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Beta Tauri

January 05, 2023

Beta Tauri is the second-brightest star in the constellation of Taurus. It has the official name Elnath;[12] Beta Tauri is the current Bayer designation, which is Latinised from β Tauri and abbreviated Beta Tau or β Tau. The original designation of Gamma Aurigae is now rarely used. It is a chemically peculiar B7 giant star, 134 light years away from the Sun with an apparent magnitude of 1.65.

β Tauri
Location of β Tauri (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Taurus
Pronunciation /ɛlˈnæθ/[1] or /ˈɛlnæθ/[2]
Right ascension 05h 26m 17.51312s[3]
Declination 28° 36′ 26.8262″[3]
Apparent magnitude (V) 1.65[4]
Characteristics
Spectral type B7III[5]
U−B color index −0.49[4]
B−V color index −0.13[4]
Astrometry
Radial velocity (Rv)9.2[6] km/s
Proper motion (μ) RA: +22.76[3] mas/yr
Dec.: −173.58[3] mas/yr
Parallax (π)24.36 ± 0.34 mas[3]
Distance134 ± 2 ly
(41.1 ± 0.6 pc)
Absolute magnitude (MV)−1.42[7]
Details
Mass5.0±0.1[8] M☉
Radius4.2[9] R☉
Luminosity700[10] L☉
Surface gravity (log g)3.65[11] cgs
Temperature13,824±475[9] K
Metallicity [Fe/H]+0.08[11] dex
Rotational velocity (v sin i)59[11] km/s
Age100±10[8] Myr
Other designations
Elnath, El Nath, Alnath, Gamma Aurigae, 112 Tauri, BD+28°795, FK5 202, GC 6681, HD 35497, HIP 25428, HR 1791, SAO 77168, CCDM 05263+2836
Database references
SIMBADdata

Nomenclature

This star has two Bayer designations: β Tauri (Latinised to Beta Tauri) and γ Aurigae (Latinised to Gamma Aurigae). Ptolemy considered the star to be shared by Auriga, and Johann Bayer assigned it a designation in both constellations. When the modern constellation boundaries were fixed in 1930, the designation γ Aurigae largely dropped from use.[13]

The traditional name Elnath, variously El Nath or Alnath, comes from the Arabic word النطح an-naţħ, meaning "the butting" (i.e. the bull's horns). As in many other Arabic star names, the article ال is transliterated literally as el, yet overwhelmingly in Arabic pronunciation it is assimilated to the n, meaning it is omitted. In 2016, the International Astronomical Union organized a Working Group on Star Names (WGSN)[14] to catalog and standardize proper names for stars. The WGSN's first bulletin of July 2016[15] included a table of the first two batches of names approved by the WGSN; which included Elnath for this star.

In Chinese, 五車 (Wǔ Chē), meaning Five Chariots, refers to an asterism consisting of β Tauri, ι Aurigae, Capella, β Aurigae and θ Aurigae.[16] Consequently, the Chinese name for β Tauri itself is 五車五 (Wǔ Chē Wǔ; English: Fifth of the Five Chariots.)[17]

Physical properties

The absolute magnitude of Beta Tauri is −1.34, similar to another star in Taurus, Maia in the Pleiades star cluster. Like Maia, β Tauri is a B-class giant with a luminosity 700 times solar (L☉).[10] It has evolved to become a giant star, larger and cooler than when it was on the main sequence.[18] However, being approximately 130 light-years distant compared to Maia's estimated 360 light-years, β Tauri ranks as the second-brightest star in the constellation.

It is a mercury-manganese star, a type of non-magnetic chemically peculiar star with unusually large signatures of some heavy elements in its spectrum.[11] Relative to the Sun, β Tauri is notable for a high abundance of manganese, but little calcium and magnesium.[10][19] However, the lack of strong mercury signatures, together with notably high levels of silicon and chromium, have led some authors to give other classifications, including as a "SrCrEu star" or even an Ap star.[20][21] Its limb-darkened angular diameter has been measured at 1.090±0.076 mas. At a distance of 41.1 pc, this corresponds to a linear radius of 4.82±0.34 R☉.[22]

