Nu1 Canis Majoris
  | |
| Observation data Epoch J2000.0 Equinox J2000.0 (ICRS) | |
|---|---|
| Constellation | Canis Major |
| Right ascension | 06h 36m 22.848s[1] |
| Declination | −18° 39′ 35.73″[1] |
| Apparent magnitude (V) | 5.704[2] (5.87 + 7.61)[3] |
| Characteristics | |
| Spectral type | G8 III + F3 IV-V[3] |
| B−V color index | +0.815[2] |
| Astrometry | |
| Radial velocity (Rv) | +26.13[2] km/s |
| Proper motion (μ) | RA: −9.902 mas/yr[1] Dec.: +23.229 mas/yr[1] |
| Parallax (π) | 12.3660±0.1985 mas[1] |
| Distance | 264 ± 4 ly (81 ± 1 pc) |
| Absolute magnitude (MV) | +1.23[4] |
| Details | |
| ν1 CMa A | |
| Mass | 1.41[2] M☉ |
| Radius | 7.1±0.3[1] R☉ |
| Luminosity | 8[2] L☉ |
| Surface gravity (log g) | 3.00[5] cgs |
| Temperature | 6,091±822[2] K |
| Metallicity [Fe/H] | −0.06[5] dex |
| Rotational velocity (v sin i) | 4.8±0.2[4] km/s |
| Age | 3.07[2] Gyr |
| Other designations | |
| ν1 CMa, 6 Canis Majoris, BD−18°1480, GC 8614, HD 47138, HIP 31564, HR 2423, SAO 151694, ADS 5253, CCDM 06364-1840, WDS 06364-1840[6] | |
| Database references | |
| SIMBAD | data |
Nu1 Canis Majoris is a binary star in the constellation Canis Major. Its name is a Bayer designation that is Latinized from ν1 Canis Majoris, and abbreviated Nu1 CMa or ν1 CMa. This system is visible to the naked eye as a point of light with an apparent visual magnitude of 5.7.[2] Based on parallax shift of 12.366 mas as seen from Earth orbit,[1] this system is approximately 264 light years from the Sun. It is drifting further away with a line of sight velocity of +26 km/s.[2]
As of 2011, the pair had an angular separation of 17.29 arc seconds along a position angle of 264.2°.[7] The yellow hued magnitude 5.87[3] primary, component A, is an evolved G-type giant star with a stellar classification of G8 III.[3] It is an estimated 3[2] billion years old and has 1.4[2] times the mass of the Sun. Having exhausted the supply of hydrogen at its core, it has expanded to 7 times the Sun's radius[1] and is radiating 8 times the luminosity of the Sun from its photosphere at an effective temperature of 6,091 K.[2]
The magnitude 7.61[3] companion, component B, is a yellow-white hued F-type main sequence/subgiant hybrid with a class of F3 IV-V.[3]
References
[edit]- 1 2 3 4 5 6 7 8 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 5 6 7 8 9 10 11 12 Luck, R. Earle (September 2015), "Abundances in the Local Region. I. G and K Giants", The Astronomical Journal, 150 (3): 23, arXiv:1507.01466, Bibcode:2015AJ....150...88L, doi:10.1088/0004-6256/150/3/88, S2CID 118505114, 88.
- 1 2 3 4 5 6 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.
- 1 2 Ammler-von Eiff, Matthias; Reiners, Ansgar (June 2012), "New measurements of rotation and differential rotation in A-F stars: are there two populations of differentially rotating stars?", Astronomy & Astrophysics, 542: A116, arXiv:1204.2459, Bibcode:2012A&A...542A.116A, doi:10.1051/0004-6361/201118724, S2CID 53666672.
- 1 2 Soubiran, C.; et al. (2008), "Vertical distribution of Galactic disk stars. IV. AMR and AVR from clump giants", Astronomy and Astrophysics, 480 (1): 91–101, arXiv:0712.1370, Bibcode:2008A&A...480...91S, doi:10.1051/0004-6361:20078788, S2CID 16602121.
- ↑ "nu01 CMa", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2017-09-05.
- ↑ Mason, Brian D.; et al. (May 2012), "Speckle Interferometry at the U.S. Naval Observatory. XVIII", The Astronomical Journal, 143 (5): 6, Bibcode:2012AJ....143..124M, doi:10.1088/0004-6256/143/5/124, 124, archived from the original on June 13, 2017.
