Astronomy:Nu Cancri
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| Observation data 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[2] mas/yr Dec.: −1.621[2] mas/yr |
| Parallax (π) | 7.2947 ± 0.1477[2] mas |
| Distance | 447 ± 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 astronomical unit|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 | |
| Mass | 2.12[4] M☉ |
| Radius | 2.73[4] R☉ |
| Luminosity | 125[4] L☉ |
| Surface gravity (log g) | 3.86[4] cgs |
| Temperature | 10,000[4] K |
| Metallicity [Fe/H] | −0.20±0.04[1] dex |
| Rotational velocity (v sin i) | 18.9±0.4[8] km/s |
| Age | 498[9] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
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
- ↑ 1.0 1.1 1.2 Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters 38 (5): 331. doi:10.1134/S1063773712050015. Bibcode: 2012AstL...38..331A. XHIP record for this object at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940. Gaia DR3 record for this source at VizieR.
- ↑ 3.0 3.1 3.2 3.3 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.
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 Glagolevskij, Yu. V. (2019). "On Properties of Main Sequence Magnetic Stars". Astrophysical Bulletin 74 (1): 66. doi:10.1134/S1990341319010073. Bibcode: 2019AstBu..74...66G.
- ↑ 5.0 5.1 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, doi:10.1051/0004-6361:20020943, Bibcode: 2002A&A...393..897R.
- ↑ 6.0 6.1 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.
- ↑ 7.0 7.1 7.2 Abt, Helmut A.; Snowden, Michael S. (February 1973), "The Binary Frequency for AP Stars", Astrophysical Journal Supplement 25: 137, doi:10.1086/190265, Bibcode: 1973ApJS...25..137A.
- ↑ 8.0 8.1 8.2 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, doi:10.1111/j.1365-2966.2011.20090.x, Bibcode: 2012MNRAS.420..757W.
- ↑ Kordopatis, G.; Schultheis, M.; McMillan, P. J.; Palicio, P. A.; De Laverny, P.; Recio-Blanco, A.; Creevey, O.; Álvarez, M. A. et al. (2023). "Stellar ages, masses, extinctions, and orbital parameters based on spectroscopic parameters of Gaia DR3". Astronomy and Astrophysics 669: A104. doi:10.1051/0004-6361/202244283. Bibcode: 2023A&A...669A.104K.
- ↑ "nu. Cnc". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=nu.+Cnc.
- ↑ 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, doi:10.3847/2515-5172/addabd, 124, Bibcode: 2025RNAAS...9..124M.
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