Zeta Volantis
  | |
| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Volans |
| Right ascension | 07h 41m 49.2590s[1] |
| Declination | −72° 36′ 21.957″[1] |
| Apparent magnitude (V) | 3.918±0.003 [2] |
| Characteristics | |
| Evolutionary stage | Giant star |
| Spectral type | K0 III[3] |
| B−V color index | 1.029±0.004[2] |
| Astrometry | |
| Radial velocity (Rv) | 48.5±0.14[1] km/s |
| Proper motion (μ) | RA: +36.179 mas/yr[1] Dec.: +14.816 mas/yr[1] |
| Parallax (π) | 22.4377 ± 0.0947 mas[1] |
| Distance | 145.4 ± 0.6 ly (44.6 ± 0.2 pc)[1] |
| Absolute magnitude (MV) | +0.75[4] |
| Details[2] | |
| Mass | 1.224±0.155 M☉ |
| Radius | 10.677±0.255 R☉ |
| Luminosity | 60[1] L☉ |
| Surface gravity (log g) | 2.82±0.09 cgs |
| Temperature | 4,788±37 K |
| Metallicity [Fe/H] | −0.17±0.03 dex |
| Age | 5.1±1.515 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Zeta Volantis, Latinized from ζ Volantis, is a binary star[6] system in the southern constellation of Volans. It has an apparent visual magnitude of 3.92,[2] which is bright enough to be seen with the naked eye. Based upon parallax measurements by the Gaia spacecraft, it is approximately 145 light-years (44.6 parsecs) from the Sun. The companion is a magnitude 9.7 star at an angular separation of 16.7″.[6] Based upon their motion through space, this system made its perihelion passage some 858,000 years ago when it came within 22 ly (6.6 pc) of the Sun.[7] It is currently moving away with a radial velocity of 48 km/s.[1]
The primary component is K-type giant star with a stellar classification of K0 III.[3] It has a derived luminosity of around 60 times that of the Sun,[1] 1.2 times the Sun's mass and is about 5.1 billion years old. At this age, it has expanded to 10.7 times the Sun's size.[2] The expanded outer envelope has an effective temperature of 4,788 K,[2] giving it the orange glow of a K-type star.[8]
References
[edit]- ^ a b c d e f g h i Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b c d e f Gomes da Silva, J.; Santos, N. C.; Adibekyan, V.; Sousa, S. G.; Campante, T. L.; Figueira, P.; Bossini, D.; Delgado-Mena, E.; Monteiro, M. J. P. F. G.; de Laverny, P.; Recio-Blanco, A.; Lovis, C. (2021-02-01). "Stellar chromospheric activity of 1674 FGK stars from the AMBRE-HARPS sample. I. A catalogue of homogeneous chromospheric activity". Astronomy and Astrophysics. 646: A77. arXiv:2012.10199. Bibcode:2021A&A...646A..77G. doi:10.1051/0004-6361/202039765. ISSN 0004-6361. Zeta Volantis' database entry at VizieR.
- ^ a b Houk, Nancy; Cowley, A. P. (1979), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 1, Ann Arbor, Michigan: Dept. of Astronomy, University of Michigan, Bibcode:1978mcts.book.....H.
- ^ 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.
- ^ "zet Vol -- High proper-motion Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg, retrieved 2016-09-05.
- ^ a b 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.
- ^ Bailer-Jones, C. A. L. (March 2015), "Close encounters of the stellar kind", Astronomy & Astrophysics, 575: 13, arXiv:1412.3648, Bibcode:2015A&A...575A..35B, doi:10.1051/0004-6361/201425221, S2CID 59039482, A35.
- ^ "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, archived from the original on 2013-12-03, retrieved 2012-01-16.
