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Theta Sculptoris

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Star in the constellation Sculptor
Theta Sculptoris
Location of θ Sculptoris (circled)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Sculptor
Right ascension 00 11 44.02079
Declination −35° 07′ 59.2320″
Apparent magnitude (V) +5.236±0.005
Characteristics
Evolutionary stage main sequence
Spectral type F5V
B−V color index 0.459±0.002
Astrometry
Radial velocity (Rv)−21.1±0.3 km/s
Proper motion (μ) RA: +171.529 mas/yr
Dec.: +126.670 mas/yr
Parallax (π)46.1936 ± 0.1565 mas
Distance70.6 ± 0.2 ly
(21.65 ± 0.07 pc)
Absolute magnitude (MV)3.52
Details
Mass1.25 M☉
Radius1.40±0.05 R☉
Luminosity3.09 L☉
Surface gravity (log g)4.25±0.10 cgs
Temperature6,395±80 K
Metallicity −0.07±0.07 dex
Rotational velocity (v sin i)1.0±1.0 km/s
Age1.6+2.4
−0.5 Gyr
Other designations
θ Scl, CD−35°4, FK5 6, GC 202, GJ 3013, HD 739, HIP 950, HR 35, SAO 192388, LTT 79, GSC 06995-01262
Database references
SIMBADdata

θ Sculptoris, Latinized as Theta Sculptoris, is a star in the southern constellation of Sculptor. This object is visible to the naked eye as a dim, yellow-white hued star with an apparent visual magnitude of +5.24. It is located 71 light years from the Sun based on parallax. The object is drifting closer with a radial velocity of −21 km/s, and may come to within 49 light-years in half a million years.

According to Fuhrmann and Chini (2015) this is an astrometric binary system, although Eggleton and Tokovinin (2008) deemed it to be a single star. The visible component is an ordinary F-type main-sequence star with a stellar classification of F5V. It is around 1.6 billion years old with 1.25 times the mass of the Sun and 1.40 times the Sun's radius. The star is radiating three times the luminosity of the Sun from its photosphere at an effective temperature of 6,395 K.

References

  1. ^ 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.
  2. ^ Fuhrmann, K.; Chini, R. (2012), "Multiplicity among F-type Stars", The Astrophysical Journal Supplement, 203 (2): 20, Bibcode:2012ApJS..203...30F, doi:10.1088/0067-0049/203/2/30, 30.
  3. ^ Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Bubar, E. J.; McGahee, C. E.; O'Donoghue, A. A.; Knox, E. R. (2006), "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc--The Southern Sample", The Astronomical Journal, 132 (1): 161–170, arXiv:astro-ph/0603770, Bibcode:2006AJ....132..161G, doi:10.1086/504637, S2CID 119476992.
  4. ^ Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv:1108.4971, Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID 119257644.
  5. "tet Scl". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-09-03.{{cite web}}: CS1 maint: postscript (link)
  6. Fuhrmann, K.; Chini, R. (August 2015), "Multiplicity among F-type stars. II", The Astrophysical Journal, 809 (1): 19, Bibcode:2015ApJ...809..107F, doi:10.1088/0004-637X/809/1/107, 107.
  7. 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, arXiv:0806.2878, Bibcode:2008MNRAS.389..869E, doi:10.1111/j.1365-2966.2008.13596.x, S2CID 14878976.
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