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{{short description|Double star system in the constellation Cygnus}}
{{Starbox begin
{{Starbox begin
| name = Albireo
| name = Albireo
}}
}}
{{Starbox image
{{Starbox image
| image=
| image = [[Image:Position beta Cyg.png|280px]]
{{Location mark
| caption = Albireo's position, lower right corner. <br /> The cross-like figure is the Northern Cross. <br /> The blue line shows the boundaries of the constellation the Swan.
| image=Cygnus constellation map.svg
| float=center | width=250 | position=right
| mark=Red circle.svg | mark_width=8 | mark_link=Albireo (star)
| x%=62.8 | y%=83.6
}}
| caption=Location of Albireo (circled)
}}
}}
{{Starbox observe 3s
{{Starbox observe 3s
Line 13: Line 20:
| ra1 = {{RA|19|30|43.286}}<ref name=tycho2/>
| ra1 = {{RA|19|30|43.286}}<ref name=tycho2/>
| dec1 = {{DEC|+27|57|34.84}}<ref name=tycho2/>
| dec1 = {{DEC|+27|57|34.84}}<ref name=tycho2/>
| appmag_v1 = 3.18<ref name=bsd/>
| appmag_v1 = 3.21<ref name=drimmel2021/>
| component2 = Albireo Ac
| component2 = Albireo Ac
| ra2 = {{RA|19|30|43.295}}<ref name=tycho/>
| ra2 = {{RA|19|30|43.295}}<ref name=tycho/>
| dec2 = {{DEC|+27|57|34.62}}<ref name=tycho/>
| dec2 = {{DEC|+27|57|34.62}}<ref name=tycho/>
| appmag_v2 = 5.82<ref name=bsd />
| appmag_v2 = 5.85<ref name=drimmel2021/>
| component3 = Albireo B
| component3 = Albireo B
| ra3 = {{RA|19|30|45.3961}}<ref name=dr1/>
| ra3 = {{RA|19|30|45.3962}}<ref name=edr3B/>
| dec3 = {{DEC|+27|57|54.990}}<ref name=dr1/>
| dec3 = {{DEC|+27|57|54.989}}<ref name=edr3B/>
| appmag_v3 = 5.11<ref name=photometry/>
| appmag_v3 = 5.11<ref name=photometry/>
}}
}}
{{Starbox character
{{Starbox character
| component = Albireo Aa
| component = Albireo Aa
| type = [[Bright giant]]
| class = K2II<ref name="ginestet">{{Cite journal | last1 = Ginestet | first1 = N. | last2 = Carquillat | first2 = J. M. | doi = 10.1086/342942 | title = Spectral Classification of the Hot Components of a Large Sample of Stars with Composite Spectra, and Implication for the Absolute Magnitudes of the Cool Supergiant Components | journal = The Astrophysical Journal Supplement Series | volume = 143 | issue = 2 | pages = 513 | year = 2002 | pmid = | pmc = |bibcode = 2002ApJS..143..513G | doi-access = free }}</ref>
| class = K2II<ref name="ginestet"/>
| v-r = +0.92<ref name=bsd />
| v-r = +0.92<ref name=bsd />
| b-v = +1.13<ref name=photometry/>
| b-v = +1.13<ref name=photometry/>
Line 33: Line 41:
| b-v2 = +0.09<ref name=tycho/>
| b-v2 = +0.09<ref name=tycho/>
}}
}}
{{Starbox character|no_heading=y
{{Starbox character
|no_heading=y
| component = Albireo B
| component = Albireo B
| class = B8Ve<ref name=levenhagen/>
| class = B8Ve<ref name=levenhagen/>
| r-i = <!--R-I color-->
| v-r = <!--V-R color-->
| b-v = -0.10<ref name=photometry/>
| b-v = -0.10<ref name=photometry/>
| u-b = -0.32<ref name=photometry/>
| u-b = -0.32<ref name=photometry/>
}}
}}
{{Starbox astrometry
{{Starbox astrometry
| component = Albireo A
| radial_v = -24.07<ref name=rv/>
| prop_mo_ra = -7.17<ref name=hipparcos/>
| radial_v = −23.54<ref name=drimmel2021/>
| prop_mo_ra = 4.915
| prop_mo_dec = -6.15<ref name=hipparcos/>
| parallax = 7.51
| prop_mo_dec = −11.127
| pm_footnote = <ref name="DR3"/>
| p_error = 0.33
| parallax = 8.9816
| parallax_footnote = <ref name=hipparcos/>
| p_error = 0.4474
| dist_ly = <!--Distance (in light years)-->
| parallax_footnote = <ref name="DR3">{{cite Gaia DR3|2026116260337482112}}</ref>
| dist_pc = <!--Distance (in parsecs)-->
| dist_ly = {{Val|364.8|15.6|15.3}}
| absmag_v = <!--Absolute magnitude ([[UBV photometric system|Johnson-Cousins V system]])-->
| dist_pc = {{val|111.9|4.8|4.7}}
| absmag_bol = <!--Absolute bolometric magnitude (accounts for emissions across all spectra of light)-->
| dist_footnote = <ref name="b-j">{{Cite journal |last1=Bailer-Jones |first1=C. A. L. |last2=Rybizki |first2=J. |last3=Fouesneau |first3=M. |last4=Demleitner |first4=M. |last5=Andrae |first5=R. |date=2021-03-01 |title=Estimating distances from parallaxes. V: Geometric and photogeometric distances to 1.47 billion stars in Gaia Early Data Release 3 |journal=The Astronomical Journal |volume=161 |issue=3 |pages=147 |doi=10.3847/1538-3881/abd806 |doi-access=free |arxiv=2012.05220 |bibcode=2021AJ....161..147B |issn=0004-6256}} Data about this star can be seen [https://dc.zah.uni-heidelberg.de/gedr3dist/q/cone/form here].<br />Beta<sup>1</sup> Cygni = Gaia DR3 2026116260337482112 <br />Beta<sup>2</sup> Cygni = Gaia DR3 2026113339752723456</ref>
}}
}}
{{Starbox astrometry|no_heading=yes
{{Starbox astrometry
|no_heading=yes
| component1 = Albireo Aa
| component1 = Albireo Aa
| absmag_v = −2.45<ref name="ginestet"/>
| absmag_v = −2.45<ref name="ginestet"/>
Line 61: Line 70:
{{Starbox astrometry|no_heading=y
{{Starbox astrometry|no_heading=y
| component1 = Albireo B
| component1 = Albireo B
| radial_v = -18.80<ref name=ascc/>
| radial_v = −18.80<ref name=ascc/>
| prop_mo_ra = -0.953<ref name=dr1/>
| prop_mo_ra = −1.078<ref name="DR3-2"/>
| prop_mo_dec = -1.624<ref name=dr1/>
| prop_mo_dec = −1.540<ref name="DR3-2"/>
| parallax = 8.16
| parallax = 8.1896
| p_error = 0.25
| p_error = 0.0781
| parallax_footnote = <ref name=hipparcos/>
| parallax_footnote = <ref name="DR3-2">{{Cite Gaia DR3|2026113339752723456}}</ref>
| dist_ly = {{val|395.4|2.9|3.3}}
| dist_pc = {{val|121.3|0.9|1}}
| dist_footnote = <ref name="b-j"/>
}}
{{Starbox relpos
| epoch = 2006
| primary = Albireo A
| component = Albireo B
| angdistsec = 35.3
| angdistref = <ref name=wdsb />
| posang = 54
| posangref = <ref name=wdsb />
}}
}}
{{Starbox orbit
{{Starbox orbit
| reference = <ref name=drimmel2021/>
| reference = &nbsp;(Aa/Ac)<ref name=wdsa>Entry, WDS identifier 19307+2758, [http://ad.usno.navy.mil/wds/orb6/orb6frames.html Sixth Catalog of Orbits of Visual Binary Stars] {{Webarchive|url=https://web.archive.org/web/20171112062424/http://ad.usno.navy.mil/wds/orb6/orb6frames.html |date=2017-11-12 }}, William I. Hartkopf & Brian D. Mason, U.S. Naval Observatory. Accessed on line July 9, 2008. [http://ad.usno.navy.mil/wds/orb6/orb6orbits.html#19307+2758 (19307+2758)] {{Webarchive|url=https://web.archive.org/web/20110517115734/http://ad.usno.navy.mil/wds/orb6/orb6orbits.html#19307+2758 |date=2011-05-17 }}</ref>
| primary = <!--Primary name -->
| primary = Aa
| name = <!--Companion name-->
| name = Ac
| period = 213.859
| period = {{val|121.65|3.34|2.90}}
| axis = {{val|0.401|0.007|0.006}}
| axis_unitless = 0.536[[Arcsecond|″]]
| eccentricity = 0.256
| eccentricity = {{val|0.20|0.01|0.02}}
| inclination = 154.9
| inclination = {{val|156.15|2.90|2.63}}
| node = 170.4
| node = {{val|84.43|5.27|4.50}}
| periastron = B1997.995
| periastron = B2026.36
| periarg = 39.4
| periarg = {{val|54.72|1.88|2.24}}
| k1 = {{val|2.91|0.09|0.12}}
}}
}}
{{Starbox detail
{{Starbox detail
| component1 = Albireo Aa
| component1 = Albireo Aa
| component2 = Albireo Ac
| component2 = Albireo Ac
| mass = 14.52<ref name=tokovinin/>
| mass = 5.2<ref name=drimmel2021/>
| mass2 = 3.84<ref name=tokovinin/>
| mass2 = 2.7<ref name=drimmel2021/>
| radius = <!--69<ref name=diameter/>-->
| radius = {{val|58.69|2.83|3.12}}<ref name="npoi"/>
| radius2 =
| radius2 = 3.0{{efn|name=radius2}}
| luminosity_bolometric = 1,200 ± 200<ref name=bsd />
| luminosity_bolometric = 1,259<ref name=drimmel2021/>
| luminosity_bolometric2 = 950 ± 250<ref name=bsd />
| luminosity_bolometric2 = 79<ref name=drimmel2021/>
| temperature = 4,270<ref name=lefevre/>
| temperature = 4,383<ref name=drimmel2021/>
| temperature2 = ~12,000<ref name=ginestet/>–30,000±100<ref name=bsd />
| temperature2 = 10,000<ref name=drimmel2021/>
| rotational_velocity = 1.4<ref name=lefevre/>
| rotational_velocity = 8.34<ref name=drimmel2021/>
| gravity = 2.0<ref name=lefevre/>
| gravity = 0.93<ref name=drimmel2021/>
| metal_fe = −0.1<ref name=lefevre/>
| metal_fe = −0.1<ref name=lefevre/>
}}
}}
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| temperature = 13,200 ± 600<ref name=physparms />
| temperature = 13,200 ± 600<ref name=physparms />
| age_myr = 100<ref name=physparms />
| age_myr = 100<ref name=physparms />
}}
{{Starbox relpos
| reference = <!-- Grand reference -->
| epoch = 2006
| primary = Albireo A
| component = Albireo B
| angdistsec = 35.3
| angdistmas = <!--Angular distance, in milliarcseconds (alternatively, use angdistsec) -->
| angdistref = <ref name=wdsb />
| posang = 54
| posangref = <ref name=wdsb />
| projsep = <!--Observed projected separation, in AU -->
| projsepref = <!--Reference for projected separation -->
}}
}}
{{Starbox catalog
{{Starbox catalog
| names = [[Bayer designation|β&nbsp;Cygni]], [[Flamsteed designation|6&nbsp;Cygni]], [[Aitken Double Star Catalogue|ADS]]&nbsp;12540, [[Catalogue of Components of Double and Multiple Stars|CCDM]]&nbsp;J19307+2758, [[Washington Double Star Catalog|WDS]]&nbsp;19307+2758<ref name=simbada /><ref name=wdsa /><ref name=pisco />
| names = [[Bayer designation|β&nbsp;Cygni]], [[Flamsteed designation|6&nbsp;Cygni]], [[Aitken Double Star Catalogue|ADS]]&nbsp;12540, [[Catalogue of Components of Double and Multiple Stars|CCDM]]&nbsp;J19307+2758, [[Washington Double Star Catalog|WDS]]&nbsp;19307+2758<ref name=simbada /><ref name=wdsa /><ref name=pisco />
| component2 = AlbireoA
| component2 = Albireo A
| names2 = β¹&nbsp;Cygni, [[Bonner Durchmusterung|BD]]+27&nbsp;3410, [[Bright Star Catalogue|HR]]&nbsp;7417, [[Henry Draper Catalogue|HD]]&nbsp;183912/183913, [[Hipparcos Catalogue|HIP]]&nbsp;95947, [[Smithsonian Astrophysical Observatory Star Catalogue|SAO]]&nbsp;87301, [[Catalogues of Fundamental Stars|FK5]]&nbsp;732, [[Double star designation|MCA]]&nbsp;55&nbsp;Aac, NSV&nbsp;12105
| names2 = β¹&nbsp;Cygni, [[Bonner Durchmusterung|BD]]+27&nbsp;3410, [[Bright Star Catalogue|HR]]&nbsp;7417, [[Henry Draper Catalogue|HD]]&nbsp;183912/183913, [[Hipparcos Catalogue|HIP]]&nbsp;95947, [[Smithsonian Astrophysical Observatory Star Catalogue|SAO]]&nbsp;87301, [[Catalogues of Fundamental Stars|FK5]]&nbsp;732, [[Double star designation|MCA]]&nbsp;55&nbsp;Aac, NSV&nbsp;12105
| component3 = AlbireoB
| component3 = Albireo B
| names3 = β²&nbsp;Cygni, [[Double star designation|STF&nbsp;4043B]], [[Bonner Durchmusterung|BD]]+27&nbsp;3411,
| names3 = β²&nbsp;Cygni, [[Double star designation|STF&nbsp;4043B]], [[Bonner Durchmusterung|BD]]+27&nbsp;3411,
[[Henry Draper Catalogue|HD]]&nbsp;183914, [[Hipparcos Catalogue|HIP]]&nbsp;95951, [[Bright Star Catalogue|HR]]&nbsp;7418, [[Smithsonian Astrophysical Observatory Star Catalogue|SAO]]&nbsp;87302<ref name=simbadb />
[[Henry Draper Catalogue|HD]]&nbsp;183914, [[Hipparcos Catalogue|HIP]]&nbsp;95951, [[Bright Star Catalogue|HR]]&nbsp;7418, [[Smithsonian Astrophysical Observatory Star Catalogue|SAO]]&nbsp;87302<ref name=simbadb />
Line 134: Line 143:
{{Starbox end}}
{{Starbox end}}


