14 Cancri

For other stars with this Bayer designation, see ψ Cancri.
14 Cancri
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Canis Major
Right ascension 08h 10m 27.18056 s[1]
Declination +25° 30′ 26.4061″[1]
Apparent magnitude (V) +5.73[2]
Characteristics
Spectral type G7 V[3]
U−B color index +0.43[2]
B−V color index +0.81[2]
Astrometry
Radial velocity (Rv)−44.48±0.09[4] km/s
Proper motion (μ) RA: −73.35[1] mas/yr
Dec.: −347.60[1] mas/yr
Parallax (π)24.18 ± 0.35 mas[1]
Distance135 ± 2 ly
(41.4 ± 0.6 pc)
Absolute magnitude (MV)+2.65[5]
Details[4]
Mass1.49±0.04 M☉
Radius3.20±0.11 R☉
Luminosity8 L☉
Surface gravity (log g)3.87±0.08 cgs
Temperature5,311±23 K
Metallicity [Fe/H]−0.12±0.06 dex
Rotational velocity (v sin i)0.98±0.42 km/s
Age2.39±0.14 Gyr
Other designations
ψ2 Cnc, 14 Cnc, BD+25°1865, FK5 2633, GC 11091, HD 67767, HIP 40023, HR 3191, SAO 79995, CCDM 08104+2530[6]
Database references
SIMBADdata

14 Cancri is a star in the northern zodiac constellation of Cancer. It can be referred to as ψ Cancri, very occasionally as ψ2 Cancri, to distinguish it from 13 Cancri which is sometimes called ψ1 Cancri.[7] It is just barely visible to the naked eye, having an apparent visual magnitude of +5.73.[2] Based upon an annual parallax shift of 24.18 mas as seen from Earth,[1] it is located 135 light years from the Sun. It may be a member of the Wolf 630 moving group of stars.[8]

This object has a stellar classification of G7 V,[3] which would suggest it is a G-type main-sequence star. However, Jofré et al. (2015) consider it to be a more evolved subgiant star due to a surface gravity of log g = 3.87. As such, it has an estimated 1.5 times the mass of the Sun and 3.2 times the Sun's radius. The star is 2.4 billion years old with what appears to be a leisurely rotation rate, judging by a projected rotational velocity of 0.98 km/s. It is radiating eight times the Sun's luminosity from its photosphere at an effective temperature of 5,311 K.[4]

References

  1. ^ a b c d e f van Leeuwen, F. (2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600.
  2. ^ a b c d Argue, A. N. (1966), "UBV photometry of 550 F, G and K type stars", Monthly Notices of the Royal Astronomical Society, 133 (4): 475, Bibcode:1966MNRAS.133..475A, doi:10.1093/mnras/133.4.475.
  3. ^ a b Cowley, A. P.; Bidelman, W. P. (February 1979), "MK spectral types for some F and G stars", Publications of the Astronomical Society of the Pacific, 91: 83–86, Bibcode:1979PASP...91...83C, doi:10.1086/130446.
  4. ^ a b c Jofré, E.; et al. (2015), "Stellar parameters and chemical abundances of 223 evolved stars with and without planets", Astronomy & Astrophysics, 574: A50, arXiv:1410.6422, Bibcode:2015A&A...574A..50J, doi:10.1051/0004-6361/201424474, S2CID 53666931.
  5. ^ 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.
  6. ^ "tet Cnc". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2017-09-08.
  7. ^ Kostjuk, N. D. (2004), "VizieR Online Data Catalog: HD-DM-GC-HR-HIP-Bayer-Flamsteed Cross Index (Kostjuk, 2002)", VizieR On-line Data Catalog: IV/27A. Originally Published in: Institute of Astronomy of Russian Academy of Sciences (2002), 4027, Bibcode:2004yCat.4027....0K.
  8. ^ McDonald, A. R. E.; Hearnshaw, J. B. (August 1983), "The Wolf 630 moving group of stars", Monthly Notices of the Royal Astronomical Society, 204 (3): 841–852, Bibcode:1983MNRAS.204..841M, doi:10.1093/mnras/204.3.841.