence stars]]
[[Category:F-type subgiants]]
[[Category:White dwarfs]]
[[Category:Binary stars]]
<!-- Location/catalogues -->
[[Category:Canis Minor]]
[[Category:Bayer objects|Canis Minoris, Alpha]]
[[Category:Bright Star Catalogue objects|2943]]
[[Category:Durchmusterung objects|BD+05 1739]]
[[Category:Flamsteed objects|Canis Minoris, 10]]
[[Category:Gliese and GJ objects|0280]]
[[Category:Henry Draper Catalogue objects|061421]]
[[Category:Hipparcos objects|037279]]
[[Category:Astronomical objects known since antiquity]]

{{Sourceattribution|Procyon}}