'''Albireo''' {{IPAc-en|æ|l|'|b|ɪr|i|ou}}<!--and yes, the 'e' is short in Latin, so the stress is on the ante-penult--><ref name=Kunitzsch/> is a [[double star]] designated '''Beta Cygni''' ('''β Cygni''', abbreviated '''Beta Cyg''', '''β Cyg'''). The [[International Astronomical Union]] uses the name "Albireo" specifically for the brightest star in the system.<ref name="IAU-CSN"/> Although designated '[[beta]]', it is fainter than [[Gamma Cygni]], [[Delta Cygni]], and [[Epsilon Cygni]] and is the [[List of stars in Cygnus|fifth-brightest point of light]] in the [[constellation]] of [[Cygnus (constellation)|Cygnus]]. Appearing to the naked eye to be a single star of [[Apparent magnitude|magnitude]] 3, viewing through even a low-magnification [[telescope]] resolves it into its two components. The brighter yellow star, itself a very close [[binary star|binary system]], makes a striking colour contrast with its fainter blue companion.<ref name=stars/>
The '''Albireo''' {{IPAc-en|æ|l|'|b|ɪr|i|ou}}<!--and yes, the 'e' is short in Latin, so the stress is on the ante-penult--><ref name=Kunitzsch>{{cite book
|last=Kunitzsch |first=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> system is a [[double star]] designated '''Beta Cygni''' ('''β Cygni''', abbreviated '''Beta Cyg''', '''β Cyg'''). The [[International Astronomical Union]] uses the name "Albireo" specifically for the brightest star in the system.<ref name="IAU-CSN">{{cite web | url=http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt | title=IAU Catalog of Star Names |accessdate=28 July 2016}}</ref> Although designated '[[beta]]', it is fainter than [[Gamma Cygni]], [[Delta Cygni]], and [[Epsilon Cygni]] and is the [[List of stars in Cygnus|fifth-brightest point of light]] in the [[constellation]] of [[Cygnus (constellation)|Cygnus]]. Appearing to the naked eye to be a single star of [[Apparent magnitude|magnitude]] 3, viewing through even a low-magnification [[telescope]] resolves it into its two components. The brighter yellow star (actually itself a very close [[binary star|binary system]]) makes a striking colour contrast with its fainter blue companion.<ref name=stars/>


==Nomenclature==
==Nomenclature==
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''β Cygni'' ([[Latinisation of names|Latinised]] to ''Beta Cygni'') is the system's [[Bayer designation]]. The brighter of the two components is designated ''β¹ Cygni'' or ''Beta Cygni A'' and the fainter ''β² Cygni'' or ''Beta Cygni B''.
''β Cygni'' ([[Latinisation of names|Latinised]] to ''Beta Cygni'') is the system's [[Bayer designation]]. The brighter of the two components is designated ''β¹ Cygni'' or ''Beta Cygni A'' and the fainter ''β² Cygni'' or ''Beta Cygni B''.


