 Hyades showing θ Tauri | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Taurus |
| θ1 Tauri | |
| Right ascension | 04h 28m 34.49603s[1] |
| Declination | +15° 57′ 43.8494″[1] |
| Apparent magnitude (V) | +3.84 |
| θ2 Tauri | |
| Right ascension | 04h 28m 39.74070s[1] |
| Declination | +15° 52′ 15.1745″[1] |
| Apparent magnitude (V) | +3.35 - 3.42[2] |
| Characteristics | |
| θ1 Tauri | |
| Spectral type | G9 III Fe-0.5[3] |
| θ2 Tauri | |
| Spectral type | A7 III[4] |
| Variable type | δ Scuti[2] |
| Astrometry | |
| θ1 Tauri | |
| Parallax (π) | 21.4183 ± 0.3731 mas[5] |
| Distance | 152 ± 3 ly (46.7 ± 0.8 pc) |
| Absolute magnitude (MV) | +0.416[6] |
| θ2 Tauri | |
| Parallax (π) | 20.8354 ± 0.3731 mas[7] |
| Distance | 157 ± 3 ly (48.0 ± 0.9 pc) |
| Absolute magnitude (MV) | +0.30/+1.44[8] |
| Orbit[9] | |
| Primary | A |
| Companion | B |
| Period (P) | 5,997 days |
| Eccentricity (e) | 0.64 |
| Semi-amplitude (K1) (primary) | 8.39 km/s |
| Orbit[8] | |
| Primary | Aa |
| Companion | Ab |
| 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 | |
| Mass | 2.86[10] M☉ |
| Radius | 4.4[10] R☉ |
| Luminosity | 59[8] L☉ |
| Surface gravity (log g) | 3.6[10] cgs |
| Temperature | 7,800[10] K |
| Rotational velocity (v sin i) | 68.4[8] km/s |
| Ab | |
| Mass | 2.16[10] M☉ |
| Radius | 2.7[10] R☉ |
| Luminosity | 21[8] L☉ |
| Temperature | 7,800[8] K |
| Rotational velocity (v sin i) | 113[8] km/s |
| Age | 650[8] Myr |
| θ1 Tauri | |
| Mass | 2.67[11] M☉ |
| Radius | 10.55[11] R☉ |
| Luminosity | 71[11] L☉ |
| Surface gravity (log g) | 3.21[11] cgs |
| Temperature | 5,080[11] K |
| Metallicity [Fe/H] | +0.14[11] dex |
| Rotational velocity (v sin i) | 1.40[11] km/s |
| Age | 510[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 | |
| SIMBAD | θ1 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.
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Nomenclature
θ Tauri (Latinised to Theta Tauri) is the double star's Bayer designation;[citation needed] 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).[12]
In the mythology of the Maya peoples, Theta Tauri is known as Chamukuy, meaning a small bird in the Yucatec Maya language.[13] In 2016, the IAU organized a Working Group on Star Names (WGSN)[14] to catalog and standardize proper names for stars. The WGSN decided to attribute proper names to individual stars rather than entire multiple systems.[15] 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.[16]
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.[17] Consequently, the Chinese name for Theta² Tauri itself is 畢宿六 (Bì Xiù liù), "the Sixth Star of Net".[18]
Properties
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.[20] 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.[21]
References
- ^ a b c d van Leeuwen, F. (November 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.
- ^ 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. Originally Published in: 2009yCat....102025S. 1: B/gcvs. Bibcode:2009yCat....102025S.
- ^ 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. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
- ^ Morgan, W. W.; Abt, Helmut A.; Tapscott, J. W. (1978). Revised MK Spectral Atlas for stars earlier than the sun. Bibcode:1978rmsa.book.....M.
- ^ 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.
- ^ Böhm-Vitense, Erika; et al. (December 2000). "Ultraviolet Emission Lines in BA and Non-BA Giants". The Astrophysical Journal. 545 (2): 992–999. Bibcode:2000ApJ...545..992B. doi:10.1086/317850.
- ^ 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 e f g h Torres, K. B. V.; Lampens, P.; Frémat, Y.; Hensberge, H.; Lebreton, Y.; Škoda, P.; Guenther, E.; Schwope, A.; Heber, U. (2011). "Spectra disentangling applied to the Hyades binary θ2 Tauri AB: New orbit, orbital parallax and component properties". Astronomy and Astrophysics. 525: A50. arXiv:1010.5643. Bibcode:2011A&A...525A..50T. doi:10.1051/0004-6361/201015166. S2CID 55408682.
- ^ 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. Bibcode:2007A&A...473..829M. doi:10.1051/0004-6361:20078007.
- ^ a b c d e f Liakos, Alexios; Niarchos, Panagiotis (2017). "Catalogue and properties of δ Scuti stars in binaries". Monthly Notices of the Royal Astronomical Society. 465 (1): 1181. arXiv:1611.00200. Bibcode:2017MNRAS.465.1181L. doi:10.1093/mnras/stw2756.
- ^ a b c d e f g h Jofré, E.; Petrucci, R.; Saffe, C.; Saker, L.; de la Villarmois, E. Artur; Chavero, C.; Gómez, M.; Mauas, P. J. D.; Heber, U. (2015). "Stellar parameters and chemical abundances of 223 evolved stars with and without planets". Astronomy and Astrophysics. 574: A50. arXiv:1410.6422. Bibcode:2015A&A...574A..50J. doi:10.1051/0004-6361/201424474. S2CID 53666931.
- ^ 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].
- ^ 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.
- ^ "IAU Working Group on Star Names (WGSN)". Retrieved 22 May 2016.
- ^ "WG Triennial Report (2015-2018) - Star Names" (PDF). p. 5. Retrieved 2018-07-14.
- ^ "Naming Stars". IAU.org. Retrieved 16 December 2017.
- ^ 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.
- ^ (in Chinese) 香港太空館 - 研究資源 - 亮星中英對照表 Archived 2008-10-25 at the Wayback Machine, Hong Kong Space Museum. Accessed on line November 23, 2010.
- ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
- ^ 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. Bibcode:1997A&AS..122..131S. doi:10.1051/aas:1997329.
- ^ 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. Bibcode:1997ApJ...485..167T. doi:10.1086/304422.
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This page was last edited on 20 August 2023, at 14:15