Nu Cancri

ν Cancri
Location of ν Cancri (circled)
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Cancer[1]
Right ascension 09h 02m 44.268s[2]
Declination +24° 27′ 10.39″[2]
Apparent magnitude (V) +5.46[3]
Characteristics
Evolutionary stage main sequence[4]
Spectral type A0 III[5]
U−B color index −0.10[3]
B−V color index −0.03[3]
Astrometry
Radial velocity (Rv)−15.6±0.7[6] km/s
Proper motion (μ) RA: −4.801 mas/yr[2]
Dec.: −1.621 mas/yr[2]
Parallax (π)7.2947±0.1477 mas[2]
Distance447 ± 9 ly
(137 ± 3 pc)
Absolute magnitude (MV)+0.05[1]
Orbit[7]
Period (P)1,401.4 ± 4.8 d (3.837 ± 0.013 yr)
Semi-major axis (a)≥ 138.3×106 km (0.924 AU)
Eccentricity (e)0.35±0.17
Periastron epoch (T)2419687±63 JD
Argument of periastron (ω)
(secondary)		264±9°
Semi-amplitude (K1)
(primary)		7.7±1.3 km/s
Details
ν Cnc A
Mass2.12[4] M☉
Radius2.73[4] R☉
Luminosity125[4] L☉
Surface gravity (log g)3.86[4] cgs
Temperature10,000[4] K
Metallicity [Fe/H]−0.20±0.04[1] dex
Rotational velocity (v sin i)18.9±0.4[8] km/s
Age498[9] Myr
Other designations
ν Cnc, 69 Cancri, BD+25°2029, FK5 2714, HD 77350, HIP 44405, HR 3595, SAO 80595[10]
Database references
SIMBADdata

Nu Cancri is a binary star system[7] in the zodiac constellation of Cancer. Its name is a Bayer designation that is Latinised from ν Cancri, and abbreviated Nu Cnc or ν Cnc. This star is faintly visible to the naked eye with an apparent visual magnitude of +5.46.[3] Based upon an annual parallax shift of 8.31 mas as seen from the Earth,[2] the star is located roughly 447 light-years (137 pc) away from the Sun. It is drifting closer with a line of sight velocity of −16 km/s.[6]

The binary nature of this system was announced in 1973. This is a single-lined spectroscopic binary system with an orbital period of 3.8 years and an eccentricity of 0.35.[7] The primary, component A, is a white-hued A-type star with a stellar classification of A0 III.[5] It is a magnetic Ap star with a field strength of 846×10−4 T, showing abundance peculiarities in strontium, chromium and mercury.[8] This has been studied as a mercury-manganese star that has reached the end of its main sequence lifetime, although it has an unusually low abundance of mercury for a star of this type.[11] The star has 2.8 times the mass of the Sun and is radiating 93 times the Sun's luminosity from its photosphere at an effective temperature of 10,250 K.[8]

References

  1. ^ a b c 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.
  2. ^ a b c d e 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.
  3. ^ a b c d 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.
  4. ^ a b c d e f Glagolevskij, Yu. V. (2019). "On Properties of Main Sequence Magnetic Stars". Astrophysical Bulletin. 74 (1): 66. Bibcode:2019AstBu..74...66G. doi:10.1134/S1990341319010073.
  5. ^ a b Royer, F.; et al. (October 2002), "Rotational velocities of A-type stars in the northern hemisphere. II. Measurement of v sin i", Astronomy and Astrophysics, 393 (3): 897–911, arXiv:astro-ph/0205255, Bibcode:2002A&A...393..897R, doi:10.1051/0004-6361:20020943, S2CID 14070763.
  6. ^ a b 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.
  7. ^ a b c Abt, Helmut A.; Snowden, Michael S. (February 1973), "The Binary Frequency for AP Stars", Astrophysical Journal Supplement, 25: 137, Bibcode:1973ApJS...25..137A, doi:10.1086/190265.
  8. ^ a b c Wraight, K. T.; et al. (February 2012), "A photometric study of chemically peculiar stars with the STEREO satellites - I. Magnetic chemically peculiar stars", Monthly Notices of the Royal Astronomical Society, 420 (1): 757–772, arXiv:1110.6283, Bibcode:2012MNRAS.420..757W, doi:10.1111/j.1365-2966.2011.20090.x, S2CID 14811051.
  9. ^ Kordopatis, G.; Schultheis, M.; McMillan, P. J.; Palicio, P. A.; De Laverny, P.; Recio-Blanco, A.; Creevey, O.; Álvarez, M. A.; Andrae, R.; Poggio, E.; Spitoni, E.; Contursi, G.; Zhao, H.; Oreshina-Slezak, I.; Ordenovic, C.; Bijaoui, A. (2023). "Stellar ages, masses, extinctions, and orbital parameters based on spectroscopic parameters of Gaia DR3". Astronomy and Astrophysics. 669: A104. arXiv:2206.07937. Bibcode:2023A&A...669A.104K. doi:10.1051/0004-6361/202244283.
  10. ^ "nu. Cnc", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2017-06-17
  11. ^ Monier, Richard (May 2025), "Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å. XX. HD 77350", Research Notes of the AAS, 9 (5): 124, Bibcode:2025RNAAS...9..124M, doi:10.3847/2515-5172/addabd, 124.
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