View source for Mintaka

{{short description|Five-star system in the constellation Orion}}
{{other uses}}
{{Starbox begin
 | name=Mintaka
}}
{{Starbox image
 | image=[[File:Orion Belt 2009-01-29.jpg|300px]]
 |caption=Orion's Belt (composed of the three brightest stars shown), Mintaka being the rightmost, on the west side
}}
{{Starbox observe 3s
 | constell=[[Orion (constellation)|Orion]]
 | epoch=J2000
 | component1=δ Ori A (Aa1 + Aa2 + Ab)
 | ra1={{RA|05|32|00.40009}}<ref name="van Leeuwen2007"/>
 | dec1={{DEC|−00|17|56.7424}}<ref name="van Leeuwen2007"/>
 | appmag_v1=2.23<ref name=hr>{{cite book|bibcode=1991bsc..book.....H|title=The Bright star catalogue|location=New Haven, Conn. |publisher=Yale University Observatory |edition=5th Revised |year=1991|last1=Hoffleit|first1=Dorrit|last2=Jaschek|first2=Carlos}}</ref> {{nowrap|(2.50 + 3.90<ref name=tokovinin1997/>)}}
 | component2=δ Ori B
 | ra2={{RA|05|31|58.745}}<ref name=ucac4>{{cite journal|bibcode=2012yCat.1322....0Z|title=VizieR Online Data Catalog: UCAC4 Catalogue (Zacharias+, 2012)|journal=VizieR On-line Data Catalog: I/322A |last1=Zacharias|first1=N.|last2=Finch|first2=C. T.|last3=Girard|first3=T. M.|last4=Henden|first4=A.|last5=Bartlett|first5=J. L.|author5-link=Jennifer Bartlett (astronomer)|last6=Monet|first6=D. G.|last7=Zacharias|first7=M. I.|year=2012}}</ref>
 | dec2={{DEC|−00|18|18.65}}<ref name=ucac4/>
 | appmag_v2=14.0<ref name=harvin2002/>
 | component3=HD 36485
 | ra3={{RA|05|32|00.406}}<ref name=tycho2>{{cite journal|bibcode=2000A&A...355L..27H|title=The Tycho-2 catalogue of the 2.5 million brightest stars|journal=Astronomy and Astrophysics|volume=355|pages=L27|last1=Høg|first1=E.|last2=Fabricius|first2=C.|last3=Makarov|first3=V. V.|last4=Urban|first4=S.|last5=Corbin|first5=T.|last6=Wycoff|first6=G.|last7=Bastian|first7=U.|last8=Schwekendiek|first8=P.|last9=Wicenec|first9=A.|year=2000|doi=10.1888/0333750888/2862}}</ref>
 | dec3={{DEC|−00|17|04.38}}<ref name=tycho2/>
 | appmag_v3=6.85<ref name=harvin2002/>
}}
{{Starbox character
 | component1 = A
 | class = O9.5II + B1V +B0IV<ref name=shenar2015>{{cite journal|bibcode=2015ApJ...809..135S|title=A Coordinated X-Ray and Optical Campaign of the Nearest Massive Eclipsing Binary, δ Orionis Aa. IV. A Multiwavelength, Non-LTE Spectroscopic Analysis|journal=Astrophysical Journal|volume=809|issue=2|pages=135|last1=Shenar|first1=T.|last2=Oskinova|first2=L.|last3=Hamann|first3=W.-R.|last4=Corcoran|first4=M. F.|last5=Moffat|first5=A. F. J.|last6=Pablo|first6=H.|last7=Richardson|first7=N. D.|last8=Waldron|first8=W. L.|last9=Huenemoerder|first9=D. P.|last10=Maíz Apellániz|first10=J.|last11=Nichols|first11=J. S.|last12=Todt|first12=H.|last13=Nazé|first13=Y.|last14=Hoffman|first14=J. L.|last15=Pollock|first15=A. M. T.|last16=Negueruela|first16=I.|year=2015|doi=10.1088/0004-637X/809/2/135|arxiv = 1503.03476 |hdl=10045/59172|s2cid=14909574}}</ref>
 | b-v = −0.22<ref name=hr/>
 | u-b = −1.05<ref name=hr/>
 | variable = [[Eclipsing binary]]<ref name=gcvs/>
 | component2 = HD 36485
 | class2 = B3V + A0V<ref name=oplistilova2023/>
 | b-v2 = −0.16<ref name=renson2009>{{cite journal | last1=Renson | first1=P. | last2=Manfroid | first2=J. | title=Catalogue of Ap, HgMn and Am stars | journal=Astronomy and Astrophysics | volume=498 | issue=3 | pages=961–966 | date=May 2009 | doi=10.1051/0004-6361/200810788 | bibcode=2009A&A...498..961R | url=https://zenodo.org/record/890529 | doi-access=free }}</ref>
