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Pi Sculptoris

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Star in the constellation Sculptor
Pi Sculptoris
Location of π Sculptoris (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Sculptor
Right ascension 01 42 08.62230
Declination −32° 19′ 37.2862″
Apparent magnitude (V) 5.25
Characteristics
Evolutionary stage horizontal branch
Spectral type K1II/III
U−B color index +0.79
B−V color index +1.05
Astrometry
Radial velocity (Rv)+13.83±0.15 km/s
Proper motion (μ) RA: −76.714 mas/yr
Dec.: +4.521 mas/yr
Parallax (π)15.0534 ± 0.1667 mas
Distance217 ± 2 ly
(66.4 ± 0.7 pc)
Absolute magnitude (MV)1.16
Details
Mass1.52 M☉
Radius9.28+0.30
−2.31 R☉
Luminosity41.173±0.53 L☉
Surface gravity (log g)2.69 cgs
Temperature4,800+737
−75 K
Metallicity −0.22 dex
Rotational velocity (v sin i)< 1.6 km/s
Other designations
π Scl, CPD−32°4292, FK5 1048, GC 2085, HD 10537, HIP 7955, HR 497, SAO 193263, GSC 07003-02207
Database references
SIMBADdata

π Sculptoris, Latinized as Pi Sculptoris, is candidate astrometric binary star system in the southern constellation Sculptor, positioned near the eastern constellation border with Fornax. It has an orange hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.25. Based upon parallax measurements, the system is located at a distance of 66 light years from the Sun, and is drifting further away with a radial velocity of +14 km/s.

The visible component is an aging giant/bright giant star with a stellar classification of K1II/III. It is a red clump giant, which indicates it is on the horizontal branch and is generating energy through core helium fusion. The star has 1.5 times the mass of the Sun and 9.3 times the Sun's radius. It is radiating 41 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,800 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. ^ 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. Vizier catalog entry
  3. ^ Liu, Y. J.; et al. (2007). "The abundances of nearby red clump giants". Monthly Notices of the Royal Astronomical Society. 382 (2): 553. Bibcode:2007MNRAS.382..553L. doi:10.1111/j.1365-2966.2007.11852.x.
  4. ^ Houk, N. (1982). Michigan Catalogue of Two-dimensional Spectral Types for the HD stars. Declinations -40_ƒ0 to -26_ƒ0. Vol. 3. Bibcode:1982mcts.book.....H.
  5. ^ Mermilliod, J. C. (2006). "Homogeneous Means in the UBV System". VizieR On-line Data Catalog: II/168. Originally Published in: Institut d'Astronomie. 2168. Bibcode:2006yCat.2168....0M.Vizier catalog entry
  6. De Medeiros, J. R.; et al. (2014). "A catalog of rotational and radial velocities for evolved stars". Astronomy & Astrophysics. 561: A126. arXiv:1312.3474. Bibcode:2014A&A...561A.126D. doi:10.1051/0004-6361/201220762. S2CID 54046583. Vizier catalog entry
  7. "pi Scl". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-13.
  8. 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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