The system's traditional name ''Albireo'' is a result of misunderstanding and mistranslation. It is thought that it originated in the [[Greek language|Greek]] name ''{{lang|grc-Latn|ornis}}'' for the constellation of Cygnus, which became ''{{transl|ar|urnis}}'' in [[Arabic]].<ref>p. 24, [https://archive.org/details/namesstarsandco00higggoog ''The names of the stars and constellations compiled from the Latin, Greek and Arabic''], W. H. Higgins, Leicester: Samuel Clarke, 1882.</ref> When translated into [[Latin language|Latin]], this name was thought to refer to the Greek name ''Erysimon'' for the plant called Hedge Mustard (''[[Sisymbrium officinale]]'', which in Latin is ''ireo''), and so was described in Latin in the [[Arabo-Latin Almagest]] of 1515 as "''Eurisim: et est volans; et jam vocatur gallina. et dicitur eurisim quasi redolens ut lilium ab ireo''" ("Eurisim: and it is the flyer, and now it is called the hen, and it is called Eurisim, as if redolent like the lily from the 'ireo'"), via a confusion between ''ireo'' and the scented flower ''[[Iris florentina]]''. This was variously miscopied, until "''ab ireo''" was treated as a miscopy of an Arabic term and changed into ''{{transl|ar|al-bireo}}''.<ref>p. 194, Allen.</ref><ref>http://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Cygnus*.html</ref>
The origin of the star system's traditional name ''Albireo'' is unclear. [[Christian Ludwig Ideler]] traced it to [https://viewer.slv.vic.gov.au/?entity=IE10167306&file=FL21840507&mode=browse the heading for the constellation we call Cygnus] in Ptolemy's star catalog, in the translation of the [[Almagest]] by [[Gerard of Cremona]]: "''Stellatio Eurisim: et est volans; et jam vocatur gallina. et dicitur eurisim quasi redolens ut lilium ab ireo''" ("Constellation Eurisim: and it is the Flyer, and it is also called the Hen, and it is called Eurisim as if redolent like the lily from the 'ireo'"). (The original Greek just calls the constellation "Ορνιθος αστερισμος", "the constellation of the Bird".) The word "ireo" is obscure as well{{snd}}Ideler suggests that Gerard took "Eurisim" to mean the plant ''[[Erysimum]]'', which is called ''[[wikt:irio|irio]]'' in Latin, but the ablative case of that is not "ireo" but ''irione''.<ref>p. 24, [https://archive.org/details/namesstarsandco00higggoog/page/n27/mode/2up ''The names of the stars and constellations compiled from the Latin, Greek and Arabic''], W. H. Higgins, Leicester: Samuel Clarke, 1882.</ref> In any case, Ideler proposed that (somehow) the phrase "ab ireo" was applied to the star at the head of the bird, and this became "Albireo" when an "l" was mistakenly inserted as though it was an Arabic name.<ref>{{Cite web|url=https://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Cygnus*.html|title=LacusCurtius • Allen's Star Names — Cygnus}} Allen quotes (in translation) a passage from Ideler's ''Untersuchungen über den Ursprung und die Bedeutung der Sternnamen'' (1809), [https://archive.org/details/untersuchungenb01idelgoog/page/n115/mode/2up page 75].</ref> Ideler also supposed that the name Eurisim was a mistaken transliteration of the Arabic name "Urnis" for Cygnus (from the Greek "Ορνις").


In 2016, the [[International Astronomical Union]] organized a [[IAU Working Group on Star Names|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)|accessdate=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 |accessdate=28 July 2016}}</ref> included a table of the first two batches of names approved by the WGSN; which included ''Albireo '' for β¹ Cygni. It is now so entered in the IAU Catalog of Star Names.<ref name="IAU-CSN"/>
In 2016, the [[International Astronomical Union]] organized a [[IAU Working Group on Star Names|Working Group on Star Names]] (WGSN)<ref name="WGSN"/> to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016<ref name="WGSN1"/> included a table of the first two batches of names approved by the WGSN; which included ''Albireo '' for β¹ Cygni. It is now so entered in the IAU Catalog of Star Names.<ref name="IAU-CSN"/>


Medieval Arabic-speaking astronomers called Beta Cygni ''{{transl|ar|minqār al-dajāja<sup>h</sup>}}'' (English: ''the hen's beak'').<ref>p. 196, [https://archive.org/details/bub_gb_5xQuAAAAIAAJ ''Star-names and Their Meanings''], Richard Hinckley Allen, New York, G. E. Stechert, 1899.</ref> The term ''{{transl|ar|minqār al-dajāja<sup>h</sup>}}'' (منقار الدجاجة) or ''Menchir al Dedjadjet'' appeared in the catalogue of stars in the ''Calendarium of Al Achsasi Al Mouakket'', which was translated into [[Latin]] as ''Rostrum Gallinae'', meaning ''the hen's beak''.<ref>{{cite journal
Medieval Arabic-speaking astronomers called Beta Cygni ''{{transl|ar|minqār al-dajāja<sup>h</sup>}}'' (English: ''the hen's beak'').<ref>p. 196, [https://archive.org/details/bub_gb_5xQuAAAAIAAJ ''Star-names and Their Meanings''], Richard Hinckley Allen, New York, G. E. Stechert, 1899.</ref> The term ''{{transl|ar|minqār al-dajāja<sup>h</sup>}}'' (منقار الدجاجة) or ''Menchir al Dedjadjet'' appeared in the catalogue of stars in the ''Calendarium of Al Achsasi Al Mouakket'', which was translated into [[Latin]] as ''Rostrum Gallinae'', meaning ''the hen's beak''.<ref name=knobel1895/>
| last=Knobel | first=E. B.
| title=Al Achsasi Al Mouakket, on a catalogue of stars in the Calendarium of Mohammad Al Achsasi Al Mouakket
| journal=[[Monthly Notices of the Royal Astronomical Society]]
| volume=55 | issue=8
| page=429 |date=June 1895
| bibcode=1895MNRAS..55..429K | doi=10.1093/mnras/55.8.429| doi-access=free}}</ref>


Since Cygnus is the swan, and Beta Cygni is located at the head of the swan, it is sometimes called the "beak star".<ref>p. 416, ''In Quest of the Universe'', Theo Koupelis and Karl F. Kuhn, 5th ed., Sudbury, Massachusetts: Jones & Bartlett Publishers, 2007, {{ISBN|0-7637-4387-9}}.</ref> With [[Deneb]], [[Gamma Cygni]] (Sadr), [[Delta Cygni]], and [[Epsilon Cygni]] (Gienah), it forms the [[Asterism (astronomy)|asterism]] called the [[Northern Cross (asterism)|Northern Cross]].<ref>[http://www.daviddarling.info/encyclopedia/N/Northern_Cross.html Northern Cross] {{Webarchive|url=https://web.archive.org/web/20080708231645/http://www.daviddarling.info/encyclopedia/N/Northern_Cross.html |date=2008-07-08 }}, entry, ''The Internet Encyclopedia of Science'', David Darling. Accessed on line July 24, 2008.</ref>
Since Cygnus is the swan, and Beta Cygni is located at the head of the swan, it is sometimes called the "beak star".<ref>p. 416, ''In Quest of the Universe'', Theo Koupelis and Karl F. Kuhn, 5th ed., Sudbury, Massachusetts: Jones & Bartlett Publishers, 2007, {{ISBN|0-7637-4387-9}}.</ref> With [[Deneb]], [[Gamma Cygni]] (Sadr), [[Delta Cygni]], and [[Epsilon Cygni]] (Gienah), it forms the [[Asterism (astronomy)|asterism]] called the [[Northern Cross (asterism)|Northern Cross]].<ref name=darling/>


==Properties==
==Properties==
[[File:NewAlbireo.jpg|thumb|left|Albireo A and B]]
[[File:NewAlbireo.jpg|thumb|left|Albireo A and B]]
Beta Cygni is about {{convert|415|ly|pc|lk=on}} away from the [[Sun]]. When viewed with the naked eye, Albireo appears to be a single star. However, in a [[telescope]] it resolves into a [[double star]] consisting of β Cygni A (amber, [[apparent magnitude]] 3.1), and β Cygni B (blue-green, apparent magnitude 5.1).<ref name=msg /> Separated by 35 seconds of arc,<ref name=wdsb>Entry, [http://ad.usno.navy.mil/wds/wdsnewframe4.html The Washington Double Star Catalog], identifier 19307+2758, discoverer identifier STFA 43. Accessed on line July 9, 2008. {{webarchive |url=https://web.archive.org/web/20080908010456/http://ad.usno.navy.mil/wds/wdsnewframe4.html |date=8 September 2008 }}</ref> the two components provide one of the best contrasting double stars in the sky due to their different colors.
Beta Cygni is about {{convert|420|ly|pc|0|lk=on}} away from the [[Sun]].<ref name=drimmel2021/> When viewed with the naked eye, Albireo appears to be a single star. However, in a [[telescope]] it resolves into a [[double star]] consisting of β Cygni A (amber, [[apparent magnitude]] 3.1), and β Cygni B (blue-green, apparent magnitude 5.1).<ref name=msg /> Separated by 35 seconds of arc,<ref name=wdsb>Entry, [http://ad.usno.navy.mil/wds/wdsnewframe4.html The Washington Double Star Catalog], identifier 19307+2758, discoverer identifier STFA 43. Accessed on line July 9, 2008. {{webarchive |url=https://web.archive.org/web/20080908010456/http://ad.usno.navy.mil/wds/wdsnewframe4.html |date=8 September 2008 }}</ref> the two components provide one of the best contrasting double stars in the sky due to their different colors.


It is not known whether the two components β Cygni A and B are orbiting around each other in a physical [[binary star|binary system]], or if they are merely an [[double star|optical double]]. If they are a physical binary, their orbital period is probably at least 100,000 years.<ref name=msg>p. 46, ''The Monthly Sky Guide'', Ian Ridpath, Wil Tirion, Cambridge University Press, 2006, {{ISBN|0-521-68435-8}}.</ref> Some experts, however, support the optical double argument, based on observations that suggest different [[proper motion]]s for the components, which implies that they are unrelated.<ref name="SkyTel1">{{cite news
It is not known whether the two components β Cygni A and B are orbiting around each other in a physical [[binary star|binary system]], or if they are merely an [[double star|optical double]].<ref name=drimmel2021/> If they are a physical binary, their orbital period is probably at least 100,000 years.<ref name=msg>p. 46, ''The Monthly Sky Guide'', Ian Ridpath, Wil Tirion, Cambridge University Press, 2006, {{ISBN|0-521-68435-8}}.</ref> Some experts, however, support the optical double argument, based on observations that suggest different [[proper motion]]s for the components, which implies that they are unrelated.<ref name="SkyTel1"/> The primary and secondary also have different measured distances from the [[Hipparcos]] mission – {{convert|133 ± 6|pc|ly|lk=on|order=flip}} for the primary and {{convert|123 ± 4|pc|ly|lk=on|order=flip}} for the secondary.<ref name=hipparcos/> More recently the [[Gaia (spacecraft)|Gaia]] mission has measured distances of about 330–390 light years (100–120 parsecs) for both components, but noise in the astrometric measurements for the stars means that data from Gaia's second data release is not yet sufficient to determine whether the stars are physically associated.<ref name=dr2distances/>

