Mintaka
 Orion's Belt (composed of the three brightest stars shown), Mintaka being the rightmost, on the west side | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Orion |
| δ Ori A (Aa1 + Aa2 + Ab) | |
| Right ascension | 05h 32m 00.40009s[1] |
| Declination | −00° 17′ 56.7424″[1] |
| Apparent magnitude (V) | 2.23[2] (2.50 + 3.90[3]) |
| δ Ori B | |
| Right ascension | 05h 31m 58.745s[4] |
| Declination | −00° 18′ 18.65″[4] |
| Apparent magnitude (V) | 14.0[5] |
| HD 36485 | |
| Right ascension | 05h 32m 00.406s[6] |
| Declination | −00° 17′ 04.38″[6] |
| Apparent magnitude (V) | 6.85[5] |
| Characteristics | |
| Spectral type | (O9.5II + B1V +B0IV[7]) + B3V[8] |
| U−B color index | −1.05[2] |
| B−V color index | −0.22[2] |
| Variable type | Eclipsing binary[9] |
| Astrometry | |
| Radial velocity (Rv) | 18.50 ± 0.5[10] km/s |
| Proper motion (μ) | RA: 0.64 ± 0.56[1] mas/yr Dec.: -0.69 ± 0.27[1] mas/yr |
| Parallax (π) | 4.71 ± 0.58[1] mas |
| Distance | 1,200[7] ly (380[7] pc) |
| Absolute magnitude (MV) | −5.8[5] |
| δ Ori Aa1 | |
| Absolute magnitude (MV) | −5.4[5] |
| δ Ori Aa2 | |
| Absolute magnitude (MV) | −2.9[5] |
| δ Ori Ab | |
| Absolute magnitude (MV) | −4.2[5] |
| Orbit[3] | |
| Primary | δ Ori Aa1 |
| Companion | δ Ori Aa2 |
| Period (P) | 5.732436 days |
| Semi-major axis (a) | 43.1 ± 1.7 R☉ |
| Eccentricity (e) | 0.1133 ± 0.0003 |
| Inclination (i) | 76.5 ± 0.2° |
| Periastron epoch (T) | 2456295.674 ± 0.062 |
| Argument of periastron (ω) (secondary) | 141.3 ± 0.2° |
| Details | |
| δ Ori Aa1 | |
| Mass | 24[7] M☉ |
| Radius | 16.5[7] R☉ |
| Luminosity | 190,000[7] L☉ |
| Surface gravity (log g) | 3.37 ± 0.15[7] cgs |
| Temperature | 29,500 ± 500[7] K |
| Rotational velocity (v sin i) | 130 ± 10[7] km/s |
| δ Ori Aa2 | |
| Mass | 8.4[7] M☉ |
| Radius | 6.5[7] R☉ |
| Luminosity | 16,000[7] L☉ |
| Surface gravity (log g) | 3.9[7] cgs |
| Temperature | 25,600 ± 3,000[7] K |
| Rotational velocity (v sin i) | 150 ± 50[7] km/s |
| δ Ori Ab | |
| Mass | 22.5[7] M☉ |
| Radius | 10.4[7] R☉ |
| Luminosity | 63,000[7] L☉ |
| Surface gravity (log g) | 3.5 ± 0.3[7] cgs |
| Temperature | 28,400 ± 1,500[7] K |
| Rotational velocity (v sin i) | 220 ± 20[7] km/s |
| δ Ori B | |
| Radius | 0.77[11] R☉ |
| Luminosity | 0.431[11] L☉ |
| Temperature | 5,324[11] K |
| HD 36485 | |
| Mass | ~9[8] M☉ |
| Radius | 5.7[12] R☉ |
| Luminosity | 3,300[12] L☉ |
| Surface gravity (log g) | 4.41[12] cgs |
| Temperature | 18,400[12] K |
| Other designations | |
| Mintaka Aa: HD 36486, HR 1851, SAO 132220/132221, BD−00°983, GC 6847 | |
| Mintaka Ab: δ Orionis B, CCDM J05320-0018D, WDS J05320-0018Ab | |
| δ Ori B: UCAC3 180-24383, CCDM J05320-0018B, WDS J05320-0018B | |
| HD 36485: δ Orionis C, HR 1851, SAO 132221, BD−00°982, GC 6848, PLX 1261, CCDM J05320-0018C | |
| Database references | |
| SIMBAD | data |
| δ Ori B | |
| HD 36485 | |
Mintaka /ˈmɪntəkə/,[13] designation Delta Orionis (δ Orionis, abbreviated Delta Ori, δ Ori) and 34 Orionis (34 Ori), is a multiple star system some 1,200 light-years from the Sun in the constellation of Orion. Together with Alnitak (Zeta Orionis) and Alnilam (Epsilon Orionis), the three stars form Orion's Belt, known by many names among ancient cultures. When Orion is near the meridian, Mintaka is the rightmost of the Belt's stars when viewed from the Northern Hemisphere facing south.
