Astronomy:Theta Tauri

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Short description: Binary star in the constellation Taurus
θ Tauri
280px
Hyades showing θ Tauri
Observation data
{{#ifeq:J2000.0|J2000.0 (ICRS)|Epoch J2000.0      Equinox J2000.0 (ICRS)| [[History:Epoch|Epoch J2000.0]]      [[Astronomy:Equinox (celestial coordinates)|Equinox J2000.0}}
Constellation Taurus
θ1 Tauri
Right ascension  04h 28m 34.49209s[1]
Declination +15° 57′ 44.2832″[2]
Apparent magnitude (V) +3.84
θ2 Tauri
Right ascension  04h 28m 39.74455s[1]
Declination +15° 52′ 15.1226″[2]
Apparent magnitude (V) +3.35 - 3.42[3]
Characteristics
θ1 Tauri
Spectral type G9 III Fe-0.5[4]
θ2 Tauri
Spectral type A7 III[5]
Variable type δ Scuti[3]
Astrometry
θ1 Tauri
Parallax (π)21.4183 ± 0.3731[1] mas
Distance152 ± 3 ly
(46.7 ± 0.8 pc)
Absolute magnitude (MV)+0.416[6]
θ2 Tauri
Parallax (π)20.8354 ± 0.3731[2] mas
Distance157 ± 3 ly
(48.0 ± 0.9 pc)
Absolute magnitude (MV)+0.08[7]
Orbit[8]
PrimaryA
CompanionB
Period (P)5,997 days
Eccentricity (e)0.64
Semi-amplitude (K1)
(primary)		8.39 km/s
Orbit[9]
PrimaryAa
CompanionAb
Period (P)140.7302 days
Semi-major axis (a)18.91″
Eccentricity (e)0.7360
Inclination (i)47.8°
Semi-amplitude (K1)
(primary)		32.95 km/s
Semi-amplitude (K2)
(secondary)		43.68 km/s
Details
Aa
Mass2.86[10] M☉
Radius4.4[10] R☉
Luminosity59[9] L☉
Surface gravity (log g)3.6[10] cgs
Temperature7,800[10] K
Rotational velocity (v sin i)68.4[9] km/s
Ab
Mass2.16[10] M☉
Radius2.7[10] R☉
Luminosity21[9] L☉
Temperature7,800[9] K
Rotational velocity (v sin i)113[9] km/s
Age650[9] Myr
θ1 Tauri
Mass2.67[11] M☉
Radius9.42±0.22[12] R☉
Luminosity47.7±2.3[12] L☉
Surface gravity (log g)3.21[11] cgs
Temperature4,940±55[12] K
Metallicity [Fe/H]+0.14[11] dex
Rotational velocity (v sin i)1.40[11] km/s
Age510[11] Myr
Other designations
θ Tauri
θ1 Tauri: 77 Tauri, BD+15 631, HD 28307, HIP 20885, HR 1411, SAO 93955
θ2 Tauri: Chamukuy, 78 Tauri, BD+15 632, HD 28319, HIP 20894, HR 1412, SAO 93957
Database references
SIMBADθ1 Tauri
θ2 Tauri

Theta Tauri (θ Tauri, abbreviated Theta Tau, θ Tau) is a wide double star in the constellation of Taurus and a member of the Hyades open cluster.

θ Tauri is composed of two 3rd magnitude stars, designated Theta1 Tauri (Theta Tauri B) and Theta2 Tauri (Theta Tauri A). Theta² is brighter, hence the pair are sometimes referred to as Theta Tauri B and A, respectively. They are separated by 5.62 arcminutes (0.094°) on the sky. Based upon parallax measurements, Theta¹ Tauri is located at a distance of 152 ly (47 pc), while Theta² Tauri is at a distance of 157 light-years (48 parsecs). θ Tauri A and B are both spectroscopic binaries; the four components are designated Theta Tauri Aa (formally named Chamukuy /ˈtʃɑːmuːkuːi/), Ab, Ba, and Bb.