 | u-b2 = −0.71<ref name=renson2009/>
 | variable2 =
}}
{{Starbox astrometry
| radial_v = {{val|18.50|0.5}}<ref name="PourbaixTokovinin2004">{{cite journal|bibcode=2004A&A...424..727P|title=SB9: The ninth catalogue of spectroscopic binary orbits|journal=Astronomy and Astrophysics|volume=424|issue=2|pages=727–732|last1=Pourbaix|first1=D.|last2=Tokovinin|first2=A. A.|last3=Batten|first3=A. H.|last4=Fekel|first4=F. C.|last5=Hartkopf|first5=W. I.|last6=Levato|first6=H.|last7=Morrell|first7=N. I.|last8=Torres|first8=G.|last9=Udry|first9=S.|year=2004|doi=10.1051/0004-6361:20041213|arxiv = astro-ph/0406573 |s2cid=119387088}}</ref>
| prop_mo_ra = {{val|0.64|0.56}}<ref name="van Leeuwen2007"/>
| prop_mo_dec = {{val|-0.69|0.27}}<ref name="van Leeuwen2007"/>
| parallax = 4.71
| p_error = 0.58
| parallax_footnote = <ref name="van Leeuwen2007"/>
| dist_pc = 380<ref name=shenar2015/>
| dist_ly = 1,200<ref name=shenar2015/>
| absmag_v = −5.8<ref name=harvin2002>{{cite journal|bibcode=2002ApJ...565.1216H|title=Tomographic Separation of Composite Spectra. VIII. The Physical Properties of the Massive Compact Binary in the Triple Star System HD 36486 (δ Orionis A)|journal=Astrophysical Journal|volume=565|issue=2|pages=1216|last1=Harvin|first1=James A.|last2=Gies|first2=Douglas R.|last3=Bagnuolo|first3=William G.|last4=Penny|first4=Laura R.|last5=Thaller|first5=Michelle L.|year=2002|doi=10.1086/324705|arxiv = astro-ph/0110683 |s2cid=118957476}}</ref>
}}
{{Starbox astrometry|no_heading=y
| component1 = δ Ori Aa1
| absmag_v = −5.4<ref name=harvin2002/>
}}
{{Starbox astrometry|no_heading=y
| component1 = δ Ori Aa2
| absmag_v = −2.9<ref name=harvin2002/>
}}
{{Starbox astrometry|no_heading=y
| component1 = δ Ori Ab
| absmag_v = −4.2<ref name=harvin2002/>
}}
{{Starbox astrometry|no_heading=y
| component1 = HD 36485
| prop_mo_ra = +1.523<ref name=dr3c/>
| prop_mo_dec = −1.653<ref name=dr3c/>
| parallax = 2.6245
| p_error = 0.0538
| parallax_footnote = <ref name=dr3c>{{cite Gaia DR3|3220757015623151616}}</ref>
|
}}
{{Starbox orbit
| reference = <ref name="CorcoranNichols2015"/>
| primary = δ Ori Aa1
| name = δ Ori Aa2
| period =
| period_unitless = 5.732436 days
| axis =
| axis_unitless = {{solar radius|{{val|43.1|1.7}}}}
| eccentricity = {{val|0.1133|0.0003}}
| inclination = {{val|76.5|0.2}}
| node =
| periastron = {{val|2,456,295.674|0.062|fmt=commas}}
| periarg = {{val|141.3|0.2}}
| periarg_primary = <!--Argument of periastron (in degrees), primary -->
| k1 = <!-- Velocity semi-amplitude (SB1, or primary in SB2), in km/s -->
| k2 = <!-- Velocity semi-amplitude (secondary in SB2), in km/s -->
}}
{{Starbox orbit
| reference = <ref name=oplistilova2023/>
| primary = δ Ori Aa1/2
| name = δ Ori Ab
| period =
| period_unitless = 53,839 days
| axis =
| axis_unitless = {{solar radius|20,038}}
| eccentricity = {{val|0.5886|0.016}}
| inclination = {{val|104.7|0.4}}
| node = {{val|122.4|0.5}}
| periastron = {{val|2,458,773.2|0.1|fmt=commas}}
| periarg = {{val|259|2}}
| periarg_primary = <!--Argument of periastron (in degrees), primary -->
| k1 = <!-- Velocity semi-amplitude (SB1, or primary in SB2), in km/s -->
| k2 = <!-- Velocity semi-amplitude (secondary in SB2), in km/s -->
}}
{{Starbox detail
 | component1=δ Ori Aa1
 | age_myr=
 | metal_fe=
 | mass=17.8<ref name=oplistilova2023/>
 | radius=13.1<ref name=oplistilova2023/>