|url=http://www.skyandtelescope.com/observing/will-the-real-albireo-please-stand-up/
In around 3.87 million years, Albireo will become [[historical brightest stars|the brightest star]] in the night sky.<ref name=tomkin1998>{{cite journal|last=Tomkin|first=Jocelyn|date=April 1998|title=Once and Future Celestial Kings|journal=Sky and Telescope|volume=95|issue=4|pages=59–63|bibcode=1998S&T....95d..59T}} – based on computations from [[HIPPARCOS]] data. (The calculations exclude stars whose distance or [[proper motion]] is uncertain.) [ftp://tlgleonid.asuscomm.com/HITACHI/BOOK_ASTRO/S&T/SkyandTelescope_1998%20-%20astronomy/04/199804059063.pdf PDF]{{dead link|date=November 2017 |bot=InternetArchiveBot |fix-attempted=yes }}</ref> It will peak in brightness with an apparent magnitude of –0.53 in 4.61 million years.<ref name=tomkin1998 />
|title=Will the Real Albireo Please Stand Up?
|author=Bob King
|date=September 21, 2016
|work=Sky and Telescope
|accessdate=October 14, 2016}}
</ref> The primary and secondary also have different measured distances from the [[Hipparcos]] mission – {{convert|133 ± 6|pc|ly|lk=on|order=flip}} for the primary and {{convert|123 ± 4|pc|ly|lk=on|order=flip}} for the secondary.<ref name=hipparcos/> More recently the [[Gaia (spacecraft)|Gaia]] mission has measured distances of about 330–390 light years (100–120 parsecs) for both components, but noise in the astrometric measurements for the stars means that data from Gaia's second data release is not yet sufficient to determine whether the stars are physically associated.<ref name=dr2distances>{{Cite journal|arxiv=1804.10121|last1=Bailer-Jones|first1=C. A. L|title=Estimating distances from parallaxes IV: Distances to 1.33 billion stars in Gaia Data Release 2|journal=The Astronomical Journal|volume=156|issue=2|pages=58|last2=Rybizki|first2=J|last3=Fouesneau|first3=M|last4=Mantelet|first4=G|last5=Andrae|first5=R|doi=10.3847/1538-3881/aacb21|year=2018|bibcode=2018AJ....156...58B}}</ref>


There are a further 10 faint companions listed in the Washington Double Star catalogue, all fainter than magnitude 10. Only one is closer to the primary than Albireo B, with the others up to 142" away.<ref name=wdsa/>
There are a further 10 faint companions listed in the Washington Double Star catalogue, all fainter than magnitude 10. Only one is closer to the primary than Albireo B, with the others up to 142" away.<ref name=wdsa>Entry, WDS identifier 19307+2758, [http://ad.usno.navy.mil/wds/orb6/orb6frames.html Sixth Catalog of Orbits of Visual Binary Stars] {{Webarchive|url=https://web.archive.org/web/20171112062424/http://ad.usno.navy.mil/wds/orb6/orb6frames.html |date=2017-11-12 }}, William I. Hartkopf & Brian D. Mason, U.S. Naval Observatory. Accessed on line July 9, 2008. [http://ad.usno.navy.mil/wds/orb6/orb6orbits.html#19307+2758 (19307+2758)] {{Webarchive|url=https://web.archive.org/web/20110517115734/http://ad.usno.navy.mil/wds/orb6/orb6orbits.html#19307+2758 |date=2011-05-17 }}</ref>


===Albireo A===
===Albireo A===
The [[stellar spectrum|spectrum]] of Beta Cygni A was found to be composite when it was observed as part of the [[Henry Draper]] Memorial project in the late 19th century, leading to the supposition that it was itself double.<ref>{{cite journal|bibcode=1897AnHar..28....1M|title=Spectra of bright stars photographed with the 11-inch Draper Telescope as part of the Henry Draper Memorial|journal=Annals of Harvard College Observatory|volume=28|pages=1|last1=Maury|first1=Antonia C.|last2=Pickering|first2=Edward C.|year=1897}}</ref> This was supported by observations from 1898 to 1918 which showed that it had a varying [[radial velocity]].<ref>{{cite journal|bibcode=1919PASP...31...38C|title=The Variable Velocity of β Cygni|journal=Publications of the Astronomical Society of the Pacific|volume=31|issue=179|pages=38|last1=Campbell|first1=W. W.|year=1919|doi=10.1086/122807|doi-access=free}}</ref> In 1923, the two components were identified in the [[Henry Draper Catalogue]] as HD 183912 and HD 183913.<ref>{{cite web|url=http://freestarcharts.com/index.php/17-guides/stars/171-albireo-beta-cygni-abeta-cyg-double-star?tmpl=component|title=freestarcharts.com|accessdate=2017-06-11}}</ref><ref>{{cite journal|bibcode=1923AnHar..98....1C|title=The Henry Draper catalogue : 19h and 20h|journal=Annals of the Astronomical Observatory of Harvard College |volume=98|pages=1|last1=Cannon|first1=Annie Jump|last2=Pickering|first2=Edward Charles|year=1923}}. See note re HD&nbsp;183912,3,4 on this page.</ref>
The [[stellar spectrum|spectrum]] of Beta Cygni A was found to be composite when it was observed as part of the [[Henry Draper]] Memorial project in the late 19th century, leading to the supposition that it was itself double.<ref name=maury1897/> This was supported by observations from 1898 to 1918 which showed that it had a varying [[radial velocity]].<ref name=campbell1919/> In 1923, the two components were identified in the [[Henry Draper Catalogue]] as HD 183912 and HD 183913.<ref name=freestarcharts/><ref name=hd/>


In 1978, speckle interferometry observations using the 1.93m telescope at the [[Haute-Provence Observatory]] resolved a companion at 0.125". This observation was published in 1980,<ref name=bonneau>{{cite journal|bibcode=1980A&A....86..295B|title=Speckle interferometric observations of binary systems with the Haute-Provence 1.93 M telescope|journal=Astronomy and Astrophysics|volume=86|pages=295|last1=Bonneau|first1=D.|last2=Foy|first2=R.|year=1980}}</ref> and the companion is referred to as component Ab in the [[Washington Double Star Catalog]].<ref name=wdsa/>
In 1978, speckle interferometry observations using the 1.93m telescope at the [[Haute-Provence Observatory]] resolved a companion at 0.125". This observation was published in 1980,<ref name=bonneau/> and the companion is referred to as component Ab in the [[Washington Double Star Catalog]].<ref name=wdsa/>


In 1976 [[speckle interferometry]] was used to resolve a companion using the 2.1-meter telescope at the [[Kitt Peak National Observatory]]. It was measured at a separation of 0.44", and it is noted that the observation was inconsistent with the Haute-Provence observations and hence not of the same star.<ref name=pisco>{{cite journal|bibcode=2008AN....329...54S|doi=10.1002/asna.200710834|title=Speckle observations with PISCO in Merate: IV. Astrometric measurements of visual binaries in 2005|journal=Astronomische Nachrichten|volume=329|issue=1|pages=54–68|year=2008|last1=Scardia|first1=M.|last2=Prieur|first2=J.-L.|last3=Pansecchi|first3=L.|last4=Argyle|first4=R.W.|last5=Sala|first5=M.|last6=Basso|first6=S.|last7=Ghigo|first7=M.|last8=Koechlin|first8=L.|last9=Aristidi|first9=E.|url=https://hal.archives-ouvertes.fr/hal-02113024/file/scard07a_MerIV.pdf}}</ref><ref>{{cite journal|bibcode=1982ApJS...48..273M|doi=10.1086/190778|title=Speckle interferometric measurements of binary stars. VI|journal=The Astrophysical Journal Supplement Series|volume=48|pages=273|year=1982|last1=McAlister|first1=H. A.|last2=Hendry|first2=E. M.}}</ref> Although these observations pre-dated those at Haute-Provence, they were not published until 1982 and this component is designated Ac in the Washington Double Star Catalog.<ref name=wdsa/> It is designated as component C in the [[Catalog of Components of Double and Multiple Stars]],<ref name=ccdm>{{cite journal|bibcode=1994CoORB.115....1D|title=Catalogue des composantes d'etoiles doubles et multiples (CCDM) premiere edition - Catalogue of the components of double and multiple stars (CCDM) first edition|journal=Com. De l'Observ. Royal de Belgique|volume=115|pages=1|last1=Dommanget|first1=J.|last2=Nys|first2=O.|year=1994}}</ref> not to be confused with component C in the Washington Double Star Catalog which is a faint optical companion.<ref name=wdsa/> An orbit for the pair has since been computed using interferometric measurements, but as only approximately a quarter of the orbit has been observed, the orbital parameters must be regarded as preliminary. The period of this orbit is 214 years.<ref name=pisco/>
In 1976 [[speckle interferometry]] was used to resolve a companion using the 2.1-meter telescope at the [[Kitt Peak National Observatory]]. It was measured at a separation of 0.44", and it is noted that the observation was inconsistent with the Haute-Provence observations and hence not of the same star.<ref name=pisco/><ref name=mcalister1982/> Although these observations pre-dated those at Haute-Provence, they were not published until 1982 and this component is designated Ac in the Washington Double Star Catalog.<ref name=wdsa/> It is designated as component C in the [[Catalog of Components of Double and Multiple Stars]],<ref name=ccdm/> not to be confused with component C in the Washington Double Star Catalog which is a faint optical companion.<ref name=wdsa/> An orbit for the pair has since been computed using interferometric measurements, but as only approximately a quarter of the orbit has been observed, the orbital parameters must be regarded as preliminary. The period of this orbit is 214 years.<ref name=pisco/> The confirmed close pair are referred to as Aa and Ac in modern papers, with Ab being the unconfirmed third component.<ref name=drimmel2021/>


