Zeta Crateris
  | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Crater |
| Right ascension | 11h 44m 45.776s[1] |
| Declination | −18° 21′ 02.435″[1] |
| Apparent magnitude (V) | 4.740[2] (4.95 + 7.84)[3] |
| Characteristics | |
| Evolutionary stage | red clump[4] |
| Spectral type | G8 III[5] |
| U−B color index | +0.724[2] |
| B−V color index | +0.961[2] |
| Variable type | Constant[6] |
| Astrometry | |
| Radial velocity (Rv) | −4.10±0.33[7] km/s |
| Proper motion (μ) | RA: +27.298 mas/yr[1] Dec.: −24.644 mas/yr[1] |
| Parallax (π) | 9.5113±0.2042 mas[1] |
| Distance | 343 ± 7 ly (105 ± 2 pc) |
| Absolute magnitude (MV) | −0.66[8] |
| Details | |
| Mass | 3.4±0.1[1] M☉ |
| Radius | 16.8±0.5[1] R☉ |
| Luminosity | 150±6[1] L☉ |
| Surface gravity (log g) | 2.50±0.01[1] cgs |
| Temperature | 5,032±8[1] K |
| Metallicity [Fe/H] | −0.11[9] dex |
| Age | 271±34[8] Myr |
| Other designations | |
| ζ Crt, 27 Crateris, BD−17°3460, FK5 1301, HD 102070, HIP 57283, HR 4514, SAO 156869, WDS J11448-1821AB[10] | |
| Database references | |
| SIMBAD | data |
Zeta Crateris is a binary star[3] system in the southern constellation of Crater, the cup. Its name is a Bayer designation that is Latinized from ζ Crateris and abbreviated Zeta Crt or ζ Crt. The system is located about half-way between the stars Epsilon Corvi to the southeast and Delta Crateris to the northwest, which marks the lower left corner of the rim of the cup.
Zeta Crateris is a photometrically constant[6] system that is visible to the naked eye with an apparent visual magnitude of 4.740.[2] With an annual parallax shift of 9.24 mas as viewed from Earth,[1] Zeta Crateris is located approximately 343 light-years (105 pc) from the Sun. At that distance, the visual magnitude of the system is diminished by an extinction factor of 0.21 due to interstellar dust.[8]
The two components of this system had an angular separation of 0.20 arc seconds along a position angle of 22°, as of 1991.[11] The primary, component A, is a magnitude 4.95 evolved giant star with a stellar classification of G8 III.[5] It is a red clump star that is generating energy through the fusion of helium at its core.[4] With 3.4 times the Sun's mass, Zeta Crateris has expanded to 16.8 times the radius of the Sun and shines with 150 times the Sun's luminosity. This energy is being radiated into outer space from the outer envelope at an effective temperature of 5,032 K.[1]
The secondary, component B, is a magnitude 7.84 star.[11] Zeta Crateris is a confirmed member of the Sirius supercluster[12] and is a candidate member of the Ursa Major Moving Group, a collection of stars that share a similar motion through space and may have at one time been members of the same open cluster.[13]
References
- 1 2 3 4 5 6 7 8 9 10 11 12 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.
- 1 2 3 4 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, Bibcode:1975MNRAS.172..667J, doi:10.1093/mnras/172.3.667.
- 1 2 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.
- 1 2 Alves, David R. (August 2000), "K-Bad Calibration of the Red Clump Luminosity", The Astrophysical Journal, 539 (2): 732–741, arXiv:astro-ph/0003329, Bibcode:2000ApJ...539..732A, doi:10.1086/309278, S2CID 16673121.
- 1 2 Houk, Nancy; Smith-Moore, M. (1978), Michigan catalogue of two-dimensional spectral types for the HD stars, vol. 4, Ann Arbor: Dept. of Astronomy, University of Michigan, Bibcode:1988mcts.book.....H.
- 1 2 Choi, Hyung-Jin; et al. (August 1995), "A Study of Variability in a Sample of G and K Giants", Publications of the Astronomical Society of the Pacific, 107: 744, Bibcode:1995PASP..107..744C, doi:10.1086/133617.
- ↑ 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.
- 1 2 3 Takeda, Yoichi; et al. (August 2008), "Stellar Parameters and Elemental Abundances of Late-G Giants", Publications of the Astronomical Society of Japan, 60 (4): 781–802, arXiv:0805.2434, Bibcode:2008PASJ...60..781T, doi:10.1093/pasj/60.4.781, S2CID 16258166.
- ↑ Soubiran, C.; et al. (July 1, 2022), "Assessment of [Fe/H] determinations for FGK stars in spectroscopic surveys", Astronomy and Astrophysics, 663: A4, arXiv:2112.07545, Bibcode:2022A&A...663A...4S, doi:10.1051/0004-6361/202142409, ISSN 0004-6361.
- ↑ "* zet Crt", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2017-03-01
- 1 2 Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466–3471, Bibcode:2001AJ....122.3466M, doi:10.1086/323920, retrieved 2015-07-22
- ↑ Eggen, Olin J. (August 1998), "The Sirius Supercluster and Missing Mass near the Sun", The Astronomical Journal, 116 (2): 782–788, Bibcode:1998AJ....116..782E, doi:10.1086/300465.
- ↑ King, Jeremy R.; et al. (April 2003), "Stellar Kinematic Groups. II. A Reexamination of the Membership, Activity, and Age of the Ursa Major Group", The Astronomical Journal, 125 (4): 1980–2017, Bibcode:2003AJ....125.1980K, doi:10.1086/368241.
