| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Cancer |
| Right ascension | 09 01 48.83393 |
| Declination | +27° 54′ 09.3505″ |
| Apparent magnitude (V) | 6.07 (6.08 + 9.22) |
| Characteristics | |
| Evolutionary stage | main sequence |
| Spectral type | A8 Vn |
| B−V color index | 0.243±0.008 |
| Astrometry | |
| Radial velocity (Rv) | +12.0±4.3 km/s |
| Proper motion (μ) | RA: −57.037 mas/yr Dec.: −80.127 mas/yr |
| Parallax (π) | 16.7647 ± 0.1550 mas |
| Distance | 195 ± 2 ly (59.6 ± 0.6 pc) |
| Absolute magnitude (MV) | 2.25 |
| Details | |
| 67 Cnc A | |
| Mass | 1.89 M☉ |
| Radius | 1.90+0.07 −0.14 R☉ |
| Luminosity | 10.465+0.111 −0.112 L☉ |
| Surface gravity (log g) | 4.35 cgs |
| Temperature | 7,982±271 K |
| Rotational velocity (v sin i) | 105 km/s |
| Age | 867 Myr |
| Other designations | |
| 67 Cnc, BD+28°1674, HD 77190, HIP 44342, HR 3589, SAO 80585, WDS 09014+3215 | |
| Database references | |
| SIMBAD | data |
67 Cancri is a wide binary star system in the zodiac constellation of Cancer, located 195 light years away from the Sun. It is just visible to the naked eye as a faint, white-hued star with a combined apparent magnitude of 6.07. The binary nature of this system was discovered by James South and John Herschel. As of 2007, the two components have an angular separation of 103.9″, corresponding to a projected separation of 6,100 AU. They are moving further from the Earth with a heliocentric radial velocity of +12 km/s.
The primary, designated component A, is an A-type main-sequence star with a stellar classification of A8 Vn. The 'n' notation indicates "nebulous" lines due to rapid rotation. It is a shell star, with weak shell lines of singly-ionized titanium being detected in the near ultraviolet in 1970. These may have come from a sporadic mass loss event. Uesugi and Fukuda (1970) gave a projected rotational velocity estimate of 105 km/s for the star, although Abt et al. (1997) suggested it could be as high as 205 km/s.
67 Cancri A is about 867 million years old with 1.89 times the mass of the Sun and 1.90 times the Sun's radius. It is radiating 10.5 times the Sun's luminosity from its photosphere at an effective temperature of 7,982 K.
References
- ^ 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.
- ^ 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.
- ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode:2001AJ....122.3466M, doi:10.1086/323920.
- ^ Cowley, A.; et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal, 74: 375–406, Bibcode:1969AJ.....74..375C, doi:10.1086/110819.
- ^ 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.
- ^ David, Trevor J.; Hillenbrand, Lynne A. (2015), "The Ages of Early-Type Stars: Strömgren Photometric Methods Calibrated, Validated, Tested, and Applied to Hosts and Prospective Hosts of Directly Imaged Exoplanets", The Astrophysical Journal, 804 (2): 146, arXiv:1501.03154, Bibcode:2015ApJ...804..146D, doi:10.1088/0004-637X/804/2/146, S2CID 33401607.
- ^ Uesugi, Akira; Fukuda, Ichiro (1970), "Catalogue of rotational velocities of the stars", Contributions from the Institute of Astrophysics and Kwasan Observatory, University of Kyoto, Bibcode:1970crvs.book.....U.
- "67 Cnc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-03-09.
- ^ Trilling, D. E.; et al. (April 2007), "Debris disks in main-sequence binary systems", The Astrophysical Journal, 658 (2): 1264–1288, arXiv:astro-ph/0612029, Bibcode:2007ApJ...658.1289T, doi:10.1086/511668, S2CID 14867168.
- Hauck, B.; Jaschek, C. (2000), "A-shell stars in the Geneva system", Astronomy and Astrophysics, 354: 157, Bibcode:2000A&A...354..157H.
- ^ Abt, Helmut A.; et al. (September 1997), "Hot Inner Disks that Appear and Disappear Around Rapidly Rotating A-Type Dwarfs", The Astrophysical Journal, 487 (1): 365–369, Bibcode:1997ApJ...487..365A, doi:10.1086/304603.
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