Astronomy:Tau Sculptoris

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Short description: Star in the constellation Sculptor
Tau Sculptoris
Observation data
Equinox J2000.0]] (ICRS)
Constellation Sculptor
Right ascension  01h 36m 08.50799s[1]
Declination −29° 54′ 26.3540″[1]
Apparent magnitude (V) +5.69[2] (6.06 + 7.35)[3]
Characteristics
Spectral type F2 V[4]
B−V color index +0.33[2]
Astrometry
Radial velocity (Rv)+3.00±4.50[5] km/s
Proper motion (μ) RA: +117.37[1] mas/yr
Dec.: +46.72[1] mas/yr
Parallax (π)14.42 ± 0.81[1] mas
Distance230 ± 10 ly
(69 ± 4 pc)
Absolute magnitude (MV)2.04 + 3.02[6]
Orbit[6]
Period (P)1503.58±35.32 yr
Semi-major axis (a)3.155±0.132″
Eccentricity (e)0.604±0.019
Inclination (i)55.6±0.8°
Longitude of the node (Ω)69.6±0.8°
Periastron epoch (T)2039.79±33.80
Argument of periastron (ω)
(secondary)		140.2±2.8°
Details
τ Scl A
Mass1.56[7] M☉
Radius2.3[8] R☉
Luminosity11.1[8] L☉
Surface gravity (log g)3.96±0.14[7] cgs
Temperature7,155±243[7] K
Metallicity [Fe/H]−0.12[9] dex
Rotational velocity (v sin i)73.8±7.8[10] km/s
Age1.284[7] Gyr
τ Scl B
Mass1.37[6] M☉
Other designations
τ Scl, CD−30°540, HD 9906, HIP 7463, HR 462, SAO 193201, WDS J01361-2954[11]
Database references
SIMBADdata

Tau Sculptoris (τ Scl, τ Sculptoris) is a binary star[6] system in the southern constellation of Sculptor, about 8° to the east-southeast of Alpha Sculptoris.[12] It is faintly visible to the naked eye with a combined apparent visual magnitude of +5.69.[2] Based upon an annual parallax shift of 14.42 mas as seen from Earth,[1] it is located around 230 light years from the Sun.

The binary nature of this system was discovered by English astronomer John Herschel in 1835. The current orbital elements are based upon a fraction of a single orbit, as the estimated orbital period is around 1,503 years. The system has a semimajor axis of 3.2 arc seconds and an eccentricity of 0.6.[6] The primary member, component A, is a yellow-white hued F-type main sequence star with an apparent magnitude of +6.06[3] and a stellar classification of F2 V.[4] The companion, component B, is a magnitude 7.35 star.[3]

The designation Tau Sculptoris hasn’t always been allocated to this star. It was given this designation by Lacaille when he created Sculptor. When Bode created his own constellation Machina Electrica, he took about half of Sculptor and parts of Fornax, including this star, which he designated Iota Machinae Electricae. Bode used Tau Sculptoris for HD 224914 instead, which is currently in Phoenix. After Machina Electrica was deemed obsolete by the IAU, the stars were returned to their original constellations.[13]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 van Leeuwen, F. (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 Johnson, H. L. et al. (1966), "UBVRIJKL photometry of the bright stars", Communications of the Lunar and Planetary Laboratory 4 (99): 99, Bibcode: 1966CoLPL...4...99J. 
  3. ↑ 3.0 3.1 3.2 Eggleton, P. P.; Tokovinin, A. A. (September 2008), "A catalogue of multiplicity among bright stellar systems", Monthly Notices of the Royal Astronomical Society 389 (2): 869–879, doi:10.1111/j.1365-2966.2008.13596.x, Bibcode: 2008MNRAS.389..869E. 
  4. ↑ 4.0 4.1 Houk, Nancy (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, 3, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode: 1982mcts.book.....H. 
  5. ↑ de Bruijne, J. H. J.; Eilers, A.-C. (October 2012), "Radial velocities for the HIPPARCOS-Gaia Hundred-Thousand-Proper-Motion project", Astronomy & Astrophysics 546: 14, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D. 
  6. ↑ 6.0 6.1 6.2 6.3 6.4 Cvetkovic, Z.; Novakovic, B. (December 2006), "Orbits For Sixteen Binaries", Serbian Astronomical Journal 173 (173): 73–82, doi:10.2298/SAJ0673073C, Bibcode: 2006SerAJ.173...73C. 
  7. ↑ 7.0 7.1 7.2 7.3 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. 
  8. ↑ 8.0 8.1 Hardegree-Ullman, Kevin K.; Apai, Dániel; Bergsten, Galen J.; Pascucci, Ilaria; López-Morales, Mercedes (2023). "Bioverse: A Comprehensive Assessment of the Capabilities of Extremely Large Telescopes to Probe Earth-like O2 Levels in Nearby Transiting Habitable-zone Exoplanets". The Astronomical Journal 165 (6): 267. doi:10.3847/1538-3881/acd1ec. Bibcode: 2023AJ....165..267H. 
  9. ↑ Casagrande, L. et al. (2011), "New constraints on the chemical evolution of the solar neighbourhood and Galactic disc(s). Improved astrophysical parameters for the Geneva-Copenhagen Survey", Astronomy & Astrophysics 530 (A138): 21, doi:10.1051/0004-6361/201016276, Bibcode: 2011A&A...530A.138C. 
  10. ↑ Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics 542: A116, doi:10.1051/0004-6361/201118724, Bibcode: 2012A&A...542A.116A. 
  11. ↑ "tau Scl". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=tau+Scl. 
  12. ↑ O'Meara, Steve (2007), Herschel 400 Observing Guide, Cambridge University Press, p. 302, ISBN 978-0521858939, https://books.google.com/books?id=Nyh9fAC_tpIC&pg=PA302. 
  13. ↑ Ian Ridpath. "Sculptor". http://www.ianridpath.com/startales/sculptor.html. 



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