At the southern edge of the narrow plane of the Milky Way Galaxy a few degrees west of the galactic anticenter, β Tauri figures (appears) as a foreground object south of many nebulae and star clusters such as M36, M37, and M38.[23] It is 5.39 degrees north of the ecliptic, still few enough to be occultable by the Moon. Such occultations occur when the Moon's ascending node is near the March equinox, as in 2007. Most are visible only in the Southern Hemisphere, because the star is at the northern edge of the lunar occultation zone – but rarely as far north as southern California.[24]

Companions

A faint star is, angularly from our viewpoint, close enough for astronomers to consider, and guides to mention, the pair as a double star. This visual companion, BD+28°795B, has a position angle of 239 degrees and is separated from the main star by 33.4 arcseconds (″).[25][26] Six angularly closer, even fainter stars have been found in a search for brown dwarf and planetary companions – all considered background objects.[27]

A very close companion was reported from lunar occultation measurements at a distance of 0.1″, but not confirmed by other observers. Radial velocity measurements indicate that Beta Tauri is a single-lined spectroscopic binary, but there is no published information about the companion or orbit.[28][22]

References

  1. ^ "Alnath". Oxford English Dictionary (Online ed.). Oxford University Press. (Subscription or participating institution membership required.)
  2. ^ Kunitzsch, Paul; Smart, Tim (2006). A Dictionary of Modern star Names: A Short Guide to 254 Star Names and Their Derivations (2nd rev. ed.). Cambridge, Massachusetts: Sky Pub. ISBN 978-1-931559-44-7.
  3. ^ a b c d e 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. S2CID 18759600. Vizier catalog entry
  4. ^ a b c Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237: 0. Bibcode:2002yCat.2237....0D.
  5. ^ Garrison, R. F; Gray, R. O (1994). "The late B-type stars: Refined MK classification, confrontation with stromgren photometry, and the effects of rotation". The Astronomical Journal. 107: 1556. Bibcode:1994AJ....107.1556G. doi:10.1086/116967.
  6. ^ Evans, D. S (1967). "The Revision of the General Catalogue of Radial Velocities". Determination of Radial Velocities and Their Applications. 30: 57. Bibcode:1967IAUS...30...57E.
  7. ^ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  8. ^ a b Janson, Markus; et al. (August 2011). "High-contrast Imaging Search for Planets and Brown Dwarfs around the Most Massive Stars in the Solar Neighborhood". The Astrophysical Journal. 736 (2): 89. arXiv:1105.2577. Bibcode:2011ApJ...736...89J. doi:10.1088/0004-637X/736/2/89. S2CID 119217803.
  9. ^ a b Underhill, A. B.; et al. (November 1979). "Effective temperatures, angular diameters, distances and linear radii for 160 O and B stars". Monthly Notices of the Royal Astronomical Society. 189 (3): 601–605. Bibcode:1979MNRAS.189..601U. doi:10.1093/mnras/189.3.601.
  10. ^ a b c Kaler, James B. "ELNATH (Beta Tauri)". University of Illinois. Retrieved 2010-03-07.