Nomenclature

The θ Tauri pair, showing contrasting blue and yellow colors, in the Hyades cluster. In this image, θ1 Tauri is above in yellow, and θ2 Tauri is below in light blue.

θ Tauri (Latinised to Theta Tauri) is the double star's Bayer designation; θ1 Tauri and θ2 Tauri those of its two constituents. The designations of the two constituents as Theta Tauri A and B, and those of the four components - Theta Tauri Aa, Ab, Ba and Bb - derive from the convention used by the Washington Multiplicity Catalog (WMC) for multiple star systems, and adopted by the International Astronomical Union (IAU).[13]

In the mythology of the Maya peoples, Theta Tauri is known as Chamukuy, meaning a small bird in the Yucatec Maya language.[14] In 2016, the IAU organized a Working Group on Star Names (WGSN)[15] to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[16] It approved the name Chamukuy for the component Theta Tauri Aa on 5 September 2017 and it is now so included in the List of IAU-approved Star Names.[17]

In Chinese, 畢宿 (Bì Xiù), meaning Net, refers to an asterism consisting of Theta² Tauri, Epsilon Tauri (named Ain), Delta³ Tauri, Delta¹ Tauri, Gamma Tauri, Alpha Tauri (Aldebaran), 71 Tauri and Lambda Tauri.[18] Consequently, the Chinese name for Theta² Tauri itself is 畢宿六 (Bì Xiù liù), "the Sixth Star of Net".[19]

Properties

A light curve for Theta2 Tauri, plotted from TESS data[20]

Theta Tauri A has a mean apparent magnitude of +3.40. It is classified as a Delta Scuti type variable star and its brightness varies from magnitude +3.35 to +3.42 with a period of 1.82 hours.[21] Its primary component, Theta Tauri Aa, is a white A-type giant. The secondary, Theta Tauri Ab, is of the 6th magnitude and is 0.005 arcseconds, or at least 2 AU, distant. It completes an orbit once every 141 days.

Theta Tauri B is the dimmer constituent. Its primary component, Theta Tauri Ba, is an orange K-type giant with an apparent magnitude of +3.84. The secondary, Theta Tauri Bb, is of the 7th-magnitude. It has a mass of 1.31 M☉ and orbits the primary every 16.26 years on a fairly eccentric (at 0.570) orbit.[22]

