Astronomy:Zeta Gruis
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Short description: Star in the constellation Grus
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Grus[1] |
| Right ascension | 23h 00m 52.79777s[2] |
| Declination | −52° 45′ 14.8705″[2] |
| Apparent magnitude (V) | 4.12[3] |
| Characteristics | |
| Spectral type | K1 III Fe−1.2 CN−0.5[4] |
| U−B color index | +0.722[3] |
| B−V color index | +0.967[3] |
| Astrometry | |
| Radial velocity (Rv) | −1.1±2.7[5] km/s |
| Proper motion (μ) | RA: −57.911[2] mas/yr Dec.: −13.371[2] mas/yr |
| Parallax (π) | 24.5452 ± 0.5124[2] mas |
| Distance | 133 ± 3 ly (40.7 ± 0.9 pc) |
| Absolute magnitude (MV) | +1.49[1] |
| Details[6] | |
| Mass | 1.44±0.06 M☉ |
| Radius | 8.83±0.21 R☉ |
| Luminosity | 39.4±1.7 L☉ |
| Surface gravity (log g) | 2.759±0.077 cgs |
| Temperature | 4,865±22 K |
| Metallicity [Fe/H] | −0.308±0.018 dex |
| Rotational velocity (v sin i) | <1.3[7] km/s |
| Other designations | |
| Database references | |
| SIMBAD | data |
Zeta Gruis, Latinised from ζ Gruis, is a solitary[9] star in the southern constellation of Grus. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.12.[3] Based upon an annual parallax shift of 24.5 mas as seen from the Earth,[2] the system is located about 133 light-years from the Sun.
This is an evolved K-type giant star with a stellar classification of K1 III Fe−1.2 CN−0.5,[4] where the suffix notation indicates underabundances of iron and cyanogen in the spectrum. Having exhausted the supply of hydrogen at its core, the star has expanded and cooled; at present it has 9 times the girth of the Sun. The star is radiating 39 times the luminosity of the Sun from its swollen photosphere at an effective temperature of 4,865 K.[6]
References
- ↑ 1.0 1.1 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A XHIP record for this object at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 Jennens, P. A.; Helfer, H. L. (September 1975), "A new photometric metal abundance and luminosity calibration for field G and K giants", Monthly Notices of the Royal Astronomical Society 172 (3): 667–679, doi:10.1093/mnras/172.3.667, Bibcode: 1975MNRAS.172..667J.
- ↑ 4.0 4.1 Gray, R. O. et al. (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): 161–70, doi:10.1086/504637, Bibcode: 2006AJ....132..161G.
- ↑ Gontcharov, G. A. (November 2006), "Pulkovo Compilation of Radial Velocities for 35495 Hipparcos stars in a common system", Astronomy Letters 32 (11): 759–771, doi:10.1134/S1063773706110065, Bibcode: 2006AstL...32..759G.
- ↑ 6.0 6.1 Ottoni, G.; Udry, S.; Ségransan, D.; Buldgen, G.; Lovis, C.; Eggenberger, P.; Pezzotti, C.; Adibekyan, V. et al. (2022). "CORALIE radial-velocity search for companions around evolved stars (CASCADES). I. Sample definition and first results: Three new planets orbiting giant stars". Astronomy and Astrophysics 657: A87. doi:10.1051/0004-6361/202040078. Bibcode: 2022A&A...657A..87O.
- ↑ De Medeiros, J. R.; Alves, S.; Udry, S.; Andersen, J.; Nordström, B.; Mayor, M. (2014). "A catalog of rotational and radial velocities for evolved stars. V. Southern stars". Astronomy and Astrophysics 561: A126. doi:10.1051/0004-6361/201220762. Bibcode: 2014A&A...561A.126D.
- ↑ "zet Gru". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=zet+Gru.
- ↑ 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.
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