The diameter of the primary K-type giant star has been measured using [[interferometry]] from the [[Navy Precision Optical Interferometer]]. A [[Limb darkening|limb-darkened]] angular diameter of {{val|4.904|ul=mas}} was measured. At the [[parallax]]-derived distance of 111.4{{nbsp}}pc, a radius equivalent to {{solar radius|58.69|link=y}} is calculated.<ref name="npoi">{{Citation|last1=Baines |first1=Ellyn K. |last2=Clark |first2=James H., III |last3=Schmitt |first3=Henrique R. |last4=Stone |first4=Jordan M. |last5=von Braun |first5=Kaspar |date=2023-12-01 |title=33 New Stellar Angular Diameters from the NPOI, and Nearly 180 NPOI Diameters as an Ensemble |journal=The Astronomical Journal |volume=166 |issue=6 |pages=268 |doi=10.3847/1538-3881/ad08be |doi-access=free |bibcode=2023AJ....166..268B |issn=0004-6256}}</ref>
The status of the two possible companions is still not clarified.<ref name=roberts>{{cite journal|bibcode=2007AJ....133..545R|title=Adaptive Optics Photometry and Astrometry of Binary Stars. II. A Multiplicity Survey of B Stars|journal=The Astronomical Journal|volume=133|issue=2|pages=545|last1=Roberts|first1=Lewis C.|last2=Turner|first2=Nils H.|last3=Ten Brummelaar|first3=Theo A.|year=2007|doi=10.1086/510335|url=http://joy.chara.gsu.edu/~nils/2007AJ....133..545R.pdf}}</ref> One set of observations reports barely resolving two components, but there has not been confirmation of this.<ref name=prieur>{{cite journal|bibcode=2002ApJS..142...95P|title=Speckle Observations of Composite Spectrum Stars with PISCO in 1993–1998|journal=The Astrophysical Journal Supplement Series|volume=142|issue=1|pages=95–104|last1=Prieur|first1=J.-L.|last2=Koechlin|first2=L.|last3=Ginestet|first3=N.|last4=Carquillat|first4=J.-M.|last5=Aristidi|first5=E.|last6=Scardia|first6=M.|last7=Arnold|first7=L.|last8=Avila|first8=R.|last9=Festou|first9=M. C.|last10=Morel|first10=S.|last11=Pérez|first11=J.-P.|year=2002|doi=10.1086/341094|doi-access=free}}</ref> Observations of Albireo assuming the spectrum is a composite of two stars derive a late B spectral type for the companion,<ref name=mk>{{cite journal|bibcode=2014yCat....1.2023S|title=VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009–2016)|journal=VizieR On-line Data Catalog: B/Mk. Originally Published in: Lowell Observatory (October 2014)|volume=1|last1=Skiff|first1=B. A.|year=2014}}</ref> for example B8.<ref name=ginestet/> [[Adaptive optics]] measurements of the companion are best modelled by a B0V spectrum for the companion with an apparent magnitude of 5.85.<ref name=bsd/> Different assumptions about the spectral type of the companion lead to wildly different physical properties, for example an [[effective temperature]] of either 12,000 K or 30,000 K.<ref name=ginestet/><ref name=bsd/>

The diameter of the primary K-type giant star has been measured using [[interferometry]]. A uniform disk of approximately 4.5 mas was measured at optical and near-[[infrared]] wavelengths, and a [[Limb darkening|limb-darkened]] diameter of 4.834 mas was calculated, equivalent to a radius of {{solar radius|69|link=y}} at a distance of 133 pc.<ref name=diameter>{{cite journal|doi=10.1086/378596|title=Angular Diameters of Stars from the Mark III Optical Interferometer|journal=The Astronomical Journal|volume=126|issue=5|pages=2502|year=2003|last1=Mozurkewich|first1=D.|last2=Armstrong|first2=J. T.|last3=Hindsley|first3=R. B.|last4=Quirrenbach|first4=A.|last5=Hummel|first5=C. A.|last6=Hutter|first6=D. J.|last7=Johnston|first7=K. J.|last8=Hajian|first8=A. R.|last9=Elias Ii|first9=Nicholas M.|last10=Buscher|first10=D. F.|last11=Simon|first11=R. S.|bibcode = 2003AJ....126.2502M }}</ref>


===Albireo B===
===Albireo B===
β Cygni B is a fast-rotating [[Be star]], with an equatorial rotational velocity of at least 250 kilometers per second.<ref name="stars"/> Its surface temperature has been [[spectroscopy|spectroscopically]] estimated to be about 13,200 [[Kelvin|K]].<ref name=physparms>Table 1, {{cite journal | doi = 10.1086/381063 | bibcode = 2004AJ....127.1176L | volume=127 | title=Physical Parameters of Southern B- and Be-Type Stars | year=2004 | journal=The Astronomical Journal | pages=1176–1180 | last1 = Levenhagen | first1 = R. S.}}</ref>
β Cygni B is a fast-rotating [[Be star]], with an equatorial rotational velocity of at least 250 kilometers per second.<ref name="stars"/> Its surface temperature has been [[spectroscopy|spectroscopically]] estimated to be about 13,200 [[Kelvin|K]].<ref name=physparms/>


β Cygni B has been reported to be a very close double,<ref name=roberts/> but the observations appear to have been incorrect.<ref name=wdsa/>
β Cygni B has been reported to be a very close double,<ref name=roberts/> but the observations appear to have been incorrect.<ref name=wdsa/>

==Moving group==
Analysis of [[Gaia Data Release 2]] astrometry suggests that four fainter stars may form a [[moving group]] along with the brighter visible components.<ref name=drimmel2021/>


==Namesakes==
==Namesakes==
[[USS Albireo (AK-90)|''Albireo'' (AK-90)]] was a [[United States Navy]] [[Crater class cargo ship]] named after the star.
[[USS Albireo (AK-90)|''Albireo'' (AK-90)]] was a [[United States Navy]] [[Crater-class cargo ship|''Crater''-class cargo ship]] named after the star.

==Notes==
{{notelist|refs=

{{efn | name=radius2 | Applying the [[Stefan-Boltzmann Law]] with a nominal [[sun|solar]] [[effective temperature]] of 5,772&nbsp;[[Kelvin|K]]:
:<math>\sqrt{(5772/10000)^4 * 79} = 2.96\ R\odot</math>}}

}}


==References==
==References==
Line 206: Line 206:
<ref name=simbadb>{{SIMBAD link|HD+183914|HD 183914 -- Emission-line Star}}, database entry, [[SIMBAD]]. Accessed on line July 9, 2008.</ref>
<ref name=simbadb>{{SIMBAD link|HD+183914|HD 183914 -- Emission-line Star}}, database entry, [[SIMBAD]]. Accessed on line July 9, 2008.</ref>


<ref name=edr3B>{{cite Gaia EDR3|2026113339752723456}}</ref>
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<ref name=bsd>{{cite journal|bibcode=2000AJ....119.2403T|title=Binary Star Differential Photometry Using the Adaptive Optics System at Mount Wilson Observatory|journal=The Astronomical Journal|volume=119|issue=5|pages=2403|last1=Ten Brummelaar|first1=Theo|last2=Mason|first2=Brian D|last3=McAlister|first3=Harold A|last4=Roberts|first4=Lewis C|last5=Turner|first5=Nils H|last6=Hartkopf|first6=William I|last7=Bagnuolo|first7=William G|year=2000|doi=10.1086/301338|doi-access=free}}. See tables 4, 5, 6, and 8. Luminosity from L<sub>bol</sub>=10<sup>2(4.75−M<sub>bol</sub>)/5</sup>.</ref>
<ref name=bsd>{{cite journal|bibcode=2000AJ....119.2403T|title=Binary Star Differential Photometry Using the Adaptive Optics System at Mount Wilson Observatory|journal=The Astronomical Journal|volume=119|issue=5|pages=2403|last1=Ten Brummelaar|first1=Theo|last2=Mason|first2=Brian D|last3=McAlister|first3=Harold A|last4=Roberts|first4=Lewis C|last5=Turner|first5=Nils H|last6=Hartkopf|first6=William I|last7=Bagnuolo|first7=William G|year=2000|doi=10.1086/301338|doi-access=free}}. See tables 4, 5, 6, and 8. Luminosity from L<sub>bol</sub>=10<sup>2(4.75−M<sub>bol</sub>)/5</sup>.</ref>
Line 212: Line 212:
<ref name=photometry>{{cite journal|bibcode=2002yCat.2237....0D|title=VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system|journal=CDS/ADC Collection of Electronic Catalogues|volume=2237|last1=Ducati|first1=J. R|year=2002}}</ref>
<ref name=photometry>{{cite journal|bibcode=2002yCat.2237....0D|title=VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system|journal=CDS/ADC Collection of Electronic Catalogues|volume=2237|last1=Ducati|first1=J. R|year=2002}}</ref>