 | rotational_velocity={{val|114|20}}<ref name=oplistilova2023/>
 | luminosity=190,000<ref name=shenar2015/>
 | temperature={{val|31400|1000|fmt=commas}}<ref name=oplistilova2023/>
 | gravity={{val|3.55|0.05}}<ref name=oplistilova2023/>
 | component2=δ Ori Aa2
 | age_myr2=
 | metal_fe2=
 | mass2=8.518<ref name=oplistilova2023/>
 | radius2=4.168<ref name=oplistilova2023/>
 | rotational_velocity2={{val|89|15}}<ref name=oplistilova2023/>
 | luminosity2=16,000<ref name=shenar2015/>
 | temperature2={{val|25,442|1500|fmt=commas}}<ref name=oplistilova2023/>
 | gravity2={{val|3.48|0.06}}<ref name=oplistilova2023/>
}}
{{Starbox detail|no_heading=y
 | component1=δ Ori Ab
 | age_myr=
 | metal_fe=
 | mass=8.787<ref name=oplistilova2023/>
 | radius=12.045<ref name=oplistilova2023/>
 | rotational_velocity={{val|216|25}}<ref name=oplistilova2023/>
 | luminosity=63,000<ref name=shenar2015/>
 | temperature={{val|30250|1000|fmt=commas}}<ref name=oplistilova2023/>
 | gravity={{val|3.64|0.05}}<ref name=oplistilova2023/>
}}
{{Starbox detail|no_heading=y
 | component1 = δ Ori B
 | mass =
 | temperature = 5,324<ref name=dr2b>{{cite DR2|3220756809465268352}}</ref>
 | radius = 0.77<ref name=dr2b/>
 | luminosity = 0.431<ref name=dr2b/>
 | component2=HD 36485
 | mass2=6-11<ref name=leone2010/>
 | luminosity2=3,300<ref name=zboril>{{cite journal|bibcode=1997A&A...324..949Z|title=Properties of He-rich stars. I. Their evolutionary state and helium abundance|journal=Astronomy and Astrophysics|volume=324|pages=949|last1=Zboril|first1=M.|last2=North|first2=P.|last3=Glagolevskij|first3=Yu. V.|last4=Betrix|first4=F.|year=1997}}</ref>
 | temperature2=18,400<ref name=zboril/>
 | radius2=5.7<ref name=zboril/>
 | gravity2=4.41<ref name=zboril/>
}}
{{Starbox catalog
 | names=Mintaka, [[Bayer designation|δ]]&nbsp;Orionis, [[Flamsteed designation|34]]&nbsp;Orionis, 88&nbsp;G.&nbsp;Orionis, [[Catalogues of Fundamental Stars|FK5]]&nbsp;206, [[Hipparcos#Published catalogues|HIP]]&nbsp;25930, [[Aitken Double Star Catalogue|ADS]]&nbsp;4134, [[Catalogue of Components of Double and Multiple Stars|CCDM]]&nbsp;J05320-0018, [[Washington Double Star Catalog|WDS]]&nbsp;J05320-0018
 | component1=Mintaka Aa
 | names1=[[Henry Draper catalogue|HD]] 36486, [[Harvard Revised catalogue|HR]]&nbsp;1851, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]]&nbsp;132220/132221, [[Durchmusterung|BD]]−00°983, [[Boss General Catalogue|GC]]&nbsp;6847
 | component2=Mintaka Ab
 | names2=[[Catalogue of Components of Double and Multiple Stars|CCDM]]&nbsp;J05320-0018D, [[Washington Double Star Catalog|WDS]]&nbsp;J05320-0018Ab
 | component3=δ Ori B
 | names3=[[USNO CCD Astrograph Catalog|UCAC3]]&nbsp;180-24383, [[Catalogue of Components of Double and Multiple Stars|CCDM]]&nbsp;J05320-0018B, [[Washington Double Star Catalog|WDS]]&nbsp;J05320-0018B
 | component4=HD 36485
 | names4=[[Bayer designation|δ]]&nbsp;Orionis&nbsp;C, [[Harvard Revised catalogue|HR]]&nbsp;1851, [[Smithsonian Astrophysical Observatory Star Catalog|SAO]]&nbsp;132221, [[Durchmusterung|BD]]−00°982, [[Boss General Catalogue|GC]]&nbsp;6848, [[General Catalogue of Trigonometric Parallaxes|PLX]]&nbsp;1261, [[Catalogue of Components of Double and Multiple Stars|CCDM]]&nbsp;J05320-0018C
}}
{{Starbox reference
 | Simbad = delta+Orionis
 | Simbad3=UCAC3+180-24383 |sn3=δ Ori B
 | Simbad4=HD+36485 |sn4=HD 36485
}}
{{Starbox end}}

