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Tau Sculptoris

From Wikipedia, the free encyclopedia
Star in the constellation Sculptor
Tau Sculptoris
Observation data
EpochJ2000.0      EquinoxJ2000.0 (ICRS)
ConstellationSculptor
Right ascension01h 36m 08.50799s[1]
Declination−29° 54′ 26.3540″[1]
Apparent magnitude (V)+5.69[2](6.06 + 7.35)[3]
Characteristics
Spectral typeF2 V[4]
B−Vcolor 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 mas[1]
Distance230 ± 10 ly
(69 ± 4 pc)
Absolute magnitude (MV)2.04 + 3.02[6]
Orbit[6]
Period (P)1503.58±35.32yr
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°
Periastronepoch (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 abinary star[6] system in the southernconstellation ofSculptor, about 8° to the east-southeast ofAlpha Sculptoris.[12] It is faintly visible to the naked eye with a combinedapparent visual magnitude of +5.69.[2] Based upon an annualparallax shift of 14.42 mas as seen from Earth,[1] it is located around 230 light years from theSun.

The binary nature of this system was discovered by English astronomerJohn 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 asemimajor axis of 3.2 arc seconds and aneccentricity of 0.6.[6] The primary member, component A, is a yellow-white huedF-type main sequence star with anapparent magnitude of +6.06[3] and astellar classification of F2 V.[4] The companion, component B, is a magnitude 7.35 star.[3]

References

[edit]
  1. ^abcdefvan 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.
  2. ^abcJohnson, 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. ^abcEggleton, 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,arXiv:0806.2878,Bibcode:2008MNRAS.389..869E,doi:10.1111/j.1365-2966.2008.13596.x,S2CID 14878976.
  4. ^abHouk, Nancy (1979),Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 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,arXiv:1208.3048,Bibcode:2012A&A...546A..61D,doi:10.1051/0004-6361/201219219,S2CID 59451347, A61.
  6. ^abcdeCvetkovic, Z.; Novakovic, B. (December 2006), "Orbits For Sixteen Binaries",Serbian Astronomical Journal,173 (173):73–82,Bibcode:2006SerAJ.173...73C,doi:10.2298/SAJ0673073C.
  7. ^abcdDavid, 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,arXiv:1501.03154,Bibcode:2015ApJ...804..146D,doi:10.1088/0004-637X/804/2/146,S2CID 33401607.
  8. ^abHardegree-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.arXiv:2304.12490.Bibcode:2023AJ....165..267H.doi:10.3847/1538-3881/acd1ec.
  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,arXiv:1103.4651,Bibcode:2011A&A...530A.138C,doi:10.1051/0004-6361/201016276,S2CID 56118016.
  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,arXiv:1204.2459,Bibcode:2012A&A...542A.116A,doi:10.1051/0004-6361/201118724,S2CID 53666672.
  11. ^"tau Scl",SIMBAD,Centre de données astronomiques de Strasbourg, retrieved2017-04-11.
  12. ^O'Meara, Steve (2007),Herschel 400 Observing Guide,Cambridge University Press, p. 302,ISBN 978-0521858939.
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