<ref name=levenhagen>{{cite journal|bibcode=2006MNRAS.371..252L|arxiv=astro-ph/0606149|title=Spectroscopic analysis of southern B and Be stars|journal=Monthly Notices of the Royal Astronomical Society|volume=371|issue=1|pages=252–262|last1=Levenhagen|first1=R. S|last2=Leister|first2=N. V|year=2006|doi=10.1111/j.1365-2966.2006.10655.x}}</ref>
<ref name=levenhagen>{{cite journal|bibcode=2006MNRAS.371..252L|arxiv=astro-ph/0606149|title=Spectroscopic analysis of southern B and Be stars|journal=Monthly Notices of the Royal Astronomical Society|volume=371|issue=1|pages=252–262|last1=Levenhagen|first1=R. S|last2=Leister|first2=N. V|year=2006|doi=10.1111/j.1365-2966.2006.10655.x|s2cid=16492030}}</ref>


<ref name=simbada>{{SIMBAD link|NAME+ALBIREO|NAME ALBIREO -- Star in double system }}, database entry, [[SIMBAD]]. Accessed on line July 9, 2008.</ref>
<ref name=simbada>{{SIMBAD link|NAME+ALBIREO|NAME ALBIREO -- Star in double system }}, database entry, [[SIMBAD]]. Accessed on line July 9, 2008.</ref>


<ref name=rv>{{cite journal|bibcode=2005A&A...430..165F|title=Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters|journal=Astronomy and Astrophysics|volume=430|pages=165–186|last1=Famaey|first1=B|last2=Jorissen|first2=A|last3=Luri|first3=X|last4=Mayor|first4=M|last5=Udry|first5=S|last6=Dejonghe|first6=H|last7=Turon|first7=C|year=2005|doi=10.1051/0004-6361:20041272|arxiv=astro-ph/0409579}}</ref>
<ref name=ascc>{{cite journal|bibcode= 2007AN....328..889K |title= Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ˜55000 stars and mean radial velocities of 516 Galactic open clusters and associations |journal= Astronomische Nachrichten |volume= 328 |issue= 9 |pages= 889 |last1= Kharchenko |first1= N. V |last2= Scholz |first2= R.-D |last3= Piskunov |first3= A. E |last4= Röser |first4= S |last5= Schilbach |first5= E |year= 2007 |doi= 10.1002/asna.200710776 |arxiv= 0705.0878 |s2cid= 119323941 }}</ref>

<ref name=ascc>{{cite journal|bibcode= 2007AN....328..889K |title= Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ˜55000 stars and mean radial velocities of 516 Galactic open clusters and associations |journal= Astronomische Nachrichten |volume= 328 |issue= 9 |pages= 889 |last1= Kharchenko |first1= N. V |last2= Scholz |first2= R.-D |last3= Piskunov |first3= A. E |last4= Röser |first4= S |last5= Schilbach |first5= E |year= 2007 |doi= 10.1002/asna.200710776 |arxiv= 0705.0878 }}</ref>


<ref name=lefevre>{{cite journal|bibcode=2006A&A...450.1173L|title=Lithium abundances and rotational behavior for bright giant stars|journal=Astronomy and Astrophysics|volume=450|issue=3|pages=1173|last1=Lèbre|first1=A.|last2=De Laverny|first2=P.|last3=Do Nascimento|first3=J. D.|last4=De Medeiros|first4=J. R.|year=2006|doi=10.1051/0004-6361:20053485|doi-access=free}}</ref>
<ref name=lefevre>{{cite journal|bibcode=2006A&A...450.1173L|title=Lithium abundances and rotational behavior for bright giant stars|journal=Astronomy and Astrophysics|volume=450|issue=3|pages=1173|last1=Lèbre|first1=A.|last2=De Laverny|first2=P.|last3=Do Nascimento|first3=J. D.|last4=De Medeiros|first4=J. R.|year=2006|doi=10.1051/0004-6361:20053485|doi-access=free}}</ref>


<ref name=tokovinin>{{cite journal|bibcode=1997A&AS..124...75T|title=MSC - a catalogue of physical multiple stars|journal=Astronomy & Astrophysics Supplement Series|volume=124|pages=75–84|last1=Tokovinin|first1=A. A.|year=1997|doi=10.1051/aas:1997181|doi-access=free}}
<ref name=fracassini>{{cite journal|bibcode=1973Ap&SS..22..141F|title=Apparent diameters of 172 B5V-A5V stars of the Catalogue of Geneva Observatory|journal=Astrophysics and Space Science|volume=22|issue=1|pages=141–152|last1=Fracassini|first1=Massimo|last2=Gilardoni|first2=Giorgio|last3=Pasinetti|first3=Laura E.|year=1973|doi=10.1007/BF00642829|s2cid=120496963}}</ref>

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

<ref name=stars>{{cite web|url=http://stars.astro.illinois.edu/sow/albireo.html|title=Albireo|author=Jim Kaler|access-date=2018-01-07}}</ref>

<ref name="ginestet">{{Cite journal | last1 = Ginestet | first1 = N. | last2 = Carquillat | first2 = J. M. | doi = 10.1086/342942 | title = Spectral Classification of the Hot Components of a Large Sample of Stars with Composite Spectra, and Implication for the Absolute Magnitudes of the Cool Supergiant Components | journal = The Astrophysical Journal Supplement Series | volume = 143 | issue = 2 | pages = 513 | year = 2002 |bibcode = 2002ApJS..143..513G | doi-access = free }}</ref>

<ref name=drimmel2021>{{cite journal |bibcode=2021MNRAS.502..328D |title=A celestial matryoshka: Dynamical and spectroscopic analysis of the Albireo system |last1=Drimmel |first1=Ronald |last2=Sozzetti |first2=Alessandro |last3=Schröder |first3=Klaus-Peter |last4=Bastian |first4=Ulrich |last5=Pinamonti |first5=Matteo |last6=Jack |first6=Dennis |last7=Hernández Huerta |first7=Missael A. |journal=Monthly Notices of the Royal Astronomical Society |year=2021 |volume=502 |issue=1 |page=328 |doi=10.1093/mnras/staa4038 |arxiv=2012.01277 }}</ref>

<ref name=darling>[http://www.daviddarling.info/encyclopedia/N/Northern_Cross.html Northern Cross] {{Webarchive|url=https://web.archive.org/web/20080708231645/http://www.daviddarling.info/encyclopedia/N/Northern_Cross.html |date=2008-07-08 }}, entry, ''The Internet Encyclopedia of Science'', David Darling. Accessed on line July 24, 2008.</ref>

<ref name=Kunitzsch>{{cite book
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<ref name="IAU-CSN">{{cite web | url=http://www.pas.rochester.edu/~emamajek/WGSN/IAU-CSN.txt | title=IAU Catalog of Star Names |access-date=28 July 2016}}</ref>

<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>

<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>

<ref name=knobel1895>{{cite journal
| last=Knobel | first=E. B.
| title=Al Achsasi Al Mouakket, on a catalogue of stars in the Calendarium of Mohammad Al Achsasi Al Mouakket
| journal=[[Monthly Notices of the Royal Astronomical Society]]
| volume=55 | issue=8
| page=429 |date=June 1895
| bibcode=1895MNRAS..55..429K | doi=10.1093/mnras/55.8.429| doi-access=free}}</ref>

<ref name="SkyTel1">{{cite news
|url=http://www.skyandtelescope.com/observing/will-the-real-albireo-please-stand-up/
|title=Will the Real Albireo Please Stand Up?
|author=Bob King
|date=September 21, 2016
|work=Sky and Telescope
|access-date=October 14, 2016}}
</ref>
</ref>


<ref name=fracassini>{{cite journal|bibcode=1973Ap&SS..22..141F|title=Apparent diameters of 172 B5V-A5V stars of the Catalogue of Geneva Observatory|journal=Astrophysics and Space Science|volume=22|issue=1|pages=141–152|last1=Fracassini|first1=Massimo|last2=Gilardoni|first2=Giorgio|last3=Pasinetti|first3=Laura E.|year=1973|doi=10.1007/BF00642829}}</ref>
<ref name=dr2distances>{{Cite journal|arxiv=1804.10121|last1=Bailer-Jones|first1=C. A. L|title=Estimating distances from parallaxes IV: Distances to 1.33 billion stars in Gaia Data Release 2|journal=The Astronomical Journal|volume=156|issue=2|pages=58|last2=Rybizki|first2=J|last3=Fouesneau|first3=M|last4=Mantelet|first4=G|last5=Andrae|first5=R|doi=10.3847/1538-3881/aacb21|year=2018|bibcode=2018AJ....156...58B|s2cid=119289017 |doi-access=free }}</ref>

<ref name=maury1897>{{cite journal|bibcode=1897AnHar..28....1M|title=Spectra of bright stars photographed with the 11-inch Draper Telescope as part of the Henry Draper Memorial|journal=Annals of Harvard College Observatory|volume=28|pages=1|last1=Maury|first1=Antonia C.|last2=Pickering|first2=Edward C.|year=1897}}</ref>

<ref name=campbell1919>{{cite journal|bibcode=1919PASP...31...38C|title=The Variable Velocity of β Cygni|journal=Publications of the Astronomical Society of the Pacific|volume=31|issue=179|pages=38|last1=Campbell|first1=W. W.|year=1919|doi=10.1086/122807|doi-access=free}}</ref>

<ref name=freestarcharts>{{cite web|url=http://freestarcharts.com/index.php/17-guides/stars/171-albireo-beta-cygni-abeta-cyg-double-star?tmpl=component|title=freestarcharts.com|access-date=2017-06-11}}</ref>

<ref name=hd>{{cite journal|bibcode=1923AnHar..98....1C|title=The Henry Draper catalogue : 19h and 20h|journal=Annals of the Astronomical Observatory of Harvard College |volume=98|pages=1|last1=Cannon|first1=Annie Jump|last2=Pickering|first2=Edward Charles|year=1923}}. See note re HD&nbsp;183912,3,4 on this page.</ref>