  11. ^ a b c d Ghazaryan, S; Alecian, G (2016). "Statistical analysis from recent abundance determinations in HgMn stars". Monthly Notices of the Royal Astronomical Society. 460 (2): 1912. Bibcode:2016MNRAS.460.1912G. doi:10.1093/mnras/stw911.
  12. ^ "IAU Catalog of Star Names". Retrieved 28 July 2016.
  13. ^ Ian Ridpath. "Bayer's Uranometria and Bayer letters". Retrieved 2017-11-27.
  14. ^ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
  15. ^ "Bulletin of the IAU Working Group on Star Names, No. 1" (PDF). Retrieved 28 July 2016.
  16. ^ (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.
  17. ^ (in Chinese) 香港太空館 - 研究資源 - 亮星中英對照表 2011-01-30 at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.
  18. ^ Knyazeva, L. N; Kharitonov, A. V (2000). "The Normal Energy Distributions in Stellar Spectra: Giants and Supergiants". Astronomy Reports. 44 (8): 548. Bibcode:2000ARep...44..548K. doi:10.1134/1.1306355. S2CID 120800469.
  19. ^ Heacox, W. D. (1979). "Chemical abundances in Hg-Mn stars". Astrophysical Journal Supplement Series. 41: 675. Bibcode:1979ApJS...41..675H. doi:10.1086/190637.
  20. ^ Chen, P. S; Liu, J. Y; Shan, H. G (2017). "A New Photometric Study of Ap and Am Stars in the Infrared". The Astronomical Journal. 153 (5): 218. Bibcode:2017AJ....153..218C. doi:10.3847/1538-3881/aa679a.
  21. ^ Bychkov, V. D; Bychkova, L. V; Madej, J (2009). "Catalogue of averaged stellar effective magnetic fields - II. Re-discussion of chemically peculiar a and B stars". Monthly Notices of the Royal Astronomical Society. 394 (3): 1338. Bibcode:2009MNRAS.394.1338B. doi:10.1111/j.1365-2966.2008.14227.x.
  22. ^ a b Gordon, Kathryn D.; Gies, Douglas R.; Schaefer, Gail H.; Huber, Daniel; Ireland, Michael (2019). "Angular Sizes, Radii, and Effective Temperatures of B-type Stars from Optical Interferometry with the CHARA Array". The Astrophysical Journal. 873 (1): 91. Bibcode:2019ApJ...873...91G. doi:10.3847/1538-4357/ab04b2. S2CID 125181833.
  23. ^ Nemiroff, R.; Bonnell, J., eds. (5 March 2010). "Deep Auriga". Astronomy Picture of the Day. NASA. Retrieved 2010-03-07.
  24. ^ . Abrams Planetarium. Archived from the original on August 30, 2007.
  25. ^ "CCDM (Catalog of Components of Double & Multiple stars (Dommanget+ 2002)". VizieR. Centre de Données astronomiques de Strasbourg. Retrieved 2010-03-07.
  26. ^ "Al Nath". Alcyone Bright Star Catalogue. Retrieved 2010-03-07.
  27. ^ Janson, Markus; Bonavita, Mariangela; Klahr, Hubert; Lafrenière, David; Jayawardhana, Ray; Zinnecker, Hans (2011). "High-contrast Imaging Search for Planets and Brown Dwarfs around the Most Massive Stars in the Solar Neighborhood". The Astrophysical Journal. 736 (2): 89. arXiv:1105.2577. Bibcode:2011ApJ...736...89J. doi:10.1088/0004-637X/736/2/89. S2CID 119217803.
  28. ^ Adelman, S. J.; Caliskan, H.; Gulliver, A. F.; Teker, A. (2006). "Elemental abundance analyses with DAO spectrograms". Astronomy & Astrophysics. 447 (2): 685–690. doi:10.1051/0004-6361:20053581.