Nomenclature[edit]
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.[14] In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[15] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[16] 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.[17]
Observational history[edit]
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.[18] 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 Potsdam Observatory showed that the orbital period was 5.7 days.[19] 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.[19]
System[edit]
δ Orionis is a multiple star system. There is a magnitude 7 star about 52 arcseconds away from the second-magnitude primary and a much fainter star in between. The system is designated WDS 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.[20]
The primary component is itself a triple system: a class O9.5 bright giant and a class B main-sequence star orbit every 5.73 days and exhibit shallow eclipses when the star dims about 0.2 magnitudes,[9] and a B-class sub-giant is resolved 0.26" away.[3] 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.[21]
The seventh-magnitude companion, HD 36485, is a 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 emission and unusually strong helium absorption lines. 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.[8]
The 14th magnitude companion is thought to be around the same distance and is a somewhat cooler and less luminous star than the Sun.[11]
Mintaka is surrounded by a cluster of faint stars, possibly part of the cluster surrounding σ Ori.[22]
Distance[edit]
The distance derived from the Hipparcos satellite parallax is 212±30 pc,[1] while spectroscopic distances, comparisons to similar stars, and cluster membership all suggest a value more than double that.[23] This type of unreconcilable discrepancy is not unique to Mintaka and the reasons for it have yet to be clarified.[7] In Gaia Data Release 2, components B and C are listed with parallaxes of 3.4531±0.0371 mas and 2.5727±0.0767 mas, respectively,[11][24] implying distances considerably further than the Hipparcos-derived value for the primary.[1]
Etymology and cultural significance[edit]
Mintaka was seen by astrologers as a portent of good fortune.[14]
Orion's Belt[edit]
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 H•akk 'the Accurate Scale Beam'. In Chinese mythology, they were also known as the Weighing Beam.
In Chinese, 參宿 (Shēn Sù), meaning Three Stars (asterism), refers to an asterism consisting of Mintaka, Alnilam, and Alnitak (Orion's Belt), with Betelgeuse, Bellatrix, Saiph, and Rigel later added.[25] Consequently, the Chinese name for Mintaka is 參宿三 (Shēn Sù sān, English: the Third Star of Three Stars).[26] It is one of the western mansions of the White Tiger.
Namesakes[edit]
The USS Mintaka (AK-94) was a United States Navy Crater-class cargo ship named after the star.
See also[edit]
References[edit]
- ^ a b c d e f g van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. Vizier catalog entry
- ^ a b c Hoffleit, Dorrit; Jaschek, Carlos (1991). The Bright star catalogue (5th Revised ed.). New Haven, Conn.: Yale University Observatory. Bibcode:1991bsc..book.....H.
- ^ a b c Tokovinin, A. A. (1997). "MSC - a catalogue of physical multiple stars". Astronomy and Astrophysics Supplement Series. 124: 75–84. Bibcode:1997A&AS..124...75T. doi:10.1051/aas:1997181.
- ^ a b Zacharias, N.; Finch, C. T.; Girard, T. M.; Henden, A.; Bartlett, J. L.; Monet, D. G.; Zacharias, M. I. (2012). "VizieR Online Data Catalog: UCAC4 Catalogue (Zacharias+, 2012)". VizieR On-line Data Catalog: I/322A. Bibcode:2012yCat.1322....0Z.
- ^ a b c d e f Harvin, James A.; Gies, Douglas R.; Bagnuolo, William G.; Penny, Laura R.; Thaller, Michelle L. (2002). "Tomographic Separation of Composite Spectra. VIII. The Physical Properties of the Massive Compact Binary in the Triple Star System HD 36486 (δ Orionis A)". Astrophysical Journal. 565 (2): 1216. arXiv:astro-ph/0110683. Bibcode:2002ApJ...565.1216H. doi:10.1086/324705.
- ^ 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. doi:10.1888/0333750888/2862.