'''Mintaka''' {{IPAc-en|'|m|I|n|t|@|k|@}},<!--Kunitzsch has this as the "Arabic" pronunciation, perhaps an error. Davis (1944), which much of Kunitzsch appears to be based on, has the name initial stress.--><ref name=Rumrill>{{cite journal
|title=Star Name Pronunciation
|last=Rumrill |first=H. B.
|journal=Publications of the Astronomical Society of the Pacific
|volume=48
|pages=139 |number=283
|date=June 1936
|location = San Francisco, California
|bibcode=1936PASP...48..139R |doi=10.1086/124681 |s2cid=120743052 |doi-access=free
}}</ref> designation '''Delta Orionis''' ('''δ Orionis''', abbreviated '''Delta Ori''', '''δ Ori''') and '''34 Orionis''' ('''34 Ori'''), is a quintuple [[star system]] some 1,200 [[light-year]]s from the [[Sun]] in the [[constellation]] of [[Orion (constellation)|Orion]]. Together with [[Alnitak]] (Zeta Orionis) and [[Alnilam]] (Epsilon Orionis), the three stars form [[Orion's Belt]], known by many names among ancient cultures. The star is located very close to the [[celestial equator]]. When Orion is near the [[meridian (astronomy)|meridian]], Mintaka is the rightmost of the Belt's stars when viewed from the [[Northern Hemisphere]] facing [[south]].