External links

  • Jim Kaler's Stars:
  • NASA Astronomy Picture of the Day: Image of Elnath (5 March 2010)

January 05, 2023
beta, tauri, second, brightest, star, constellation, taurus, official, name, elnath, current, bayer, designation, which, latinised, from, tauri, abbreviated, beta, original, designation, gamma, aurigae, rarely, used, chemically, peculiar, giant, star, light, y. Beta Tauri is the second brightest star in the constellation of Taurus It has the official name Elnath 12 Beta Tauri is the current Bayer designation which is Latinised from b Tauri and abbreviated Beta Tau or b Tau The original designation of Gamma Aurigae is now rarely used It is a chemically peculiar B7 giant star 134 light years away from the Sun with an apparent magnitude of 1 65 b TauriLocation of b Tauri circled Observation dataEpoch J2000 Equinox J2000Constellation TaurusPronunciation ɛ l ˈ n ae 8 1 or ˈ ɛ l n ae 8 2 Right ascension 05h 26m 17 51312s 3 Declination 28 36 26 8262 3 Apparent magnitude V 1 65 4 CharacteristicsSpectral type B7III 5 U B color index 0 49 4 B V color index 0 13 4 AstrometryRadial velocity Rv 9 2 6 km sProper motion m RA 22 76 3 mas yr Dec 173 58 3 mas yrParallax p 24 36 0 34 mas 3 Distance134 2 ly 41 1 0 6 pc Absolute magnitude MV 1 42 7 DetailsMass5 0 0 1 8 M Radius4 2 9 R Luminosity700 10 L Surface gravity log g 3 65 11 cgsTemperature13 824 475 9 KMetallicity Fe H 0 08 11 dexRotational velocity v sin i 59 11 km sAge100 10 8 MyrOther designationsElnath El Nath Alnath Gamma Aurigae 112 Tauri BD 28 795 FK5 202 GC 6681 HD 35497 HIP 25428 HR 1791 SAO 77168 CCDM 05263 2836Database referencesSIMBADdata Contents 1 Nomenclature 2 Physical properties 3 Companions 4 References 5 External linksNomenclature EditThis star has two Bayer designations b Tauri Latinised to Beta Tauri and g Aurigae Latinised to Gamma Aurigae Ptolemy considered the star to be shared by Auriga and Johann Bayer assigned it a designation in both constellations When the modern constellation boundaries were fixed in 1930 the designation g Aurigae largely dropped from use 13 The traditional name Elnath variously El Nath or Alnath comes from the Arabic word النطح an naţħ meaning the butting i e the bull s horns As in many other Arabic star names the article ال is transliterated literally as el yet overwhelmingly in Arabic pronunciation it is assimilated to the n meaning it is omitted In 2016 the International Astronomical Union organized a Working Group on Star Names WGSN 14 to catalog and standardize proper names for stars The WGSN s first bulletin of July 2016 15 included a table of the first two batches of names approved by the WGSN which included Elnath for this star In Chinese 五車 Wǔ Che meaning Five Chariots refers to an asterism consisting of b Tauri i Aurigae Capella b Aurigae and 8 Aurigae 16 Consequently the Chinese name for b Tauri itself is 五車五 Wǔ Che Wǔ English Fifth of the Five Chariots 17 Physical properties EditThe absolute magnitude of Beta Tauri is 1 34 similar to another star in Taurus Maia in the Pleiades star cluster Like Maia b Tauri is a B class giant with a luminosity 700 times solar L 10 It has evolved to become a giant star larger and cooler than when it was on the main sequence 18 However being approximately 130 light years distant compared to Maia s estimated 360 light years b Tauri ranks as the second brightest star in the constellation It is a mercury manganese star a type of non magnetic chemically peculiar star with unusually large signatures of some heavy elements in its spectrum 11 Relative to the Sun b Tauri is notable for a high abundance of manganese but little calcium and magnesium 10 19 However the lack of strong mercury signatures together with notably high levels of silicon and chromium have led some authors to give other classifications including as a SrCrEu star or even an Ap star 20 21 Its limb darkened angular diameter has been measured at 1 090 0 076 mas At a distance of 41 1 pc this corresponds to a linear radius of 4 82 0 34 R 22 At the southern edge of the narrow plane of the Milky Way Galaxy a few degrees west of the galactic anticenter b Tauri figures appears as a foreground object south of many nebulae and star clusters such as M36 M37 and M38 23 It is 5 39 degrees north of the ecliptic still few enough to be occultable by the Moon Such occultations occur when the Moon s ascending node is near the March equinox as in 2007 Most are visible only in the Southern Hemisphere because the star is at the northern edge of the lunar occultation zone but rarely as far north as southern California 24 Companions EditA faint star is angularly from our viewpoint close enough for astronomers to consider and guides to mention the pair as a double star This visual companion BD 28 795B has a position angle of 239 degrees and is separated from the main star by 33 4 arcseconds 25 26 Six angularly closer even fainter stars have been found in a search for brown dwarf and planetary companions all considered background objects 27 A very close