References

  1. ↑ 1.0 1.1 1.2 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  2. ↑ 2.0 2.1 2.2 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G.  Gaia DR2 record for this source at VizieR.
  3. ↑ 3.0 3.1 Samus, N. N. et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus+ 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S 1: B/GCVS. Bibcode: 2009yCat....102025S. 
  4. ↑ Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins Catalog of Revised MK Types for the Cooler Stars". The Astrophysical Journal Supplement Series 71: 245. doi:10.1086/191373. Bibcode: 1989ApJS...71..245K. 
  5. ↑ Morgan, W. W.; Abt, Helmut A.; Tapscott, J. W. (1978). Revised MK Spectral Atlas for stars earlier than the sun. Bibcode: 1978rmsa.book.....M. 
  6. ↑ Böhm-Vitense, Erika et al. (December 2000). "Ultraviolet Emission Lines in BA and Non-BA Giants". The Astrophysical Journal 545 (2): 992–999. doi:10.1086/317850. Bibcode: 2000ApJ...545..992B. 
  7. ↑ Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A. 
  8. ↑ Mermilliod, J. -C; Andersen, J.; Latham, D. W.; Mayor, M. (2007). "Red giants in open clusters. XIII. Orbital elements of 156 spectroscopic binaries". Astronomy and Astrophysics 473 (3): 829. doi:10.1051/0004-6361:20078007. Bibcode: 2007A&A...473..829M. 
  9. ↑ 9.0 9.1 9.2 9.3 9.4 9.5 9.6 Torres, K. B. V.; Lampens, P.; Frémat, Y.; Hensberge, H.; Lebreton, Y.; Škoda, P.; Guenther, E.; Schwope, A. et al. (2011). "Spectra disentangling applied to the Hyades binary θ2 Tauri AB: New orbit, orbital parallax and component properties". Astronomy and Astrophysics 525: A50. doi:10.1051/0004-6361/201015166. Bibcode: 2011A&A...525A..50T. 
  10. ↑ 10.0 10.1 10.2 10.3 10.4 10.5 Liakos, Alexios; Niarchos, Panagiotis (2017). "Catalogue and properties of δ Scuti stars in binaries". Monthly Notices of the Royal Astronomical Society 465 (1): 1181. doi:10.1093/mnras/stw2756. Bibcode: 2017MNRAS.465.1181L. 
  11. ↑ 11.0 11.1 11.2 11.3 11.4 Jofré, E.; Petrucci, R.; Saffe, C.; Saker, L.; de la Villarmois, E. Artur; Chavero, C.; Gómez, M.; Mauas, P. J. D. et al. (2015). "Stellar parameters and chemical abundances of 223 evolved stars with and without planets". Astronomy and Astrophysics 574: A50. doi:10.1051/0004-6361/201424474. Bibcode: 2015A&A...574A..50J. 
  12. ↑ 12.0 12.1 12.2 Baines, Ellyn K.; Thomas Armstrong, J.; Clark, James H.; Gorney, Jim; Hutter, Donald J.; Jorgensen, Anders M.; Kyte, Casey; Mozurkewich, David et al. (2021). "Angular Diameters and Fundamental Parameters of Forty-four Stars from the Navy Precision Optical Interferometer". The Astronomical Journal 162 (5): 198. doi:10.3847/1538-3881/ac2431. Bibcode: 2021AJ....162..198B. 
  13. ↑ Hessman, F. V.; Dhillon, V. S.; Winget, D. E.; Schreiber, M. R.; Horne, K.; Marsh, T. R.; Guenther, E.; Schwope, A.; Heber, U. (2010). "On the naming convention used for multiple star systems and extrasolar planets". arXiv:1012.0707 [astro-ph.SR].
  14. ↑ Susan Milbrath (1 January 2010). Star Gods of the Maya: Astronomy in Art, Folklore, and Calendars. University of Texas Press. ISBN 978-0-292-77851-1. https://books.google.com/books?id=kd7_dzfVK_AC. 
  15. ↑ "IAU Working Group on Star Names (WGSN)". https://www.iau.org/science/scientific_bodies/working_groups/280/. Retrieved 22 May 2016. 
  16. ↑ "WG Triennial Report (2015-2018) - Star Names". p. 5. https://www.iau.org/static/science/scientific_bodies/working_groups/280/wg-starnames-triennial-report-2015-2018.pdf. Retrieved 2018-07-14. 
  17. ↑ "Naming Stars". IAU.org. https://www.iau.org/public/themes/naming_stars/. Retrieved 16 December 2017. 
  18. ↑ 陳久金 (2005). 中國星座神話. 五南圖書出版股份有限公司. ISBN 978-986-7332-25-7. https://books.google.com/books?id=0Vex0rYzdu8C. 
  19. ↑ (in Chinese) 香港太空館 - 研究資源 - 亮星中英對照表 , Hong Kong Space Museum. Accessed on line November 23, 2010.
  20. ↑ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html. 
  21. ↑ Solano, E.; Fernley, J. (April 1997). "Spectroscopic survey of delta Scuti stars. I. Rotation velocities and effective temperatures". Astronomy & Astrophysics Supplement Series 122: 131–147. doi:10.1051/aas:1997329. Bibcode: 1997A&AS..122..131S. 
  22. ↑ Torres, Guillermo; Stefanik, Robert P.; Latham, David W. (1997). "The Hyades Binaries θ1 Tauri and θ2Tauri: The Distance to the Cluster and the Mass-Luminosity Relation". The Astrophysical Journal 485 (1): 167. doi:10.1086/304422. Bibcode: 1997ApJ...485..167T. 



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