The five stars form a hierarchy:<ref name=oplistilova2023/>
* Delta Ori A
** Delta Ori Aa, an eclipsing binary with an orbital period of 5.7 days
*** Delta Ori Aa1, a single star
*** Delta Ori Aa2, a single star
** Delta Ori Ab, which orbits Aa at a distance, with an orbital period of 152 years
* Delta Ori B, a single star not physically associated with the system
* Delta Ori C, a binary star with an orbital period of 30 days, also known as '''HD 36485'''
** Delta Ori Ca, a single star
** Delta Ori Cb, a single star

"Mintaka" may also be used as the base name, e.g. "Mintaka C" for δ Ori C.

== Nomenclature ==

''Delta Orionis'' is the star's [[Bayer designation]], ''34 Orionis'' its [[Flamsteed designation]]. The name ''Mintaka'' itself is derived from an [[Arabic]] term for 'belt': منطقة or ''manṭaqa''.<ref name=allen>{{cite book |title=Star-names and their meanings|author=Allen, Richard Hinckley|year=1963|orig-year=1899|publisher=[[Dover Publications]]|location=New York, NY |isbn=1-931559-44-9|page=314}}</ref> In 2016, the [[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 | archive-date=10 June 2016 | archive-url=https://web.archive.org/web/20160610172014/https://www.iau.org/science/scientific_bodies/working_groups/280/ | url-status=dead }}</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 ''Mintaka'' for this star. It is now so entered in the IAU Catalog of Star Names.<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>

== Observational history ==
{{Location mark
|image=Orion constellation map.svg|alt=|float=left|width=250|type=thumb
|label=|position=right
|mark=Red circle.svg|mark_width=12|mark_link=Mintaka|x=609|y=525
|caption=Location of δ Orionis (circled), as shown in a conventional star chart with north up
}}
Mintaka is the westernmost of the three stars of Orion's belt. It is easily visible to the naked eye, one of the [[brightest stars]] in the sky, and has been known since antiquity.

[[Radial velocity]] measurements taken by [[Henri-Alexandre Deslandres]] in 1900 at [[Paris Observatory]] showed that Mintaka had a variable radial velocity and therefore was a [[spectroscopic binary]].<ref name="Deslandres1900"/> His preliminary [[orbital period]] estimate of 1.92 days was shown to be incorrect in 1904 when [[Johannes Franz Hartmann]] using photographic plates taken at [[Leibniz Institute for Astrophysics Potsdam|Potsdam Observatory]] showed that the orbital period was 5.7 days.<ref name="Hartmann1904"/> Hartmann also noticed that the [[calcium K line]] at 393.4 nanometres in the [[stellar spectrum]] did not share in the periodic displacements of the lines due to orbital motion of the star and theorized that there was a cloud in the line of sight to Mintaka that contained [[calcium]]. This was the first detection of the [[interstellar medium]].<ref name="Hartmann1904"/>
{{clear left}}

==System==
{{stack begin|float=left}}
<div style="float:left; width:220px; border:solid black 1px; text-align: center; margin: 8px; padding: 4px; font-size: 90%;">
{{tree chart/start}}
{{tree chart|border=1|  |  |, |S1| |S1='''Aa1''' }}
{{tree chart|border=0|  |, |( |PA| |PA=Period&nbsp;=&nbsp;5.7&nbsp;d }}
{{tree chart|border=1|  |! |` |S2| |S2='''Aa2''' }}
{{tree chart|border=0|, |( |  |PB| |PB=Period&nbsp;=&nbsp;152&nbsp;yr }}
{{tree chart|border=1|! |` |- |S3| |S3='''Ab''' }}
{{tree chart|border=0|( |PC|  |  | |PC=52″&nbsp;separation }}
{{tree chart|border=1|! |, |- |S4| |S4='''Ca''' }}
{{tree chart|border=0|` |( |  |PD| |PD=Period&nbsp;=&nbsp;30&nbsp;d }}
{{tree chart|border=1|  |` |- |S5| |S5='''Cb''' }}
{{tree chart/end}}
Hierarchy of orbits in the system<ref name=oplistilova2023/>
</div>
[[File:DeltaOriLightCurve.png|thumb|left|A [[Photometric system#Photometric letters|green band]] [[light curve]] for Delta Orionis, plotted from data published by Koch and Hrivnak (1981)<ref name="Koch"/>]]
{{stack end}}
δ Orionis is a [[multiple star system]]. There is a [[apparent magnitude|magnitude]] 7 star about 52 [[arcseconds]] away from the second-magnitude primary and a much fainter star in between. The system is designated WDS&nbsp;05320-0018 in the [[Washington Double Star Catalog]], with the 14th-magnitude companion listed as component B and the seventh-magnitude star as component C.<ref name=wds>{{cite journal |bibcode=2001AJ....122.3466M |title=The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog |journal=The Astronomical Journal |volume=122 |issue=6 |pages=3466 |last1=Mason |first1=Brian D. |last2=Wycoff |first2=Gary L. |last3=Hartkopf |first3=William I. |last4=Douglass |first4=Geoffrey G. |last5=Worley |first5=Charles E. |year=2001 |doi=10.1086/323920 |doi-access=free }}</ref>