companion was reported from lunar occultation measurements at a distance of 0 1 but not confirmed by other observers Radial velocity measurements indicate that Beta Tauri is a single lined spectroscopic binary but there is no published information about the companion or orbit 28 22 References Edit Alnath Oxford English Dictionary Online ed Oxford University Press Subscription or participating institution membership required Kunitzsch Paul Smart Tim 2006 A Dictionary of Modern star Names A Short Guide to 254 Star Names and Their Derivations 2nd rev ed Cambridge Massachusetts Sky Pub ISBN 978 1 931559 44 7 a b c d e Van Leeuwen F 2007 Validation of the new Hipparcos reduction Astronomy and Astrophysics 474 2 653 664 arXiv 0708 1752 Bibcode 2007A amp A 474 653V doi 10 1051 0004 6361 20078357 S2CID 18759600 Vizier catalog entry a b c Ducati J R 2002 VizieR Online Data Catalog Catalogue of Stellar Photometry in Johnson s 11 color system CDS ADC Collection of Electronic Catalogues 2237 0 Bibcode 2002yCat 2237 0D Garrison R F Gray R O 1994 The late B type stars Refined MK classification confrontation with stromgren photometry and the effects of rotation The Astronomical Journal 107 1556 Bibcode 1994AJ 107 1556G doi 10 1086 116967 Evans D S 1967 The Revision of the General Catalogue of Radial Velocities Determination of Radial Velocities and Their Applications 30 57 Bibcode 1967IAUS 30 57E Anderson E Francis Ch 2012 XHIP An extended hipparcos compilation Astronomy Letters 38 5 331 arXiv 1108 4971 Bibcode 2012AstL 38 331A doi 10 1134 S1063773712050015 S2CID 119257644 a b Janson Markus et al August 2011 High contrast Imaging Search for Planets and Brown Dwarfs around the Most Massive Stars in the Solar Neighborhood The Astrophysical Journal 736 2 89 arXiv 1105 2577 Bibcode 2011ApJ 736 89J doi 10 1088 0004 637X 736 2 89 S2CID 119217803 a b Underhill A B et al November 1979 Effective temperatures angular diameters distances and linear radii for 160 O and B stars Monthly Notices of the Royal Astronomical Society 189 3 601 605 Bibcode 1979MNRAS 189 601U doi 10 1093 mnras 189 3 601 a b c Kaler James B ELNATH Beta Tauri University of Illinois Retrieved 2010 03 07 a b c d Ghazaryan S Alecian G 2016 Statistical analysis from recent abundance determinations in HgMn stars Monthly Notices of the Royal Astronomical Society 460 2 1912 Bibcode 2016MNRAS 460 1912G doi 10 1093 mnras stw911 IAU Catalog of Star Names Retrieved 28 July 2016 Ian Ridpath Bayer s Uranometria and Bayer letters Retrieved 2017 11 27 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 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 香港太空館 研究資源 亮星中英對照表 Archived 2011 01 30 at the Wayback Machine Hong Kong Space Museum Accessed on line November 23 2010 Knyazeva L N Kharitonov A V 2000 The Normal Energy Distributions in Stellar Spectra Giants and Supergiants Astronomy Reports 44 8 548 Bibcode 2000ARep 44 548K doi 10 1134 1 1306355 S2CID 120800469 Heacox W D 1979 Chemical abundances in Hg Mn stars Astrophysical Journal Supplement Series 41 675 Bibcode 1979ApJS 41 675H doi 10 1086 190637 Chen P S Liu J Y Shan H G 2017 A New Photometric Study of Ap and Am Stars in the Infrared The Astronomical Journal 153 5 218 Bibcode 2017AJ 153 218C doi 10 3847 1538 3881 aa679a Bychkov V D Bychkova L V Madej J 2009 Catalogue of averaged stellar effective magnetic fields II Re discussion of chemically peculiar a and B stars Monthly Notices of the Royal Astronomical Society 394 3 1338 Bibcode 2009MNRAS 394 1338B doi 10 1111 j 1365 2966 2008 14227 x a b Gordon Kathryn D Gies Douglas R Schaefer Gail H Huber Daniel Ireland Michael 2019 Angular Sizes Radii and Effective Temperatures of B type Stars from Optical Interferometry with the CHARA Array The Astrophysical Journal 873 1 91 Bibcode 2019ApJ 873 91G doi 10 3847 1538 4357 ab04b2 S2CID 125181833 Nemiroff R Bonnell J eds 5 March 2010 Deep Auriga Astronomy Picture of the Day NASA Retrieved 2010 03 07 Skywatcher s Diary Abrams Planetarium Archived from the original on August 30 2007 CCDM Catalog of Components of Double amp Multiple stars Dommanget 2002 VizieR Centre de Donnees astronomiques de Strasbourg Retrieved 2010 03 07 Al Nath Alcyone Bright Star Catalogue Retrieved 2010 03 07 Janson Markus Bonavita Mariangela Klahr Hubert Lafreniere David Jayawardhana Ray Zinnecker Hans 2011 High contrast Imaging Search for Planets and Brown Dwarfs around the Most Massive Stars in the Solar Neighborhood The Astrophysical Journal 736 2 89 arXiv 1105 2577 Bibcode 2011ApJ 736 89J doi 10 1088 0004 637X 736 2 89 S2CID 119217803 Adelman S J Caliskan H Gulliver A F Teker A 2006 Elemental abundance analyses with DAO spectrograms Astronomy amp Astrophysics 447 2 685 690 doi 10 1051 0004 6361 20053581 External links EditJim Kaler s Stars Elnath NASA Astronomy Picture of the Day Image of Elnath 5 March 2010 Retrieved from https en wikipedia org w index php title Beta Tauri amp oldid 1121970087, wikipedia, wiki, book, books, library,

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