<ref name=bonneau>{{cite journal|bibcode=1980A&A....86..295B|title=Speckle interferometric observations of binary systems with the Haute-Provence 1.93 M telescope|journal=Astronomy and Astrophysics|volume=86|pages=295|last1=Bonneau|first1=D.|last2=Foy|first2=R.|year=1980}}</ref>

<ref name=pisco>{{cite journal|bibcode=2008AN....329...54S|doi=10.1002/asna.200710834|title=Speckle observations with PISCO in Merate: IV. Astrometric measurements of visual binaries in 2005|journal=Astronomische Nachrichten|volume=329|issue=1|pages=54–68|year=2008|last1=Scardia|first1=M.|last2=Prieur|first2=J.-L.|last3=Pansecchi|first3=L.|last4=Argyle|first4=R.W.|last5=Sala|first5=M.|last6=Basso|first6=S.|last7=Ghigo|first7=M.|last8=Koechlin|first8=L.|last9=Aristidi|first9=E.|s2cid=263306085 |url=https://hal.archives-ouvertes.fr/hal-02113024/file/scard07a_MerIV.pdf}}</ref>

<ref name=mcalister1982>{{cite journal|bibcode=1982ApJS...48..273M|doi=10.1086/190778|title=Speckle interferometric measurements of binary stars. VI|journal=The Astrophysical Journal Supplement Series|volume=48|pages=273|year=1982|last1=McAlister|first1=H. A.|last2=Hendry|first2=E. M.|doi-access=free}}</ref>

<ref name=ccdm>{{cite journal|bibcode=1994CoORB.115....1D|title=Catalogue des composantes d'etoiles doubles et multiples (CCDM) premiere edition - Catalogue of the components of double and multiple stars (CCDM) first edition|journal=Com. De l'Observ. Royal de Belgique|volume=115|pages=1|last1=Dommanget|first1=J.|last2=Nys|first2=O.|year=1994}}</ref>

<!--<ref name=diameter>{{cite journal|doi=10.1086/378596|title=Angular Diameters of Stars from the Mark III Optical Interferometer|journal=The Astronomical Journal|volume=126|issue=5|pages=2502|year=2003|last1=Mozurkewich|first1=D.|last2=Armstrong|first2=J. T.|last3=Hindsley|first3=R. B.|last4=Quirrenbach|first4=A.|last5=Hummel|first5=C. A.|last6=Hutter|first6=D. J.|last7=Johnston|first7=K. J.|last8=Hajian|first8=A. R.|last9=Elias Ii|first9=Nicholas M.|last10=Buscher|first10=D. F.|last11=Simon|first11=R. S.|bibcode = 2003AJ....126.2502M |s2cid=67789347 }}</ref>-->


<ref name=hipparcos>{{cite journal|bibcode=2007A&A...474..653V|title=Validation of the new Hipparcos reduction|journal=Astronomy and Astrophysics|volume=474|issue=2|pages=653–664|last1=Van Leeuwen|first1=F|year=2007|doi=10.1051/0004-6361:20078357|arxiv=0708.1752}}</ref>
<ref name=physparms>Table 1, {{cite journal | doi = 10.1086/381063 | bibcode = 2004AJ....127.1176L | volume=127 | title=Physical Parameters of Southern B- and Be-Type Stars | year=2004 | journal=The Astronomical Journal | pages=1176–1180 | last1 = Levenhagen | first1 = R. S.| issue = 2 | s2cid = 121487369 }}</ref>


<ref name=roberts>{{cite journal|bibcode=2007AJ....133..545R|title=Adaptive Optics Photometry and Astrometry of Binary Stars. II. A Multiplicity Survey of B Stars|journal=The Astronomical Journal|volume=133|issue=2|pages=545|last1=Roberts|first1=Lewis C.|last2=Turner|first2=Nils H.|last3=Ten Brummelaar|first3=Theo A.|year=2007|doi=10.1086/510335|s2cid=10416471 |url=http://joy.chara.gsu.edu/~nils/2007AJ....133..545R.pdf}}</ref>
<ref name=stars>{{cite web|url=http://stars.astro.illinois.edu/sow/albireo.html|title=Albireo|author=Jim Kaler|accessdate=2018-01-07}}</ref>


}}
}}
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==External links==
==External links==
{{Commons}}
*{{APOD |date=30 August 2005 |title=Albireo: A Bright and Beautiful Double}}
* {{APOD |date=30 August 2005 |title=Albireo: A Bright and Beautiful Double}}
*[http://www.photomeeting.de/astromeeting/double/050728betCYGa1024.htm A picture of Albireo by Stefan Seip]
* [http://www.photomeeting.de/astromeeting/double/050728betCYGa1024.htm A picture of Albireo by Stefan Seip] {{Webarchive|url=https://web.archive.org/web/20070927185356/http://www.photomeeting.de/astromeeting/double/050728betCYGa1024.htm |date=2007-09-27 }}
*[http://fuzzyblobsmk.blogspot.co.uk/2011/08/famous-summer-double.html Albireo] at Pete Roberts' Fuzzy Blobs site
*[http://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Cygnus*.html About Cygnus], including more information about the origin of the name Albireo.
* [http://fuzzyblobsmk.blogspot.co.uk/2011/08/famous-summer-double.html Albireo] at Pete Roberts' Fuzzy Blobs site
* [https://penelope.uchicago.edu/Thayer/E/Gazetteer/Topics/astronomy/_Texts/secondary/ALLSTA/Cygnus*.html About Cygnus], including more information about the origin of the name Albireo.

{{commons|Albireo|Albireo}}


{{Stars of Cygnus}}
{{Stars of Cygnus}}
{{Portal bar|Astronomy|Stars|Spaceflight|Outer space|Solar System}}


[[Category:B-type main-sequence stars]]
[[Category:Bayer objects|Cygni, Beta]]
[[Category:Bayer objects|Cygni, Beta]]
[[Category:Be stars]]
[[Category:Flamsteed objects|Cygni, 06]]
[[Category:Flamsteed objects|Cygni, 06]]
[[Category:Be stars]]
[[Category:Triple stars]]
[[Category:Binary stars]]
[[Category:Binary stars]]
[[Category:B-type main-sequence stars]]
[[Category:Cygnus (constellation)]]
[[Category:Cygnus (constellation)]]
[[Category:K-type bright giants]]
[[Category:Durchmusterung objects|BD+27 3410]]
[[Category:Stars with proper names]]
[[Category:Henry Draper Catalogue objects|183912]]
[[Category:Henry Draper Catalogue objects|183912]]
[[Category:Hipparcos objects|095947]]
[[Category:Hipparcos objects|095947]]
[[Category:HR objects|7417]]
[[Category:Bright Star Catalogue objects|7417]]
[[Category:Durchmusterung objects|BD+27 3410]]
[[Category:K-type bright giants]]
[[Category:Stars with proper names|Albireo]]
[[Category:Triple stars]]

Revision as of 22:17, 3 June 2024

Albireo
Location of Albireo (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Cygnus
Albireo Aa
Right ascension 19h 30m 43.286s[1]
Declination +27° 57′ 34.84″[1]
Apparent magnitude (V) 3.21[2]
Albireo Ac
Right ascension 19h 30m 43.295s[3]
Declination +27° 57′ 34.62″[3]
Apparent magnitude (V) 5.85[2]
Albireo B
Right ascension 19h 30m 45.3962s[4]
Declination +27° 57′ 54.989″[4]
Apparent magnitude (V) 5.11[5]
Characteristics
Albireo Aa
Evolutionary stage Bright giant
Spectral type K2II[6]
B−V color index +1.13[5]
V−R color index +0.92[7]
Albireo Ac
Spectral type B8:p[6]
B−V color index +0.09[3]
V−R color index +0.09[7]
Albireo B
Spectral type B8Ve[8]
U−B color index -0.32[5]
B−V color index -0.10[5]
Astrometry
Albireo A
Radial velocity (Rv)−23.54[2] km/s
Proper motion (μ) RA: 4.915 mas/yr[9]
Dec.: −11.127 mas/yr[9]
Parallax (π)8.9816 ± 0.4474 mas[9]
Distance364.8+15.6
−15.3 ly
(111.9+4.8
−4.7 pc)[10]
Albireo Aa
Absolute magnitude (MV)−2.45[6]
Albireo Ac
Absolute magnitude (MV)−0.25[6]
Albireo B
Radial velocity (Rv)−18.80[11] km/s
Proper motion (μ) RA: −1.078[12] mas/yr
Dec.: −1.540[12] mas/yr
Parallax (π)8.1896 ± 0.0781 mas[12]
Distance395.4+2.9
−3.3 ly
(121.3+0.9
−1 pc)[10]
Position (relative to Albireo A)
ComponentAlbireo B
Epoch of observation2006
Angular distance35.3″ [13]
Position angle54° [13]
Orbit[2]
PrimaryAa
CompanionAc
Period (P)121.65+3.34
−2.90 yr
Semi-major axis (a)0.401+0.007
−0.006″
Eccentricity (e)0.20+0.01
−0.02
Inclination (i)156.15+2.90
−2.63°
Longitude of the node (Ω)84.43+5.27
−4.50°
Periastron epoch (T)B2026.36
Argument of periastron (ω)
(secondary)		54.72+1.88
−2.24°
Semi-amplitude (K1)
(primary)		2.91+0.09
−0.12 km/s
Details
Albireo Aa
Mass5.2[2] M☉
Radius58.69+2.83
−3.12[14] R☉
Luminosity (bolometric)1,259[2] L☉
Surface gravity (log g)0.93[2] cgs
Temperature4,383[2] K
Metallicity [Fe/H]−0.1[15] dex
Rotational velocity (v sin i)8.34[2] km/s
Albireo Ac
Mass2.7[2] M☉
Radius3.0[a] R☉
Luminosity (bolometric)79[2] L☉
Temperature10,000[2] K
Albireo B
Mass3.7 ± 0.8[16] M☉
Radius2.59[17] R☉
Luminosity (bolometric)230 ± 90[16] L☉
Surface gravity (log g)4.00 ± 0.15[16] cgs
Temperature13,200 ± 600[16] K
Age100[16] Myr
Other designations
β Cygni, 6 Cygni, ADS 12540, CCDM J19307+2758, WDS 19307+2758[18][19][20]
Albireo A: β¹ Cygni, BD+27 3410, HR 7417, HD 183912/183913, HIP 95947, SAO 87301, FK5 732, MCA 55 Aac, NSV 12105
Albireo B: β² Cygni, STF 4043B, BD+27 3411, HD 183914, HIP 95951, HR 7418, SAO 87302[21]
Database references
SIMBADβ Cyg (STF 4043)
Albireo A
Albireo Aa
Albireo Ab
Albireo B