The primary component is itself a triple system: a [[stellar classification#Class O|class-O9.5]] bright giant and a [[stellar classification#Class B|class-B]] [[main-sequence star]] orbit every 5.73 days and exhibit shallow eclipses when the star dims about 0.2 of a magnitude,<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 |last1=Samus|first1=N. N.|last2=Durlevich|first2=O. V.|year=2009|display-authors=etal}}</ref> and a B-class [[subgiant]] is resolved 0.26" away.<ref name=tokovinin1997>{{cite journal|bibcode=1997A&AS..124...75T|title=MSC - a catalogue of physical multiple stars|journal=Astronomy and Astrophysics Supplement Series|volume=124|pages=75–84|last1=Tokovinin|first1=A. A.|year=1997|doi=10.1051/aas:1997181|doi-access=free}}</ref> At the primary eclipse, the apparent magnitude (of the whole system) drops from 2.23 to 2.35, while it only drops to 2.29 at the secondary eclipse.<ref name=zasche>{{cite journal|bibcode=2009AJ....138..664Z|title=A Catalog of Visual Double and Multiple Stars with Eclipsing Components|journal=Astronomical Journal|volume=138|issue=2|pages=664|last1=Zasche|first1=P.|last2=Wolf|first2=M.|last3=Hartkopf|first3=W. I.|last4=Svoboda|first4=P.|last5=Uhlař|first5=R.|last6=Liakos|first6=A.|last7=Gazeas|first7=K.|year=2009|doi=10.1088/0004-6256/138/2/664|arxiv = 0907.5172 |s2cid=17089387}}</ref>

The outer star of the triple system orbits the inner pair once every {{convert|53,839|days|years}}.  The orbit is quite eccentric, with the separation varying between {{convert|8244|solar radius|au|lk=on}} and {{convert|31832|solar radius|au}}.<ref name=oplistilova2023/>

The seventh-magnitude companion, HD 36485, is a [[chemically peculiar star|chemically peculiar]] [[B-type main-sequence star]] and itself a spectroscopic binary with a faint A-type companion in a 30-day orbit. It has an unusual spectrum with [[H-alpha]] [[Spectral line|emission]] and unusually strong helium [[absorption line]]s. It has a strong magnetic field and a very slow rotational velocity that produces chemical stratification in its atmosphere, which leads to the unusual abundances seen in the spectrum.<ref name=leone2010>{{cite journal|bibcode=2010MNRAS.401.2739L|title=The magnetic field and circumstellar environment of the helium-strong star HD36485 = δ Ori C|journal=Monthly Notices of the Royal Astronomical Society|volume=401|issue=4|pages=2739|last1=Leone|first1=F.|last2=Bohlender|first2=D. A.|last3=Bolton|first3=C. T.|last4=Buemi|first4=C.|last5=Catanzaro|first5=G.|last6=Hill|first6=G. M.|last7=Stift|first7=M. J.|year=2010|doi=10.1111/j.1365-2966.2009.15858.x|doi-access=free}}</ref>

The 14th-magnitude companion, δ Orionis B, is thought to be closer than the rest of the system and not physically associated with it.<ref name=dr3b/> It is likely to be a [[K-type main sequence star]].<ref name=oplistilova2023/>

Mintaka is surrounded by a cluster of faint stars, possibly part of the cluster surrounding [[σ Ori]].<ref name="CaballeroSolano2008">{{cite journal|bibcode=2008A&A...485..931C|title=Young stars and brown dwarfs surrounding Alnilam (ɛ Orionis) and Mintaka (δ Orionis)|journal=Astronomy and Astrophysics|volume=485|issue=3|pages=931|last1=Caballero|first1=J. A.|last2=Solano|first2=E.|year=2008|doi=10.1051/0004-6361:200809595|arxiv = 0804.2184 |s2cid=16175953}}</ref>

