Zeta Crucis
  | |
| Observation data Epoch J2000 Equinox ICRS | |
|---|---|
| Constellation | Crux[1] |
| Right ascension | 12h 18m 26.24075s[2] |
| Declination | −64° 00′ 11.1073″[2] |
| Apparent magnitude (V) | 4.04[3] |
| Characteristics | |
| Evolutionary stage | main sequence[2] |
| Spectral type | B2.5V[4] |
| U−B color index | −0.68[3] |
| B−V color index | −0.17[3] |
| Astrometry | |
| Radial velocity (Rv) | +15.8[5] km/s |
| Proper motion (μ) | RA: −37.431[2] mas/yr Dec.: −6.576[2] mas/yr |
| Parallax (π) | 9.2402±0.1928 mas[2] |
| Distance | 353 ± 7 ly (108 ± 2 pc) |
| Absolute magnitude (MV) | −1.13[1] |
| Details | |
| Mass | 6.4±0.1[6] M☉ |
| Radius | 3.7[2] R☉ |
| Luminosity | 737[1] L☉ |
| Surface gravity (log g) | 3.99[2] cgs |
| Temperature | 18,155[7] K |
| Rotational velocity (v sin i) | 115[8] km/s |
| Age | 19.8[9] Myr |
| Other designations | |
| ζ Cru, CPD−63°2235, HD 106983, HIP 60009, HR 4679, SAO 251841[10] | |
| Database references | |
| SIMBAD | data |
Zeta Crucis is a binary star system in the southern constellation of Crux. Its name is a Bayer designation that is Latinized from ζ Crucis and abbreviated ζ Cru or ζ Cru. This system is visible to the naked eye as a point of light with an apparent visual magnitude of 4.06m. Based on parallax measurements, ζ Crucis is located at a distance of about 353 light-years (108 pc) from the Sun. It is a member of the Lower Centaurus–Crux subgroup of the Scorpius–Centaurus association.[11]
This is a double-lined spectroscopic binary star system.[12] The spectrum matches a B-type main-sequence star with a stellar classification of B2.5 V. It displays pulsational behavior matching a slowly pulsating B-type star and Beta Cephei variable.[13] There is a faint visual companion with an apparent magnitude of 12.49.[14]
A K-type companion star has an angular separation of 0.15″. This corresponds to a projected separation of about 20 au that would yield an orbital period of around 20 years. A common proper motion companion of type M2 is at a separation of around 11′. This would correspond to a projected separation of 60,000 au. It is about 1.5 magnitudes brighter than expected for its temperature, so it is most likely a pre-main-sequence star.[15]
References
- 1 2 3 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. XHIP record for this object at VizieR.
- 1 2 3 4 5 6 7 8 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 Johnson, H. L.; et al. (1966). "UBVRIJKL photometry of the bright stars". Communications of the Lunar and Planetary Laboratory. 4 (99): 99. Bibcode:1966CoLPL...4...99J.
- ↑ Hiltner, W. A.; et al. (July 1969). "MK Spectral Types for Bright Southern OB Stars". Astrophysical Journal. 157: 313–326. Bibcode:1969ApJ...157..313H. doi:10.1086/150069.
- ↑ Evans, D. S. (June 20–24, 1966). "The Revision of the General Catalogue of Radial Velocities". In Batten, Alan Henry; Heard, John Frederick (eds.). Determination of Radial Velocities and their Applications, Proceedings from IAU Symposium no. 30. University of Toronto: International Astronomical Union. Bibcode:1967IAUS...30...57E.
- ↑ Tetzlaff, N.; et al. (January 2011), "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun", Monthly Notices of the Royal Astronomical Society, 410 (1): 190–200, arXiv:1007.4883, Bibcode:2011MNRAS.410..190T, doi:10.1111/j.1365-2966.2010.17434.x, S2CID 118629873.
- ↑ Gerbaldi, M.; et al. (November 2001). "Binary systems with post-T Tauri secondaries". Astronomy and Astrophysics. 379: 162–184. Bibcode:2001A&A...379..162G. doi:10.1051/0004-6361:20011298.
- ↑ Bernacca, P. L.; Perinotto, M. (1970). "A catalogue of stellar rotational velocities". Contributi Osservatorio Astronomico di Padova in Asiago. 239 (1): 1. Bibcode:1970CoAsi.239....1B.
- ↑ Gratton, R.; et al. (2023). "Multiples among B stars in the Scorpius-Centaurus association". Astronomy and Astrophysics. 678: A93. arXiv:2308.09962. Bibcode:2023A&A...678A..93G. doi:10.1051/0004-6361/202346806.
- ↑ "zet Cru". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2009-09-10.
- ↑ Chen, Christine H.; et al. (September 2012), "A Spitzer MIPS Study of 2.5–2.0 M☉ Stars in Scorpius–Centaurus", The Astrophysical Journal, 756 (2): 24, arXiv:1207.3415, Bibcode:2012ApJ...756..133C, doi:10.1088/0004-637X/756/2/133, S2CID 119278056, 133.
- ↑ Chini, R.; et al. (2012), "A spectroscopic survey on the multiplicity of high-mass stars", Monthly Notices of the Royal Astronomical Society, 424 (3): 1925, arXiv:1205.5238, Bibcode:2012MNRAS.424.1925C, doi:10.1111/j.1365-2966.2012.21317.x, S2CID 119120749.
- ↑ Balona, L. A.; Ozuyar, D. (2020). "Pulsation among TESS A and B stars and the Maia variables". Monthly Notices of the Royal Astronomical Society. 493 (4): 5871. arXiv:2001.04497. Bibcode:2020MNRAS.493.5871B. doi:10.1093/mnras/staa670.
- ↑ Gahm, G. F.; et al. (January 1983). "A study of visual double stars with early type primaries. I - Spectroscopic results". Astronomy and Astrophysics Supplement Series. 51: 143–159. Bibcode:1983A&AS...51..143G.
- ↑ Gratton, R.; et al. (October 2023). "Multiples among B stars in the Scorpius-Centaurus association". Astronomy & Astrophysics. 678. id. A93. arXiv:2308.09962. Bibcode:2023A&A...678A..93G. doi:10.1051/0004-6361/202346806.
