Astronomy:67 Cancri
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Cancer |
| Right ascension | 09h 01m 48.83393s[1] |
| Declination | +27° 54′ 09.3505″[1] |
| Apparent magnitude (V) | 6.07[2] (6.08 + 9.22)[3] |
| Characteristics | |
| Evolutionary stage | main sequence |
| Spectral type | A8 Vn[4] |
| B−V color index | 0.243±0.008[2] |
| Astrometry | |
| Radial velocity (Rv) | +12.0±4.3[5] km/s |
| Proper motion (μ) | RA: −57.037[1] mas/yr Dec.: −80.127[1] mas/yr |
| Parallax (π) | 16.7647 ± 0.1550[1] mas |
| Distance | 195 ± 2 ly (59.6 ± 0.6 pc) |
| Absolute magnitude (MV) | 2.25[2] |
| Details | |
| 67 Cnc A | |
| Mass | 1.89[6] M☉ |
| Radius | 1.90+0.07 −0.14[1] R☉ |
| Luminosity | 10.465+0.111 −0.112[1] L☉ |
| Surface gravity (log g) | 4.35[6] cgs |
| Temperature | 7,982±271[6] K |
| Rotational velocity (v sin i) | 105[7] km/s |
| Age | 867[6] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
67 Cancri is a wide binary star[9] system in the zodiac constellation of Cancer, located 195[1] 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.[2] The binary nature of this system was discovered by James South and John Herschel.[3] As of 2007, the two components have an angular separation of 103.9″, corresponding to a projected separation of 6,100 astronomical unit|AU.[9] They are moving further from the Earth with a heliocentric radial velocity of +12 km/s.[5]
The primary, designated component A, is an A-type main-sequence star with a stellar classification of A8 Vn.[4] The 'n' notation indicates "nebulous" lines due to rapid rotation. It is a shell star,[10] 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.[11] Uesugi and Fukuda (1970) gave a projected rotational velocity estimate of 105[7] km/s for the star, although Abt et al. (1997) suggested it could be as high as 205 km/s.[11]
67 Cancri A is about 867[6] million years old with 1.89[6] times the mass of the Sun and 1.90[1] times the Sun's radius. It is radiating 10.5[1] times the Sun's luminosity from its photosphere at an effective temperature of 7,982 K.[6]
References
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 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.
- ↑ 2.0 2.1 2.2 2.3 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters 38 (5): 331, doi:10.1134/S1063773712050015, Bibcode: 2012AstL...38..331A.
- ↑ 3.0 3.1 Mason, B. D. et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal 122 (6): 3466, doi:10.1086/323920, Bibcode: 2001AJ....122.3466M.
- ↑ 4.0 4.1 Cowley, A. et al. (April 1969), "A study of the bright A stars. I. A catalogue of spectral classifications", Astronomical Journal 74: 375–406, doi:10.1086/110819, Bibcode: 1969AJ.....74..375C.
- ↑ 5.0 5.1 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, doi:10.1051/0004-6361/201219219, A61, Bibcode: 2012A&A...546A..61D.
- ↑ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 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, doi:10.1088/0004-637X/804/2/146, Bibcode: 2015ApJ...804..146D.
- ↑ 7.0 7.1 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. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=67+Cnc.
- ↑ 9.0 9.1 Trilling, D. E. et al. (April 2007), "Debris disks in main-sequence binary systems", The Astrophysical Journal 658 (2): 1264–1288, doi:10.1086/511668, Bibcode: 2007ApJ...658.1289T.
- ↑ Hauck, B.; Jaschek, C. (2000), "A-shell stars in the Geneva system", Astronomy and Astrophysics 354: 157, Bibcode: 2000A&A...354..157H.
- ↑ 11.0 11.1 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, doi:10.1086/304603, Bibcode: 1997ApJ...487..365A.
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