Albireo /ælˈbɪrioʊ/[22] is a double star designated Beta Cygni (β Cygni, abbreviated Beta Cyg, β Cyg). The International Astronomical Union uses the name "Albireo" specifically for the brightest star in the system.[23] Although designated 'beta', it is fainter than Gamma Cygni, Delta Cygni, and Epsilon Cygni and is the fifth-brightest point of light in the constellation of Cygnus. Appearing to the naked eye to be a single star of magnitude 3, viewing through even a low-magnification telescope resolves it into its two components. The brighter yellow star, itself a very close binary system, makes a striking colour contrast with its fainter blue companion.[24]

Nomenclature

Albireo is the star in the head of the constellation of Cygnus (bottom).

β Cygni (Latinised to Beta Cygni) is the system's Bayer designation. The brighter of the two components is designated β¹ Cygni or Beta Cygni A and the fainter β² Cygni or Beta Cygni B.

The origin of the star system's traditional name Albireo is unclear. Christian Ludwig Ideler traced it to the heading for the constellation we call Cygnus in Ptolemy's star catalog, in the translation of the Almagest by Gerard of Cremona: "Stellatio Eurisim: et est volans; et jam vocatur gallina. et dicitur eurisim quasi redolens ut lilium ab ireo" ("Constellation Eurisim: and it is the Flyer, and it is also called the Hen, and it is called Eurisim as if redolent like the lily from the 'ireo'"). (The original Greek just calls the constellation "Ορνιθος αστερισμος", "the constellation of the Bird".) The word "ireo" is obscure as well – Ideler suggests that Gerard took "Eurisim" to mean the plant Erysimum, which is called irio in Latin, but the ablative case of that is not "ireo" but irione.[25] In any case, Ideler proposed that (somehow) the phrase "ab ireo" was applied to the star at the head of the bird, and this became "Albireo" when an "l" was mistakenly inserted as though it was an Arabic name.[26] Ideler also supposed that the name Eurisim was a mistaken transliteration of the Arabic name "Urnis" for Cygnus (from the Greek "Ορνις").

In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[27] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[28] included a table of the first two batches of names approved by the WGSN; which included Albireo for β¹ Cygni. It is now so entered in the IAU Catalog of Star Names.[23]

Medieval Arabic-speaking astronomers called Beta Cygni minqār al-dajājah (English: the hen's beak).[29] The term minqār al-dajājah (منقار الدجاجة) or Menchir al Dedjadjet appeared in the catalogue of stars in the Calendarium of Al Achsasi Al Mouakket, which was translated into Latin as Rostrum Gallinae, meaning the hen's beak.[30]

Since Cygnus is the swan, and Beta Cygni is located at the head of the swan, it is sometimes called the "beak star".[31] With Deneb, Gamma Cygni (Sadr), Delta Cygni, and Epsilon Cygni (Gienah), it forms the asterism called the Northern Cross.[32]

Properties

Albireo A and B

Beta Cygni is about 420 light-years (129 pc) away from the Sun.[2] When viewed with the naked eye, Albireo appears to be a single star. However, in a telescope it resolves into a double star consisting of β Cygni A (amber, apparent magnitude 3.1), and β Cygni B (blue-green, apparent magnitude 5.1).[33] Separated by 35 seconds of arc,[13] the two components provide one of the best contrasting double stars in the sky due to their different colors.

It is not known whether the two components β Cygni A and B are orbiting around each other in a physical binary system, or if they are merely an optical double.[2] If they are a physical binary, their orbital period is probably at least 100,000 years.[33] Some experts, however, support the optical double argument, based on observations that suggest different proper motions for the components, which implies that they are unrelated.[34] The primary and secondary also have different measured distances from the Hipparcos mission – 434 ± 20 light-years (133 ± 6 pc) for the primary and 401 ± 13 light-years (123 ± 4 pc) for the secondary.[35] More recently the Gaia mission has measured distances of about 330–390 light years (100–120 parsecs) for both components, but noise in the astrometric measurements for the stars means that data from Gaia's second data release is not yet sufficient to determine whether the stars are physically associated.[36]

In around 3.87 million years, Albireo will become the brightest star in the night sky.[37] It will peak in brightness with an apparent magnitude of –0.53 in 4.61 million years.[37]

There are a further 10 faint companions listed in the Washington Double Star catalogue, all fainter than magnitude 10. Only one is closer to the primary than Albireo B, with the others up to 142" away.[19]

Albireo A

The spectrum of Beta Cygni A was found to be composite when it was observed as part of the Henry Draper Memorial project in the late 19th century, leading to the supposition that it was itself double.[38] This was supported by observations from 1898 to 1918 which showed that it had a varying radial velocity.[39] In 1923, the two components were identified in the Henry Draper Catalogue as HD 183912 and HD 183913.[40][41]

In 1978, speckle interferometry observations using the 1.93m telescope at the Haute-Provence Observatory resolved a companion at 0.125". This observation was published in 1980,[42] and the companion is referred to as component Ab in the Washington Double Star Catalog.[19]

In 1976 speckle interferometry was used to resolve a companion using the 2.1-meter telescope at the Kitt Peak National Observatory. It was measured at a separation of 0.44", and it is noted that the observation was inconsistent with the Haute-Provence observations and hence not of the same star.[20][43] Although these observations pre-dated those at Haute-Provence, they were not published until 1982 and this component is designated Ac in the Washington Double Star Catalog.[19] It is designated as component C in the Catalog of Components of Double and Multiple Stars,[44] not to be confused with component C in the Washington Double Star Catalog which is a faint optical companion.[19] An orbit for the pair has since been computed using interferometric measurements, but as only approximately a quarter of the orbit has been observed, the orbital parameters must be regarded as preliminary. The period of this orbit is 214 years.[20] The confirmed close pair are referred to as Aa and Ac in modern papers, with Ab being the unconfirmed third component.[2]

The diameter of the primary K-type giant star has been measured using interferometry from the Navy Precision Optical Interferometer. A limb-darkened angular diameter of 4.904 mas was measured. At the parallax-derived distance of 111.4 pc, a radius equivalent to 58.69 R☉ is calculated.[14]

Albireo B

β Cygni B is a fast-rotating Be star, with an equatorial rotational velocity of at least 250 kilometers per second.[24] Its surface temperature has been spectroscopically estimated to be about 13,200 K.[16]

β Cygni B has been reported to be a very close double,[45] but the observations appear to have been incorrect.[19]

Moving group

Analysis of Gaia Data Release 2 astrometry suggests that four fainter stars may form a moving group along with the brighter visible components.[2]

Namesakes

Albireo (AK-90) was a United States Navy Crater-class cargo ship named after the star.

Notes

  1. ^ Applying the Stefan-Boltzmann Law with a nominal solar effective temperature of 5,772 K:

References

  1. ^ a b Høg, E; Fabricius, C; Makarov, V. V; Urban, S; Corbin, T; Wycoff, G; Bastian, U; Schwekendiek, P; Wicenec, A (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27. Bibcode:2000A&A...355L..27H.
  2. ^ a b c d e f g h i j k l m n o p Drimmel, Ronald; Sozzetti, Alessandro; Schröder, Klaus-Peter; Bastian, Ulrich; Pinamonti, Matteo; Jack, Dennis; Hernández Huerta, Missael A. (2021). "A celestial matryoshka: Dynamical and spectroscopic analysis of the Albireo system". Monthly Notices of the Royal Astronomical Society. 502 (1): 328. arXiv:2012.01277. Bibcode:2021MNRAS.502..328D. doi:10.1093/mnras/staa4038.
  3. ^ a b c Fabricius, C; Høg, E; Makarov, V. V; Mason, B. D; Wycoff, G. L; Urban, S. E (2002). "The Tycho double star catalogue". Astronomy and Astrophysics. 384: 180–189. Bibcode:2002A&A...384..180F. doi:10.1051/0004-6361:20011822.
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    Beta1 Cygni = Gaia DR3 2026116260337482112
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Further reading

  • Webb, T. W.; McAlister, H. A.; Worley, C. E.; Burnham, S. W.; Aitken, R. G. (1980). "Albireo as a Triple Star". Sky and Telescope. 59: 210. Bibcode:1980S&T....59..210W.
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