| Observation data Epoch J2000.0 Equinox J2000.0 | |
|---|---|
| Constellation | Cancer |
| Right ascension | 08h 20m 03.86070s[1] |
| Declination | +27° 13′ 03.7464″[1] |
| Apparent magnitude (V) | 5.14[2] |
| Characteristics | |
| Evolutionary stage | main sequence |
| Spectral type | F6V[3] |
| U−B color index | –0.06[2] |
| B−V color index | +0.47[2] |
| Astrometry | |
| Radial velocity (Rv) | +32.91±0.08[4] km/s |
| Proper motion (μ) | RA: –17.433[1] mas/yr Dec.: –377.614[1] mas/yr |
| Parallax (π) | 54.8640 ± 0.1728 mas[1] |
| Distance | 59.4 ± 0.2 ly (18.23 ± 0.06 pc) |
| Absolute magnitude (MV) | 3.85[5] |
| Details[3] | |
| Mass | 1.070 M☉ |
| Radius | 1.3870±0.0276 R☉ |
| Luminosity | 2.4378±0.0341 L☉ |
| Surface gravity (log g) | 4.35[5] cgs |
| Temperature | 6,130±58 K |
| Metallicity [Fe/H] | −0.26 dex |
| Rotational velocity (v sin i) | 4.2[5] km/s |
| Age | 5.8 Gyr |
| Other designations | |
| Database references | |
| SIMBAD | data |
Chi Cancri, Latinized from χ Cancri, is a candidate astrometric binary[7] star system in the northern zodiac constellation of Cancer. It has a yellow-white hue and is dimly visible to the naked eye with an apparent visual magnitude of 5.14.[2] The system is located at a distance of 59 light years from the Sun, based on parallax, and is drifting further away with a radial velocity of +33 km/s.[4] It is estimated to have made its closest approach some 274,000 years ago when it came to within 42 light-years.[8]
The visible component of this system is an F-type main-sequence star with a stellar classification of F6V,[3] where the luminosity class of 'V' indicates it is generating energy through core hydrogen fusion. The star is 5.8[3] billion years old and is spinning with a projected rotational velocity of just 4.2 km/s.[5] It has about the same mass as the Sun but 1.4 times the Sun's radius. Chi Cancri is radiating 2.4 times the luminosity of the Sun from its photosphere at an effective temperature of 6,130 K.[3] It displays an infrared excess in the 18μm wavelength band, suggesting a circumstellar disk of dusty debris is orbiting the star.[9]
References
- 1 2 3 4 5 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.
- 1 2 3 4 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.
- 1 2 3 4 5 Boyajian, Tabetha S.; et al. (July 2013), "Stellar Diameters and Temperatures. III. Main-sequence A, F, G, and K Stars: Additional High-precision Measurements and Empirical Relations", The Astrophysical Journal, 771 (1): 40, arXiv:1306.2974, Bibcode:2013ApJ...771...40B, doi:10.1088/0004-637X/771/1/40, S2CID 14911430.
- 1 2 Nidever, David L.; et al. (August 2002), "Radial Velocities for 889 Late-Type Stars", The Astrophysical Journal Supplement Series, 141 (2): 503–522, arXiv:astro-ph/0112477, Bibcode:2002ApJS..141..503N, doi:10.1086/340570, S2CID 51814894.
- 1 2 3 4 Paunzen, E.; et al. (July 2014), "Investigating the possible connection between λ Bootis stars and intermediate Population II type stars", Astronomy & Astrophysics, 567: 8, arXiv:1406.3936, Bibcode:2014A&A...567A..67P, doi:10.1051/0004-6361/201423817, S2CID 56332289, A67.
- ↑ "chi Cnc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2019-10-23.
{{cite web}}: CS1 maint: postscript (link) - ↑ 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.
- ↑ 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.
- ↑ Ishihara, Daisuke; et al. (May 2017), "Faint warm debris disks around nearby bright stars explored by AKARI and IRSF", Astronomy & Astrophysics, 601: 18, arXiv:1608.04480, Bibcode:2017A&A...601A..72I, doi:10.1051/0004-6361/201526215, S2CID 55234482, A72.
