Astronomy:Tau Herculis

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Short description: Variable star in the constellation Hercules
τ Herculis
Location of τ Herculis (circled in red)
Observation data
Equinox J2000.0]] (ICRS)
Constellation Hercules
Right ascension  16h 19m 44.43666s[1]
Declination +46° 18′ 48.1123″[1]
Apparent magnitude (V) 3.91[2] 3.83 to 3.86[3]
Characteristics
Evolutionary stage Main sequence[4]
Spectral type B5 IV[5]
U−B color index −0.569[2]
B−V color index −0.151±0.009[2]
Variable type SPB[3]
Astrometry
Radial velocity (Rv)−15.5±0.5[2] km/s
Proper motion (μ) RA: −13.33[1] mas/yr
Dec.: 38.48[1] mas/yr
Parallax (π)10.61 ± 0.11[1] mas
Distance307 ± 3 ly
(94.3 ± 1.0 pc)
Absolute magnitude (MV)−0.96[2]
Details
Mass4.01[6] M☉
Radius3.55±0.19 R☉[7]
3.80±0.25[8] R☉
Luminosity574[2] L☉
Surface gravity (log g)4.02±0.05[7] cgs
Temperature15,615±301[7] K
Metallicity [Fe/H]0.15[9] dex
Rotational velocity (v sin i)32[6] km/s
Age26[6] Myr
Other designations
Asuusiha, τ Her, 22 Her, BD+46°2169, FK5 608, GC 21987, HD 147394, HIP 79992, HR 6092, SAO 46028, CCDM J16197+4619A[10]
Database references
SIMBADdata

Tau Herculis, also named Asuusiha (Template:Lang-mnc),[11] is a variable star in the northern constellation of Hercules. It has a blue-white hue and is visible to the naked eye at night with an apparent visual magnitude that fluctuates around 3.91.[2] The star is located at a distance of approximately 307 light-years from the Sun based on parallax,[1] but it is drifting closer with a radial velocity of −16 km/s.[2]

Nomenclature

Tau Herculis, Latinized from τ Herculis and abbreviated Tau Her or τ Her, is the star's Bayer designation.

In Chinese astronomy, 七公 (Qī Gōng), meaning Seven Excellencies, refers to an asterism consisting of τ Herculis, 42 Herculis, φ Herculis, χ Herculis, ν1 Boötis, μ1 Boötis and δ Boötis.[12] Consequently, the Chinese name for τ Herculis itself is 七公二 (Qī Gōng èr, English: the Second Star of Seven Excellencies).[13] This star is also part of the Manchu constellation Asu Usiha (Template:Lang-mnc), representing a net used to hunt sables. The IAU Working Group on Star Names adopted the name Asuusiha for τ Herculis on 14 May 2026.[11]

Properties

A light curve for Tau Herculis, plotted from TESS data[14]

The stellar classification of Tau Herculis is B5 IV,[5] and it serves as a standard spectrum in the modern Morgan–Keenan (MK) classification.[15] It is estimated to be just 26 million years old with a relatively low projected rotational velocity of 32 km/s.[6] Slowly rotating B-type stars are often chemically peculiar, so the mostly normal spectra of this star suggests we may be viewing it from near pole-on.[16] The abundance of most heavier elements in this star are about 85% of those in the Sun.[17] The star has four times the mass of the Sun[6] and around 3.8[8] times the Sun's radius. On average, it is radiating 574[2] times the luminosity of the Sun from its photosphere at an effective temperature of 15,615 K.[7]

During the Hipparcos mission,[4] Tau Herculis was discovered to be a variable star of the slowly pulsating B-type. These are mid-B main sequence stars that vary with a period of about a day;[4] the brightness of Tau Herculis varies by 0.03 magnitude[3] over a period of 1.24970±0.00008 days. The radial velocity of the star varies at a different rate than the photometric period, with the object showing both radial and non-radial pulsation modes.[4][18]

Pole star

Small white disks representing the northern stars on a black background, overlaid by a circle showing the position of the north pole over time
The path of the north celestial pole among the stars due to the precession.