==Distance==
The distance derived from the ''[[Hipparcos]]'' satellite parallax is {{val|212|30|ul=parsecs}},<ref name="van Leeuwen2007"/> while spectroscopic distances, comparisons to similar stars, and cluster membership all suggest a value more than double that.<ref name="CorcoranNichols2015">{{cite journal|last1=Corcoran|first1=M. F.|last2=Nichols|first2=J. S.|last3=Pablo|first3=H.|last4=Shenar|first4=T.|last5=Pollock|first5=A. M. T.|last6=Waldron|first6=W. L.|last7=Moffat|first7=A. F. J.|last8=Richardson|first8=N. D.|last9=Russell|first9=C. M. P.|last10=Hamaguchi|first10=K.|last11=Huenemoerder|first11=D. P.|last12=Oskinova|first12=L.|last13=Hamann|first13=W.-R.|last14=Nazé|first14=Y.|last15=Ignace|first15=R.|last16=Evans|first16=N. R.|last17=Lomax|first17=J. R.|last18=Hoffman|first18=J. L.|last19=Gayley|first19=K.|last20=Owocki|first20=S. P.|last21=Leutenegger|first21=M.|last22=Gull|first22=T. R.|last23=Hole|first23=K. T.|last24=Lauer|first24=J.|last25=Iping|first25=R. C.|title=A Coordinated X-Ray and Optical Campaign of the Nearest Massive Eclipsing Binary, δ Orionis Aa. I. Overview of the X-Ray Spectrum|journal=Astrophysical Journal |volume=809 |issue=2 |year=2015 |pages=132 |doi=10.1088/0004-637X/809/2/132 |bibcode=2015ApJ...809..132C|arxiv = 1507.05101 |s2cid=17339779}}</ref> This type of unreconcilable discrepancy is not unique to Mintaka and the reasons for it have yet to be clarified.<ref name=shenar2015/> In [[Gaia Data Release 3]], component C is listed with a parallax of {{val|2.6245|0.0538|ul=mas}},<ref name=dr3c/> consistent with the distances derived by other methods but disagreeing with the ''Hipparcos''-derived value for the primary.<ref name="van Leeuwen2007"/>

The Gaia DR3 parallax for component B is {{val|3.5002|0.0119|u="}}, strongly suggesting it is considerably closer than the other members of the system and merely a chance alignment.<ref name=dr3b>{{cite Gaia DR3|3220756809465268352}}</ref>  At that distance it is likely to be a [[K-type main sequence star]].<ref name=oplistilova2023/>

==Etymology and cultural significance==
Mintaka was seen by astrologers as a portent of good fortune.<ref name=allen/>

===Orion's Belt===
{{Main|Orion's Belt}}
[[File:Dunhuang Star Atlas - Orion.jpg|thumb|left|[[Dunhuang Star Chart|Dunhuang Star Atlas]] – Orion]]
The three belt stars were collectively known by many names in many cultures. Arabic terms include ''Al Nijād'' 'the Belt', ''Al Nasak'' 'the Line', ''Al Alkāt'' 'the Golden Grains or Nuts', and, in modern Arabic, ''Al Mīzān al Ḥakk'' 'the Accurate Scale Beam'. In [[Chinese mythology]], they were also known as the Weighing Beam.{{citation needed|date=November 2020}}

In [[Chinese astronomy|Chinese]], {{lang|zh|參宿}} ({{lang|zh-Latn|Shēn Sù}}), meaning ''[[Three Stars (Chinese constellation)|Three Stars]] (asterism)'', refers to an asterism consisting of Mintaka, [[Alnilam]], and [[Alnitak]] (Orion's Belt), with [[Betelgeuse]], [[Bellatrix]], [[Saiph]] and [[Rigel]] later added.<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, the [[Chinese star names|Chinese name]] for Mintaka is {{lang|zh|參宿三}} ({{lang|zh-Latn|Shēn Sù sān}}, {{langx|en|the Third Star of Three Stars}}).<ref>{{in lang|zh}}  [http://aeea.nmns.edu.tw/2006/0605/ap060525.html AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 25 日] {{Webarchive|url=https://web.archive.org/web/20110716122642/http://aeea.nmns.edu.tw/2006/0605/ap060525.html |date=2011-07-16 }}</ref> It is one of the western mansions of the [[White Tiger (mythology)|White Tiger]].
{{clear left}}

==Namesakes==
The [[USS Mintaka (AK-94)|USS ''Mintaka'' (AK-94)]] was a [[United States Navy]] [[Crater-class cargo ship|''Crater''-class cargo ship]] named after the star.