- ^ a b c d e f g h i j k l m n o p q r s t u v Shenar, T.; Oskinova, L.; Hamann, W.-R.; Corcoran, M. F.; Moffat, A. F. J.; Pablo, H.; Richardson, N. D.; Waldron, W. L.; Huenemoerder, D. P.; Maíz Apellániz, J.; Nichols, J. S.; Todt, H.; Nazé, Y.; Hoffman, J. L.; Pollock, A. M. T.; Negueruela, I. (2015). "A Coordinated X-Ray and Optical Campaign of the Nearest Massive Eclipsing Binary, δ Orionis Aa. IV. A Multiwavelength, Non-LTE Spectroscopic Analysis". Astrophysical Journal. 809 (2): 135. arXiv:1503.03476. Bibcode:2015ApJ...809..135S. doi:10.1088/0004-637X/809/2/135. hdl:10045/59172.
- ^ a b c Leone, F.; Bohlender, D. A.; Bolton, C. T.; Buemi, C.; Catanzaro, G.; Hill, G. M.; Stift, M. J. (2010). "The magnetic field and circumstellar environment of the helium-strong star HD36485 = δ Ori C". Monthly Notices of the Royal Astronomical Society. 401 (4): 2739. Bibcode:2010MNRAS.401.2739L. doi:10.1111/j.1365-2966.2009.15858.x.
- ^ a b Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007–2013)". VizieR On-line Data Catalog: B/gcvs. Bibcode:2009yCat....102025S.
- ^ Pourbaix, D.; Tokovinin, A. A.; Batten, A. H.; Fekel, F. C.; Hartkopf, W. I.; Levato, H.; Morrell, N. I.; Torres, G.; Udry, S. (2004). "SB9: The ninth catalogue of spectroscopic binary orbits". Astronomy and Astrophysics. 424 (2): 727. arXiv:astro-ph/0406573. Bibcode:2004A&A...424..727P. doi:10.1051/0004-6361:20041213.
- ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ a b c d Zboril, M.; North, P.; Glagolevskij, Yu. V.; Betrix, F. (1997). "Properties of He-rich stars. I. Their evolutionary state and helium abundance". Astronomy and Astrophysics. 324: 949. Bibcode:1997A&A...324..949Z.
- ^ Rumrill, H. B. (June 1936). "Star Name Pronunciation". Publications of the Astronomical Society of the Pacific. San Francisco, California. 48 (283): 139. Bibcode:1936PASP...48..139R. doi:10.1086/124681.
- ^ a b Allen, Richard Hinckley (1963) [1899]. Star-names and their meanings. New York, NY: Dover Publications. p. 314. ISBN 1-931559-44-9.
- ^ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
- ^ "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
- ^ "IAU Catalog of Star Names". Retrieved 28 July 2016.
- ^ Deslandres, H. (1900). "Variable velocity in line of sight of delta Orionis. (Notes)". The Observatory. 23: 148. Bibcode:1900Obs....23..148D.
- ^ a b Hartmann, J. (1904). "Investigations on the spectrum and orbit of delta Orionis". Astrophysical Journal. 19: 268–286. Bibcode:1904ApJ....19..268H. doi:10.1086/141112.
- ^ Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.
- ^ Zasche, P.; Wolf, M.; Hartkopf, W. I.; Svoboda, P.; Uhlař, R.; Liakos, A.; Gazeas, K. (2009). "A Catalog of Visual Double and Multiple Stars with Eclipsing Components". Astronomical Journal. 138 (2): 664. arXiv:0907.5172. Bibcode:2009AJ....138..664Z. doi:10.1088/0004-6256/138/2/664.
- ^ Caballero, J. A.; Solano, E. (2008). "Young stars and brown dwarfs surrounding Alnilam (ɛ Orionis) and Mintaka (δ Orionis)". Astronomy and Astrophysics. 485 (3): 931. arXiv:0804.2184. Bibcode:2008A&A...485..931C. doi:10.1051/0004-6361:200809595.
- ^ Corcoran, M. F.; Nichols, J. S.; Pablo, H.; Shenar, T.; Pollock, A. M. T.; Waldron, W. L.; Moffat, A. F. J.; Richardson, N. D.; Russell, C. M. P.; Hamaguchi, K.; Huenemoerder, D. P.; Oskinova, L.; Hamann, W.-R.; Nazé, Y.; Ignace, R.; Evans, N. R.; Lomax, J. R.; Hoffman, J. L.; Gayley, K.; Owocki, S. P.; Leutenegger, M.; Gull, T. R.; Hole, K. T.; Lauer, J.; Iping, R. C. (2015). "A Coordinated X-Ray and Optical Campaign of the Nearest Massive Eclipsing Binary, δ Orionis Aa. I. Overview of the X-Ray Spectrum". Astrophysical Journal. 809 (2): 132. arXiv:1507.05101. Bibcode:2015ApJ...809..132C. doi:10.1088/0004-637X/809/2/132.
- ^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
- ^ (in Chinese) 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
- ^ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 5 月 25 日