Tau Herculis is located within 1° of the precessional path traced across the celestial sphere by the Earth's North pole. It could have served the northern pole star around the year 7400 BCE, a phenomenon which is expected to reoccur in the year 18,400 due to precession.[16]

Preceded by Pole Star Succeeded by
Iota Herculis 18,400 AD Alpha Draconis

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics 474 (2): 653–664, doi:10.1051/0004-6361:20078357, Bibcode: 2007A&A...474..653V. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 2.8 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A. 
  3. ↑ 3.0 3.1 3.2 Samus', N. N et al. (2017), "General catalogue of variable stars: Version GCVS 5.1", Astronomy Reports 61 (1): 80, doi:10.1134/S1063772917010085, Bibcode: 2017ARep...61...80S. 
  4. ↑ 4.0 4.1 4.2 4.3 Masuda, Seiji; Hirata, Ryuko (April 2000), "Line-profile variation in tau Herculis", Astronomy and Astrophysics 356: 209–212, Bibcode: 2000A&A...356..209M. 
  5. ↑ 5.0 5.1 Morgan, W. W.; Keenan, P. C. (1973), "Spectral Classification", Annual Review of Astronomy and Astrophysics 11: 29, doi:10.1146/annurev.aa.11.090173.000333, Bibcode: 1973ARA&A..11...29M. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal 804 (2): 146, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D. 
  7. ↑ 7.0 7.1 7.2 7.3 Fitzpatrick, E. L.; Massa, D. (March 2005), "Determining the Physical Properties of the B Stars. II. Calibration of Synthetic Photometry", The Astronomical Journal 129 (3): 1642–1662, doi:10.1086/427855, Bibcode: 2005AJ....129.1642F. 
  8. ↑ 8.0 8.1 Gordon, Kathryn D. et al. (2019), "Angular Sizes, Radii, and Effective Temperatures of B-type Stars from Optical Interferometry with the CHARA Array", The Astrophysical Journal 873 (1): 91, doi:10.3847/1538-4357/ab04b2, Bibcode: 2019ApJ...873...91G. 
  9. ↑ Smith, K. C.; Dworetsky, M. M. (1993), "Elemental Abundances in Normal Late B-Stars and Hgmn-Stars from Co-Added IUE Spectra - Part One - Iron Peak Elements", Astronomy and Astrophysics 274 (2): 335, Bibcode: 1993A&A...274..335S 
  10. ↑ "* tau Her". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=%2A+tau+Her. 
  11. ↑ 11.0 11.1 "IAU Catalog of Star Names". https://exopla.net/star-names/modern-iau-star-names/. 
  12. ↑ (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.
  13. ↑ (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 6 月 26 日
  14. ↑ MAST: Barbara A. Mikulski Archive for Space Telescopes, Space Telescope Science Institute, https://mast.stsci.edu/portal/Mashup/Clients/Mast/Portal.html, retrieved 24 September 2022. 
  15. ↑ Garcia, B. (June 1989), "A list of MK standard stars", Bulletin d'Information du Centre de Donnees Stellaires 36: 27, Bibcode: 1989BICDS..36...27G. 
  16. ↑ 16.0 16.1 "TAU HER (Tau Herculis)", Stars (University of Illinois), http://stars.astro.illinois.edu/sow/tauher.html, retrieved 2018-04-27. 
  17. ↑ Adelman, Saul J. et al. (June 2001), "Elemental abundance analyses with DAO spectrograms. XXV. The superficially normal B and A stars alpha Draconis, tau Herculis, gamma Lyrae, and HR 7926", Astronomy and Astrophysics 371 (3): 1078–1083, doi:10.1051/0004-6361:20010408, Bibcode: 2001A&A...371.1078A 
  18. ↑ Briquet, M. et al. (April 2003), "Spectroscopic mode identification for the slowly pulsating B star HD 147394", Astronomy and Astrophysics 401: 281–288, doi:10.1051/0004-6361:20030086, Bibcode: 2003A&A...401..281B. 

Template:Pole star

Coordinates: Sky map 16h 19m 44.437s, +46° 18′ 48.12″



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