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

<ref name="Koch">{{cite journal |last1=Koch |first1=R. H. |last2=Hrivnak |first2=B. J. |title=A photometric study of the close binary delta Orionis A |journal=Astrophysical Journal |date=August 1981 |volume=248 |pages=249–255 |doi=10.1086/159148 |url=https://articles.adsabs.harvard.edu/pdf/1981ApJ...248..249K |access-date=14 July 2022}}</ref>

<ref name="Deslandres1900">{{cite journal | title=Variable velocity in line of sight of delta Orionis. (Notes) | last1=Deslandres | first1=H. | journal=The Observatory | volume=23 | pages=148 | year=1900 | bibcode=1900Obs....23..148D }}</ref>

<ref name="Hartmann1904">{{cite journal | title=Investigations on the spectrum and orbit of delta Orionis | last1=Hartmann | first1=J. | journal=Astrophysical Journal | volume=19 | pages=268–286 | year=1904 | bibcode=1904ApJ....19..268H | doi=10.1086/141112 }}</ref>

<ref name="van Leeuwen2007">{{cite journal | title=Validation of the new Hipparcos reduction | last1=van Leeuwen | first1=F. | journal=Astronomy and Astrophysics | volume=474 | issue=2 | pages=653–664 | year=2007 | arxiv=0708.1752 | bibcode=2007A&A...474..653V | doi=10.1051/0004-6361:20078357 | s2cid=18759600 }} [http://webviz.u-strasbg.fr/viz-bin/VizieR-5?-out.add=.&-source=I/311/hip2&recno=25863 Vizier catalog entry ]</ref>

<ref name=oplistilova2023>{{cite journal |bibcode=2023A&A...672A..31O |title=Spectrum of the secondary component and new orbital elements of the massive triple star δ Ori A |last1=Oplištilová |first1=A. |last2=Mayer |first2=P. |last3=Harmanec |first3=P. |last4=Brož |first4=M. |last5=Pigulski |first5=A. |last6=Božić |first6=H. |last7=Zasche |first7=P. |last8=Šlechta |first8=M. |last9=Pablo |first9=H. |last10=Kołaczek-Szymański |first10=P. A. |last11=Moffat |first11=A. F. J. |last12=Lovekin |first12=C. C. |last13=Wade |first13=G. A. |last14=Zwintz |first14=K. |last15=Popowicz |first15=A. |last16=Weiss |first16=W. W. |journal=Astronomy and Astrophysics |date=2023 |volume=672 |pages=A31 |doi=10.1051/0004-6361/202245272 |arxiv=2301.10290 |s2cid=256226821 }}</ref>

}}

==External links==
* {{APOD |date=10 February 2009 |title=Image of Mintaka}}
* [http://www.constellationsofwords.com/stars/Mintaka.html Mintaka page constellationsofwords.com]
* [https://web.archive.org/web/20130102053617/http://www.astrostudio.org/xhip.php?hip=25930 Mintaka page at Astrostudio]
* [http://aladin.u-strasbg.fr/AladinLite/?target=*%20del%20Ori&fov=0.46&survey=P%2F2MASS%2Fcolor Mintaka with HD 36485 visible at 12 noon and star C at 4 o'clock]

{{Stars of Orion}}
{{Portal bar|Astronomy|Stars|Outer space}}
{{Sky|05|32|00.4|-|00|17|57|800}}

{{DEFAULTSORT:Mintaka}}
[[Category:Bayer objects|Orionis, Delta]]
[[Category:Spectroscopic binaries]]
[[Category:Eclipsing binaries]]
[[Category:O-type bright giants]]
[[Category:B-type main-sequence stars]]
[[Category:Orion (constellation)]]
[[Category:Flamsteed objects|Orionis, 34]]
[[Category:Bright Star Catalogue objects|1851]]
[[Category:Henry Draper Catalogue objects|036486]]
[[Category:Triple star systems]]
[[Category:Durchmusterung objects|BD-00 0983]]
[[Category:Hipparcos objects|025930]]
[[Category:Stars with proper names|Mintaka]]